id stringlengths 9 13 | submitter stringlengths 1 64 ⌀ | authors stringlengths 5 22.9k | title stringlengths 4 245 | comments stringlengths 1 548 ⌀ | journal-ref stringlengths 4 362 ⌀ | doi stringlengths 12 82 ⌀ | report-no stringlengths 2 281 ⌀ | categories stringclasses 793 values | license stringclasses 9 values | orig_abstract stringlengths 24 1.95k | versions listlengths 1 30 | update_date stringlengths 10 10 | authors_parsed listlengths 1 1.74k | abstract stringlengths 21 1.95k |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
2310.18594 | Umananda Dev Goswami | Ronit Karmakar and Umananda Dev Goswami | Quasinormal modes, temperatures and greybody factors of black holes in a
generalized Rastall gravity theory | 19 pages, 15 figures; Published version | Phys. Scr. 99 (2024) 055003 | 10.1088/1402-4896/ad350e | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | We introduce a modification in the energy-momentum conservation violating
Rastall's theory of gravity and obtain a Reissner-Nordstr\"om-type black hole
solution in spacetime surrounded by a cloud of strings and charge fields. We
examine the horizons of the black hole along with the influence of the
parameters of the model on it. The scalar quasinormal modes (QNMs) of
oscillations of the black hole are also computed using the 6th order WKB
approximation method. It is seen that the Rastall parameter $\beta$ and the
newly introduced energy-momentum tensor trace parameter $\alpha$ as well as the
charge parameter $q$ and strings field parameter $a$ influence the amplitude
and damping of the QNMs. From the metric function, we obtain the temperature of
the black hole and study the effects of the four model parameters $\beta$,
$\alpha$, $q$ and $a$ on the temperature. We then examine the greybody factors
associated with the black hole and the corresponding total absorption
cross-section for it. It is seen that the modification we introduced in the
Rastall theory has a drastic effect on various properties of the black hole and
may lead to interesting outcomes in future when the better detection techniques
will be available with the LISA and the Einstein Telescope.
| [
{
"created": "Sat, 28 Oct 2023 05:10:39 GMT",
"version": "v1"
},
{
"created": "Sun, 17 Dec 2023 03:32:56 GMT",
"version": "v2"
},
{
"created": "Wed, 10 Apr 2024 10:40:29 GMT",
"version": "v3"
}
] | 2024-04-11 | [
[
"Karmakar",
"Ronit",
""
],
[
"Goswami",
"Umananda Dev",
""
]
] | We introduce a modification in the energy-momentum conservation violating Rastall's theory of gravity and obtain a Reissner-Nordstr\"om-type black hole solution in spacetime surrounded by a cloud of strings and charge fields. We examine the horizons of the black hole along with the influence of the parameters of the model on it. The scalar quasinormal modes (QNMs) of oscillations of the black hole are also computed using the 6th order WKB approximation method. It is seen that the Rastall parameter $\beta$ and the newly introduced energy-momentum tensor trace parameter $\alpha$ as well as the charge parameter $q$ and strings field parameter $a$ influence the amplitude and damping of the QNMs. From the metric function, we obtain the temperature of the black hole and study the effects of the four model parameters $\beta$, $\alpha$, $q$ and $a$ on the temperature. We then examine the greybody factors associated with the black hole and the corresponding total absorption cross-section for it. It is seen that the modification we introduced in the Rastall theory has a drastic effect on various properties of the black hole and may lead to interesting outcomes in future when the better detection techniques will be available with the LISA and the Einstein Telescope. |
gr-qc/9802015 | Ruth A. W. Gregory | Owen Dando and Ruth Gregory | Dilatonic global strings | 18 pages RevTeX, 3 figures, references amended | Phys. Rev. D 58, 023502 (1998) | 10.1103/PhysRevD.58.023502 | DTP/98/1 | gr-qc astro-ph hep-th | null | We examine the field equations of a self-gravitating global string in low
energy superstring gravity, allowing for an arbitrary coupling of the global
string to the dilaton. Massive and massless dilatons are considered. For the
massive dilaton the spacetime is similar to the recently discovered
non-singular time-dependent Einstein self-gravitating global string, but the
massless dilaton generically gives a singular spacetime, even allowing for
time-dependence. We also demonstrate a time-dependent non-singular
string/anti-string configuration, in which the string pair causes a
compactification of two of the spatial dimensions, albeit on a very large
scale.
| [
{
"created": "Fri, 6 Feb 1998 15:21:54 GMT",
"version": "v1"
},
{
"created": "Thu, 12 Feb 1998 17:23:37 GMT",
"version": "v2"
}
] | 2016-08-25 | [
[
"Dando",
"Owen",
""
],
[
"Gregory",
"Ruth",
""
]
] | We examine the field equations of a self-gravitating global string in low energy superstring gravity, allowing for an arbitrary coupling of the global string to the dilaton. Massive and massless dilatons are considered. For the massive dilaton the spacetime is similar to the recently discovered non-singular time-dependent Einstein self-gravitating global string, but the massless dilaton generically gives a singular spacetime, even allowing for time-dependence. We also demonstrate a time-dependent non-singular string/anti-string configuration, in which the string pair causes a compactification of two of the spatial dimensions, albeit on a very large scale. |
2010.15355 | Titus K Mathew | Jerin Mohan N D and Titus K Mathew | On the feasibility of truncated Israel-Stewart model in the context of
late acceleration | 34 pages and 9 figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A dissipative model of the Universe based on the causal relativistic
truncated Israel-Stewart theory is analysed in the context of recent
accelerated expansion of the Universe. The bulk viscosity and relaxation time
are taken as $\xi=\alpha\rho^s$ and
$\tau=\frac{\alpha}{\epsilon\gamma(2-\gamma)}\rho^{s-1}$ respectively. For
$s=1/2,$ we found an analytical solution for the Hubble parameter of the model.
We have estimated the model parameters by treating $\gamma=1$ and $\gamma$ as a
free parameter using the latest cosmological data.
The model predicts a prior decelerated phase and an end de Sitter phase as in
the standard $\Lambda$CDM model. The dynamical system analysis shows that the
prior decelerated epoch is an unstable equilibrium, while the far future de
Sitter epoch is stable. The age of the Universe obtained around $13.66$ Gyr,
which is close to the recent observations. The second law of thermodynamics is
found to be satisfied throughout the evolution in this model. The feasibility
of the model has been checked by contrasting with models based on the full
Israel-Stewart and the Eckart viscous theories. The truncated viscous model
appears more compatible with astronomical observations than the Eckart and full
causal viscous models.
| [
{
"created": "Thu, 29 Oct 2020 05:07:28 GMT",
"version": "v1"
},
{
"created": "Thu, 12 Aug 2021 12:42:19 GMT",
"version": "v2"
}
] | 2021-08-13 | [
[
"D",
"Jerin Mohan N",
""
],
[
"Mathew",
"Titus K",
""
]
] | A dissipative model of the Universe based on the causal relativistic truncated Israel-Stewart theory is analysed in the context of recent accelerated expansion of the Universe. The bulk viscosity and relaxation time are taken as $\xi=\alpha\rho^s$ and $\tau=\frac{\alpha}{\epsilon\gamma(2-\gamma)}\rho^{s-1}$ respectively. For $s=1/2,$ we found an analytical solution for the Hubble parameter of the model. We have estimated the model parameters by treating $\gamma=1$ and $\gamma$ as a free parameter using the latest cosmological data. The model predicts a prior decelerated phase and an end de Sitter phase as in the standard $\Lambda$CDM model. The dynamical system analysis shows that the prior decelerated epoch is an unstable equilibrium, while the far future de Sitter epoch is stable. The age of the Universe obtained around $13.66$ Gyr, which is close to the recent observations. The second law of thermodynamics is found to be satisfied throughout the evolution in this model. The feasibility of the model has been checked by contrasting with models based on the full Israel-Stewart and the Eckart viscous theories. The truncated viscous model appears more compatible with astronomical observations than the Eckart and full causal viscous models. |
2110.15820 | Odysse Halim | O. Halim, G. Vedovato, E. Milotti, G. A. Prodi, S. Bini, M. Drago, V.
Gayathri, C. Lazzaro, D. Lopez, A. Miani, B. O'Brien, F. Salemi, M.
Szczepanczyk, S. Tiwari, A. Virtuoso, S. Klimenko | The search of higher multipole radiation in gravitational waves from
compact binary coalescences by a minimally-modelled pipeline | 5 pages, Proceedings for the "17th International Conference on Topics
in Astroparticle and Underground Physics (TAUP)" | null | 10.1088/1742-6596/2156/1/012081 | null | gr-qc astro-ph.IM | http://creativecommons.org/licenses/by/4.0/ | The coherent WaveBurst (cWB) pipeline implements a minimally-modelled search
to find a coherent response in the network of gravitational wave detectors of
the LIGO-Virgo Collaboration in the time-frequency domain. In this manuscript,
we provide a timely introduction to an extension of the cWB analysis to detect
spectral features beyond the main quadrupolar emission of gravitational waves
during the inspiral phase of compact binary coalescences; more detailed
discussion will be provided in a forthcoming paper [1]. The search is performed
by defining specific regions in the time-frequency map to extract the energy of
harmonics of main quadrupole mode in the inspiral phase. This method has
already been used in the GW190814 discovery paper (Astrophys. J. Lett. 896
L44). Here we show the procedure to detect the (3, 3) multipole in GW190814
within the cWB framework.
Keywords: gravitational waves, analysis, multipoles, compact binary
coalescences
| [
{
"created": "Fri, 29 Oct 2021 14:32:21 GMT",
"version": "v1"
}
] | 2022-03-02 | [
[
"Halim",
"O.",
""
],
[
"Vedovato",
"G.",
""
],
[
"Milotti",
"E.",
""
],
[
"Prodi",
"G. A.",
""
],
[
"Bini",
"S.",
""
],
[
"Drago",
"M.",
""
],
[
"Gayathri",
"V.",
""
],
[
"Lazzaro",
"C.",
""
],
[
"Lopez",
"D.",
""
],
[
"Miani",
"A.",
""
],
[
"O'Brien",
"B.",
""
],
[
"Salemi",
"F.",
""
],
[
"Szczepanczyk",
"M.",
""
],
[
"Tiwari",
"S.",
""
],
[
"Virtuoso",
"A.",
""
],
[
"Klimenko",
"S.",
""
]
] | The coherent WaveBurst (cWB) pipeline implements a minimally-modelled search to find a coherent response in the network of gravitational wave detectors of the LIGO-Virgo Collaboration in the time-frequency domain. In this manuscript, we provide a timely introduction to an extension of the cWB analysis to detect spectral features beyond the main quadrupolar emission of gravitational waves during the inspiral phase of compact binary coalescences; more detailed discussion will be provided in a forthcoming paper [1]. The search is performed by defining specific regions in the time-frequency map to extract the energy of harmonics of main quadrupole mode in the inspiral phase. This method has already been used in the GW190814 discovery paper (Astrophys. J. Lett. 896 L44). Here we show the procedure to detect the (3, 3) multipole in GW190814 within the cWB framework. Keywords: gravitational waves, analysis, multipoles, compact binary coalescences |
gr-qc/9712091 | Fernando Lombardo | Fernando C. Lombardo and Francisco D. Mazzitelli | Influence functional in two dimensional dilaton gravity | 25 pages, RevTex, no figures. Minor changes has been added. To appear
in Physical Review D | Phys.Rev. D58 (1998) 024009 | 10.1103/PhysRevD.58.024009 | null | gr-qc hep-th | null | We evaluate the influence functional for two dimensional models of dilaton
gravity. This functional is exactly computed when the conformal invariance is
preserved, and it can be written as the difference between the Liouville
actions on each closed-time-path branch plus a boundary term. From the
influence action we derive the covariant form of the semiclassical field
equations. We also study the quantum to classical transition in cosmological
backgrounds. In the conformal case we show that the semiclassical approximation
is not valid because there is no imaginary part in the influence action.
Finally we show that the inclusion of the dilaton loop in the influence
functional breaks conformal invariance and ensures the validity of the
semiclassical approximation.
| [
{
"created": "Tue, 23 Dec 1997 20:02:37 GMT",
"version": "v1"
},
{
"created": "Tue, 14 Apr 1998 19:22:51 GMT",
"version": "v2"
}
] | 2009-10-30 | [
[
"Lombardo",
"Fernando C.",
""
],
[
"Mazzitelli",
"Francisco D.",
""
]
] | We evaluate the influence functional for two dimensional models of dilaton gravity. This functional is exactly computed when the conformal invariance is preserved, and it can be written as the difference between the Liouville actions on each closed-time-path branch plus a boundary term. From the influence action we derive the covariant form of the semiclassical field equations. We also study the quantum to classical transition in cosmological backgrounds. In the conformal case we show that the semiclassical approximation is not valid because there is no imaginary part in the influence action. Finally we show that the inclusion of the dilaton loop in the influence functional breaks conformal invariance and ensures the validity of the semiclassical approximation. |
0907.0462 | Christian Reisswig | Christian Reisswig, Sascha Husa, Luciano Rezzolla, Ernst Nils Dorband,
Denis Pollney, Jennifer Seiler | Gravitational-wave detectability of equal-mass black-hole binaries with
aligned spins | 18 pages, 11 figures, matches published version | Phys.Rev.D80:124026,2009 | 10.1103/PhysRevD.80.124026 | null | gr-qc astro-ph.CO astro-ph.GA astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Binary black-hole systems with spins aligned or anti-aligned to the orbital
angular momentum provide the natural ground to start detailed studies of the
influence of strong-field spin effects on gravitational wave observations of
coalescing binaries. Furthermore, such systems may be the preferred end-state
of the inspiral of generic supermassive binary black-hole systems. In view of
this, we have computed the inspiral and merger of a large set of binary systems
of equal-mass black holes with spins parallel to the orbital angular momentum
but otherwise arbitrary. Our attention is particularly focused on the
gravitational-wave emission so as to quantify how much spin effects contribute
to the signal-to-noise ratio, to the horizon distances, and to the relative
event rates for the representative ranges in masses and detectors. As expected,
the signal-to-noise ratio increases with the projection of the total black hole
spin in the direction of the orbital momentum. We find that equal-spin binaries
with maximum spin aligned with the orbital angular momentum are more than
"three times as loud" as the corresponding binaries with anti-aligned spins,
thus corresponding to event rates up to 30 times larger. We also consider the
waveform mismatch between the different spinning configurations and find that,
within our numerical accuracy, binaries with opposite spins S_1=-S_2 cannot be
distinguished whereas binaries with spin S_1=S_2 have clearly distinct
gravitational-wave emissions. Finally, we derive a simple expression for the
energy radiated in gravitational waves and find that the binaries always have
efficiencies E_rad/M > 3.6%, which can become as large as E_rad/M = 10% for
maximally spinning binaries with spins aligned with the orbital angular
momentum.
| [
{
"created": "Thu, 2 Jul 2009 19:11:05 GMT",
"version": "v1"
},
{
"created": "Fri, 8 Jan 2010 10:33:55 GMT",
"version": "v2"
}
] | 2010-01-09 | [
[
"Reisswig",
"Christian",
""
],
[
"Husa",
"Sascha",
""
],
[
"Rezzolla",
"Luciano",
""
],
[
"Dorband",
"Ernst Nils",
""
],
[
"Pollney",
"Denis",
""
],
[
"Seiler",
"Jennifer",
""
]
] | Binary black-hole systems with spins aligned or anti-aligned to the orbital angular momentum provide the natural ground to start detailed studies of the influence of strong-field spin effects on gravitational wave observations of coalescing binaries. Furthermore, such systems may be the preferred end-state of the inspiral of generic supermassive binary black-hole systems. In view of this, we have computed the inspiral and merger of a large set of binary systems of equal-mass black holes with spins parallel to the orbital angular momentum but otherwise arbitrary. Our attention is particularly focused on the gravitational-wave emission so as to quantify how much spin effects contribute to the signal-to-noise ratio, to the horizon distances, and to the relative event rates for the representative ranges in masses and detectors. As expected, the signal-to-noise ratio increases with the projection of the total black hole spin in the direction of the orbital momentum. We find that equal-spin binaries with maximum spin aligned with the orbital angular momentum are more than "three times as loud" as the corresponding binaries with anti-aligned spins, thus corresponding to event rates up to 30 times larger. We also consider the waveform mismatch between the different spinning configurations and find that, within our numerical accuracy, binaries with opposite spins S_1=-S_2 cannot be distinguished whereas binaries with spin S_1=S_2 have clearly distinct gravitational-wave emissions. Finally, we derive a simple expression for the energy radiated in gravitational waves and find that the binaries always have efficiencies E_rad/M > 3.6%, which can become as large as E_rad/M = 10% for maximally spinning binaries with spins aligned with the orbital angular momentum. |
2103.11999 | Hao-Jui Kuan | Hao-Jui Kuan, Daniela D. Doneva, Stoytcho S. Yazadjiev | Dynamical Formation of Scalarized Black Holes and Neutron Stars through
Stellar Core Collapse | 9 pages, 10 figures; accepted in PRL. This version is based on fully
nonlinear simulations beyond the decoupling limit | Phys. Rev. Lett. 127, 161103 (2021) | 10.1103/PhysRevLett.127.161103 | null | gr-qc astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In a certain class of scalar-Gauss-Bonnet gravity, the black holes and the
neutron stars can undergo spontaneous scalarization -- a strong gravity phase
transition triggered by a tachyonic instability due to the nonminimal coupling
between the scalar field and the spacetime curvature. Studies of this
phenomenon have, so far, been restricted mainly to the study of the tachyonic
instability and stationary scalarized black holes and neutron stars. To date,
no realistic physical mechanism for the formation of isolated scalarized black
holes and neutron stars has been proposed. We study, for the first time, the
spherically symmetric fully nonlinear stellar core collapse to a black hole and
a neutron star in scalar-Gauss-Bonnet theories allowing for a spontaneous
scalarization. We show that the core collapse can produce scalarized black
holes and scalarized neutron stars starting with a nonscalarized progenitor
star. The possible paths to reach the end (non)scalarized state are quite rich
leading to interesting possibilities for observational manifestations.
| [
{
"created": "Mon, 22 Mar 2021 16:47:20 GMT",
"version": "v1"
},
{
"created": "Wed, 13 Oct 2021 13:22:46 GMT",
"version": "v2"
},
{
"created": "Fri, 15 Oct 2021 15:07:57 GMT",
"version": "v3"
}
] | 2021-10-18 | [
[
"Kuan",
"Hao-Jui",
""
],
[
"Doneva",
"Daniela D.",
""
],
[
"Yazadjiev",
"Stoytcho S.",
""
]
] | In a certain class of scalar-Gauss-Bonnet gravity, the black holes and the neutron stars can undergo spontaneous scalarization -- a strong gravity phase transition triggered by a tachyonic instability due to the nonminimal coupling between the scalar field and the spacetime curvature. Studies of this phenomenon have, so far, been restricted mainly to the study of the tachyonic instability and stationary scalarized black holes and neutron stars. To date, no realistic physical mechanism for the formation of isolated scalarized black holes and neutron stars has been proposed. We study, for the first time, the spherically symmetric fully nonlinear stellar core collapse to a black hole and a neutron star in scalar-Gauss-Bonnet theories allowing for a spontaneous scalarization. We show that the core collapse can produce scalarized black holes and scalarized neutron stars starting with a nonscalarized progenitor star. The possible paths to reach the end (non)scalarized state are quite rich leading to interesting possibilities for observational manifestations. |
1705.06705 | Gregory J. Galloway | Gregory J. Galloway and Eric Ling | Topology and singularities in cosmological spacetimes obeying the null
energy condition | 8 pages; v2: minor changes, version to appear in CMP | null | 10.1007/s00220-017-3020-9 | null | gr-qc math.DG | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We consider globally hyperbolic spacetimes with compact Cauchy surfaces in a
setting compatible with the presence of a positive cosmological constant. More
specifically, for 3+1 dimensional spacetimes which satisfy the null energy
condition and contain a future expanding compact Cauchy surface, we establish a
precise connection between the topology of the Cauchy surfaces and the
occurrence of past singularities. In addition to (a refinement of) the Penrose
singularity theorem, the proof makes use of some recent advances in the
topology of 3-manifolds and of certain fundamental existence results for
minimal surfaces.
| [
{
"created": "Thu, 18 May 2017 17:22:10 GMT",
"version": "v1"
},
{
"created": "Fri, 9 Mar 2018 22:43:58 GMT",
"version": "v2"
}
] | 2018-03-13 | [
[
"Galloway",
"Gregory J.",
""
],
[
"Ling",
"Eric",
""
]
] | We consider globally hyperbolic spacetimes with compact Cauchy surfaces in a setting compatible with the presence of a positive cosmological constant. More specifically, for 3+1 dimensional spacetimes which satisfy the null energy condition and contain a future expanding compact Cauchy surface, we establish a precise connection between the topology of the Cauchy surfaces and the occurrence of past singularities. In addition to (a refinement of) the Penrose singularity theorem, the proof makes use of some recent advances in the topology of 3-manifolds and of certain fundamental existence results for minimal surfaces. |
0912.1769 | Scott Pollack | S. E. Pollack, M. D. Turner, S. Schlamminger, C. A. Hagedorn, and J.
H. Gundlach | Charge Management for Gravitational Wave Observatories using UV LEDs | 5 pages, submitted to PRD | Phys.Rev.D81:021101,2010 | 10.1103/PhysRevD.81.021101 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Accumulation of electrical charge on the end mirrors of gravitational wave
observatories, such as the space-based LISA mission and ground-based LIGO
detectors, can become a source of noise limiting the sensitivity of such
detectors through electronic couplings to nearby surfaces. Torsion balances
provide an ideal means for testing gravitational wave technologies due to their
high sensitivity to small forces. Our torsion pendulum apparatus consists of a
movable Au-coated Cu plate brought near a Au-coated Si plate pendulum suspended
from a non-conducting quartz fiber. A UV LED located near the pendulum
photoejects electrons from the surface, and a UV LED driven electron gun
directs photoelectrons towards the pendulum surface. We have demonstrated both
charging and discharging of the pendulum with equivalent charging rates of
$\sim$$10^5 e/\mathrm{s}$, as well as spectral measurements of the pendulum
charge resulting in a white noise level equivalent to $3\times10^5
e/\sqrt{Hz}$.
| [
{
"created": "Wed, 9 Dec 2009 15:09:02 GMT",
"version": "v1"
}
] | 2010-04-21 | [
[
"Pollack",
"S. E.",
""
],
[
"Turner",
"M. D.",
""
],
[
"Schlamminger",
"S.",
""
],
[
"Hagedorn",
"C. A.",
""
],
[
"Gundlach",
"J. H.",
""
]
] | Accumulation of electrical charge on the end mirrors of gravitational wave observatories, such as the space-based LISA mission and ground-based LIGO detectors, can become a source of noise limiting the sensitivity of such detectors through electronic couplings to nearby surfaces. Torsion balances provide an ideal means for testing gravitational wave technologies due to their high sensitivity to small forces. Our torsion pendulum apparatus consists of a movable Au-coated Cu plate brought near a Au-coated Si plate pendulum suspended from a non-conducting quartz fiber. A UV LED located near the pendulum photoejects electrons from the surface, and a UV LED driven electron gun directs photoelectrons towards the pendulum surface. We have demonstrated both charging and discharging of the pendulum with equivalent charging rates of $\sim$$10^5 e/\mathrm{s}$, as well as spectral measurements of the pendulum charge resulting in a white noise level equivalent to $3\times10^5 e/\sqrt{Hz}$. |
1010.0523 | Milton Ruiz | Milton Ruiz, David Hilditch, Sebastiano Bernuzzi | Constraint preserving boundary conditions for the Z4c formulation of
general relativity | 18 pages, 8 figures | Phys.Rev.D83:024025,2011 | 10.1103/PhysRevD.83.024025 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We discuss high order absorbing constraint preserving boundary conditions for
the Z4c formulation of general relativity coupled to the moving puncture family
of gauges. We are primarily concerned with the constraint preservation and
absorption properties of these conditions. In the frozen coefficient
approximation, with an appropriate first order pseudo-differential reduction,
we show that the constraint subsystem is boundary stable on a four dimensional
compact manifold. We analyze the remainder of the initial boundary value
problem for a spherical reduction of the Z4c formulation with a particular
choice of the puncture gauge. Numerical evidence for the efficacy of the
conditions is presented in spherical symmetry.
| [
{
"created": "Mon, 4 Oct 2010 10:03:25 GMT",
"version": "v1"
},
{
"created": "Wed, 9 Feb 2011 11:41:38 GMT",
"version": "v2"
}
] | 2015-03-17 | [
[
"Ruiz",
"Milton",
""
],
[
"Hilditch",
"David",
""
],
[
"Bernuzzi",
"Sebastiano",
""
]
] | We discuss high order absorbing constraint preserving boundary conditions for the Z4c formulation of general relativity coupled to the moving puncture family of gauges. We are primarily concerned with the constraint preservation and absorption properties of these conditions. In the frozen coefficient approximation, with an appropriate first order pseudo-differential reduction, we show that the constraint subsystem is boundary stable on a four dimensional compact manifold. We analyze the remainder of the initial boundary value problem for a spherical reduction of the Z4c formulation with a particular choice of the puncture gauge. Numerical evidence for the efficacy of the conditions is presented in spherical symmetry. |
gr-qc/0309006 | Sanjeev S. Seahra | Sanjeev S. Seahra and Paul S. Wesson | Universes encircling 5-dimensional black holes | Reference added, 20 pages, 3 figures, REVTeX4 | J.Math.Phys. 44 (2003) 5664-5680 | 10.1063/1.1623617 | null | gr-qc hep-th | null | We clarify the status of two known solutions to the 5-dimensional vacuum
Einstein field equations derived by Liu, Mashhoon & Wesson (LMW) and Fukui,
Seahra & Wesson (FSW), respectively. Both 5-metrics explicitly embed
4-dimensional Friedman-Lemaitre-Robertson-Walker cosmologies with a wide range
of characteristics. We show that both metrics are also equivalent to
5-dimensional topological black hole (TBH) solutions, which is demonstrated by
finding explicit coordinate transformations from the TBH to LMW and FSW line
elements. We argue that the equivalence is a direct consequence of Birkhoff's
theorem generalized to 5 dimensions. Finally, for a special choice of
parameters we plot constant coordinate surfaces of the LMW patch in a
Penrose-Carter diagram. This shows that the LMW coordinates are regular across
the black and/or white hole horizons.
| [
{
"created": "Mon, 1 Sep 2003 20:34:38 GMT",
"version": "v1"
},
{
"created": "Wed, 7 Jan 2004 15:50:18 GMT",
"version": "v2"
}
] | 2009-11-10 | [
[
"Seahra",
"Sanjeev S.",
""
],
[
"Wesson",
"Paul S.",
""
]
] | We clarify the status of two known solutions to the 5-dimensional vacuum Einstein field equations derived by Liu, Mashhoon & Wesson (LMW) and Fukui, Seahra & Wesson (FSW), respectively. Both 5-metrics explicitly embed 4-dimensional Friedman-Lemaitre-Robertson-Walker cosmologies with a wide range of characteristics. We show that both metrics are also equivalent to 5-dimensional topological black hole (TBH) solutions, which is demonstrated by finding explicit coordinate transformations from the TBH to LMW and FSW line elements. We argue that the equivalence is a direct consequence of Birkhoff's theorem generalized to 5 dimensions. Finally, for a special choice of parameters we plot constant coordinate surfaces of the LMW patch in a Penrose-Carter diagram. This shows that the LMW coordinates are regular across the black and/or white hole horizons. |
gr-qc/0611083 | Francisco Lobo | Francisco S. N. Lobo, Aaron V. B. Arellano | Gravastars supported by nonlinear electrodynamics | 23 pages, 10 figures, LaTeX2e, IOP style files. V2: considerable
changes, references added; to appear in Class. Quant. Gravity | Class.Quant.Grav.24:1069-1088,2007 | 10.1088/0264-9381/24/5/004 | null | gr-qc astro-ph hep-th | null | Gravastar models have recently been proposed as an alternative to black
holes, mainly to avoid the problematic issues associated with event horizons
and singularities. In this work, a wide variety of gravastar models within the
context of nonlinear electrodynamics are constructed. Using the $F$
representation, specific forms of Lagrangians are considered describing
magnetic gravastars, which may be interpreted as self-gravitating magnetic
monopoles with charge $g$. Using the dual $P$ formulation of nonlinear
electrodynamics, electric gravastar models are constructed by considering
specific structural functions, and the characteristics and physical properties
of the solutions are further explored. These interior nonlinear electrodynamic
geometries are matched to an exterior Schwarzschild spacetime at a junction
interface.
| [
{
"created": "Wed, 15 Nov 2006 11:21:49 GMT",
"version": "v1"
},
{
"created": "Mon, 22 Jan 2007 17:26:43 GMT",
"version": "v2"
},
{
"created": "Tue, 23 Jan 2007 10:25:39 GMT",
"version": "v3"
}
] | 2008-11-26 | [
[
"Lobo",
"Francisco S. N.",
""
],
[
"Arellano",
"Aaron V. B.",
""
]
] | Gravastar models have recently been proposed as an alternative to black holes, mainly to avoid the problematic issues associated with event horizons and singularities. In this work, a wide variety of gravastar models within the context of nonlinear electrodynamics are constructed. Using the $F$ representation, specific forms of Lagrangians are considered describing magnetic gravastars, which may be interpreted as self-gravitating magnetic monopoles with charge $g$. Using the dual $P$ formulation of nonlinear electrodynamics, electric gravastar models are constructed by considering specific structural functions, and the characteristics and physical properties of the solutions are further explored. These interior nonlinear electrodynamic geometries are matched to an exterior Schwarzschild spacetime at a junction interface. |
1004.1760 | Sun ChengYi | Cheng-Yi Sun | Trapping Horizons in the Sultana-Dyer Space-Time | no figures, 5 pages; PCAS and key words are added | Commun.Theor.Phys.55:597-598,2011 | 10.1088/0253-6102/55/4/13 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Sultana-Dyer space-time is suggested as a model describing a black hole
embedded in an expanding universe. Recently, in \cite{0705.4012}, its global
structure is analyzed and the trapping horizons are shown. In the paper, by
directly calculating the expansions of the radial null vector fields normal to
the space-like two-spheres foliating the trapping horizons, we find that the
trapping horizon outside the event horizon in the Sultana-Dyer space-time is a
past trapping horizon. Further, we find that the past trapping horizon is an
outer, instantaneously degenerate or inner trapping horizon accordingly when
the radial coordinate is less than, equal to or greater than some value.
| [
{
"created": "Sun, 11 Apr 2010 04:35:23 GMT",
"version": "v1"
},
{
"created": "Mon, 19 Apr 2010 06:26:10 GMT",
"version": "v2"
},
{
"created": "Sat, 29 May 2010 05:44:36 GMT",
"version": "v3"
}
] | 2011-05-05 | [
[
"Sun",
"Cheng-Yi",
""
]
] | The Sultana-Dyer space-time is suggested as a model describing a black hole embedded in an expanding universe. Recently, in \cite{0705.4012}, its global structure is analyzed and the trapping horizons are shown. In the paper, by directly calculating the expansions of the radial null vector fields normal to the space-like two-spheres foliating the trapping horizons, we find that the trapping horizon outside the event horizon in the Sultana-Dyer space-time is a past trapping horizon. Further, we find that the past trapping horizon is an outer, instantaneously degenerate or inner trapping horizon accordingly when the radial coordinate is less than, equal to or greater than some value. |
1705.07703 | Javad Taghizadeh Firouzjaee | Abasalt Rostami and Javad T. Firouzjaee | Quantum decoherence from entanglement during inflation | 11 pages | null | null | null | gr-qc astro-ph.CO hep-th quant-ph | http://creativecommons.org/licenses/by/4.0/ | We study the primary entanglement effect on the decoherence of fields reduced
density matrix which are in interaction with another fields or independent mode
functions. We show that the primary entanglement has a significant role in
decoherence of the system quantum state. We find that the existence of
entanglement could couple dynamical equations coming from Schr\"{o}dinger
equation. We show if one wants to see no effect of the entanglement parameter
in decoherence then interaction terms in Hamiltonian can not be independent
from each other. Generally, including the primary entanglement destroys the
independence of the interaction terms. Our results could be generalized to
every scalar quantum field theory with a well defined quantization in a given
curved space time.
| [
{
"created": "Mon, 22 May 2017 13:09:30 GMT",
"version": "v1"
}
] | 2017-05-23 | [
[
"Rostami",
"Abasalt",
""
],
[
"Firouzjaee",
"Javad T.",
""
]
] | We study the primary entanglement effect on the decoherence of fields reduced density matrix which are in interaction with another fields or independent mode functions. We show that the primary entanglement has a significant role in decoherence of the system quantum state. We find that the existence of entanglement could couple dynamical equations coming from Schr\"{o}dinger equation. We show if one wants to see no effect of the entanglement parameter in decoherence then interaction terms in Hamiltonian can not be independent from each other. Generally, including the primary entanglement destroys the independence of the interaction terms. Our results could be generalized to every scalar quantum field theory with a well defined quantization in a given curved space time. |
2207.07060 | Valerio Faraoni | Reza Saadati, Andrea Giusti, Valerio Faraoni, Fatimah Shojai | New time-dependent solutions of viable Horndeski gravity | 17 pages, 2 figures | null | 10.1088/1475-7516/2022/09/067 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We generate new spherical and time-dependent solutions of viable Horndeski
gravity by disforming a solution of the Einstein equations with scalar field
source and positive cosmological constant. They describe dynamical objects
embedded in asymptotically FLRW spacetimes and contain apparent horizons and a
finite radius singularity that evolve in time in peculiar ways apparently not
encountered before in Einstein and "old" scalar-tensor gravity.
| [
{
"created": "Thu, 14 Jul 2022 16:59:22 GMT",
"version": "v1"
}
] | 2022-10-05 | [
[
"Saadati",
"Reza",
""
],
[
"Giusti",
"Andrea",
""
],
[
"Faraoni",
"Valerio",
""
],
[
"Shojai",
"Fatimah",
""
]
] | We generate new spherical and time-dependent solutions of viable Horndeski gravity by disforming a solution of the Einstein equations with scalar field source and positive cosmological constant. They describe dynamical objects embedded in asymptotically FLRW spacetimes and contain apparent horizons and a finite radius singularity that evolve in time in peculiar ways apparently not encountered before in Einstein and "old" scalar-tensor gravity. |
2402.13014 | A. Yu. Petrov | A. A. Ara\'ujo Filho, J. R. Nascimento, A. Yu. Petrov, P. J.
Porf\'irio | An exact stationary axisymmetric vacuum solution within a metric--affine
bumblebee gravity | 36 pages, version accepted to JCAP | JCAP07(2024)004 | 10.1088/1475-7516/2024/07/004 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Within the framework of the spontaneous Lorentz symmetry breaking, we
consider a metric--affine generalization of the gravitational sector of the
Standard--Model Extension (SME), including the Lorentz--violating (LV)
coefficients $u$ and $s^{\mu\nu}$. In this model, we derive the modified
Einstein field equations in order to obtain a new axisymmetric vacuum spinning
solution for a particular bumblebee's profile. Such a solution has the
remarkable property of incorporating the effects of Lorentz symmetry breaking
(LSB) through the LV dimensionless parameter $X=\xi b^2$, as the LSB is turned
off, $X=0$, we recover the well--established result, the Kerr solution, as
expected. Afterwards, we calculate the geodesics, the radial acceleration and
thermodynamic quantities for this new metric. We also estimate an upper bound
for $X$ by using astrophysical data of the advance Mercury's perihelion.
| [
{
"created": "Tue, 20 Feb 2024 13:57:23 GMT",
"version": "v1"
},
{
"created": "Mon, 10 Jun 2024 16:20:40 GMT",
"version": "v2"
}
] | 2024-07-03 | [
[
"Filho",
"A. A. Araújo",
""
],
[
"Nascimento",
"J. R.",
""
],
[
"Petrov",
"A. Yu.",
""
],
[
"Porfírio",
"P. J.",
""
]
] | Within the framework of the spontaneous Lorentz symmetry breaking, we consider a metric--affine generalization of the gravitational sector of the Standard--Model Extension (SME), including the Lorentz--violating (LV) coefficients $u$ and $s^{\mu\nu}$. In this model, we derive the modified Einstein field equations in order to obtain a new axisymmetric vacuum spinning solution for a particular bumblebee's profile. Such a solution has the remarkable property of incorporating the effects of Lorentz symmetry breaking (LSB) through the LV dimensionless parameter $X=\xi b^2$, as the LSB is turned off, $X=0$, we recover the well--established result, the Kerr solution, as expected. Afterwards, we calculate the geodesics, the radial acceleration and thermodynamic quantities for this new metric. We also estimate an upper bound for $X$ by using astrophysical data of the advance Mercury's perihelion. |
gr-qc/0509081 | Gaurav Khanna | Seth Connors, Gaurav Khanna | Approximate pre-classical solutions in loop quantum cosmology | 10 pages, 5 figures | Class.Quant.Grav.23:2919-2926,2006 | 10.1088/0264-9381/23/9/009 | null | gr-qc | null | In this paper we introduce a numerical approximation technique to obtain
pre-classical solutions to models of loop quantum gravity. In particular, we
apply the technique to vacuum Bianchi I cosmological models and recover known
solutions. We also present a pre-classical solution to the Bianchi I LRS model
with cosmological constant, which has not appeared elsewhere.
| [
{
"created": "Tue, 20 Sep 2005 21:14:19 GMT",
"version": "v1"
}
] | 2014-11-17 | [
[
"Connors",
"Seth",
""
],
[
"Khanna",
"Gaurav",
""
]
] | In this paper we introduce a numerical approximation technique to obtain pre-classical solutions to models of loop quantum gravity. In particular, we apply the technique to vacuum Bianchi I cosmological models and recover known solutions. We also present a pre-classical solution to the Bianchi I LRS model with cosmological constant, which has not appeared elsewhere. |
1904.09260 | Lo\"ic Marsot | Lo\"ic Marsot | How does the photon's spin affect Gravitational Wave measurements? | 12 pages; version 2 matches publication with an improved
introduction, 14 pages | Phys. Rev. D 100, 064050 (2019) | 10.1103/PhysRevD.100.064050 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the effect of the polarization of light beams on the time delay
measured in Gravitational Wave experiments. To this end, we consider the
Mathisson-Papapetrou-Dixon equations in a gravitational wave background, with
two of the possible spin supplementary conditions: by Frenkel-Pirani, or by
Tulczyjew. In the first case, photons follow a null geodesic and thus no spin
effect is present. The second case shows a deviation of the photons from the
null geodesic, resulting in a tiny effect on the measured time delay of photons
depending on their polarization state.
| [
{
"created": "Fri, 19 Apr 2019 16:42:09 GMT",
"version": "v1"
},
{
"created": "Wed, 25 Sep 2019 13:07:12 GMT",
"version": "v2"
}
] | 2019-10-02 | [
[
"Marsot",
"Loïc",
""
]
] | We study the effect of the polarization of light beams on the time delay measured in Gravitational Wave experiments. To this end, we consider the Mathisson-Papapetrou-Dixon equations in a gravitational wave background, with two of the possible spin supplementary conditions: by Frenkel-Pirani, or by Tulczyjew. In the first case, photons follow a null geodesic and thus no spin effect is present. The second case shows a deviation of the photons from the null geodesic, resulting in a tiny effect on the measured time delay of photons depending on their polarization state. |
gr-qc/0501006 | Hernando Quevedo | Hernando Quevedo | Pioneer's Anomaly and the Solar Quadrupole Moment | Typos corrected, references added | null | 10.1063/1.1900512 | null | gr-qc | null | The trajectories of test particles moving in the gravitational field of a
non-spherically symmetric mass distribution become affected by the presence of
multipole moments. In the case of hyperbolic trajectories, the quadrupole
moment of an oblate mass induces a displacement of the trajectory towards the
mass source, an effect that can be interpreted as an additional acceleration
directed towards the source. Although this additional acceleration is not
constant, we perform a general relativistic analysis in order to evaluate the
possibility of explaining Pioneer's anomalous acceleration by means of the
observed Solar quadrupole moment, within the range of accuracy of the observed
anomalous acceleration. We conclude that the Solar quadrupole moment generates
an acceleration which is of the same order of magnitude of Pioneer's constant
acceleration only at distances of a few astronomical units.
| [
{
"created": "Tue, 4 Jan 2005 05:16:28 GMT",
"version": "v1"
},
{
"created": "Mon, 23 May 2005 23:56:16 GMT",
"version": "v2"
}
] | 2009-11-11 | [
[
"Quevedo",
"Hernando",
""
]
] | The trajectories of test particles moving in the gravitational field of a non-spherically symmetric mass distribution become affected by the presence of multipole moments. In the case of hyperbolic trajectories, the quadrupole moment of an oblate mass induces a displacement of the trajectory towards the mass source, an effect that can be interpreted as an additional acceleration directed towards the source. Although this additional acceleration is not constant, we perform a general relativistic analysis in order to evaluate the possibility of explaining Pioneer's anomalous acceleration by means of the observed Solar quadrupole moment, within the range of accuracy of the observed anomalous acceleration. We conclude that the Solar quadrupole moment generates an acceleration which is of the same order of magnitude of Pioneer's constant acceleration only at distances of a few astronomical units. |
gr-qc/0602061 | Ouali Taoufik | A. Errahmani, T. Ouali | High energy description of dark energy in an approximate 3-brane
Brans-Dicke cosmology | 9 pages | Phys.Lett. B641 (2006) 357-361 | 10.1016/j.physletb.2006.08.063 | null | gr-qc | null | We consider a Brans-Dicke cosmology in five-dimensional space-time.
Neglecting the quadratic and the mixed Brans-Dicke terms in the Einstein
equation, we derive a modified wave equation of the Brans-Dicke field. We show
that, at high energy limit, the 3-brane Brans-Dicke cosmology could be
described as the standard one by changing the equation of state. Finally as an
illustration of the purpose, we show that the dark energy component of the
universe agrees with the observations data.
| [
{
"created": "Wed, 15 Feb 2006 13:39:43 GMT",
"version": "v1"
},
{
"created": "Thu, 20 Apr 2006 11:53:51 GMT",
"version": "v2"
}
] | 2009-11-11 | [
[
"Errahmani",
"A.",
""
],
[
"Ouali",
"T.",
""
]
] | We consider a Brans-Dicke cosmology in five-dimensional space-time. Neglecting the quadratic and the mixed Brans-Dicke terms in the Einstein equation, we derive a modified wave equation of the Brans-Dicke field. We show that, at high energy limit, the 3-brane Brans-Dicke cosmology could be described as the standard one by changing the equation of state. Finally as an illustration of the purpose, we show that the dark energy component of the universe agrees with the observations data. |
gr-qc/0609081 | Ignazio Ciufolini | Ignazio Ciufolini | On the orbit of the LARES satellite | null | null | null | null | gr-qc | null | This paper is motivated by the recent possibility to find an inexpensive
launching vehicle for the LARES satellite, however at an altitude much lower
than originally planned for the LAGEOS III/LARES satellite.
We present here a preliminary error analysis corresponding to a lower,
quasi-polar, orbit, in particular we analyze the effect on the LARES node of
the Earth's static gravitational field, and in particular of the Earth's even
zonal harmonics, the effect of the time dependent Earth's gravitational field,
and in particular of the K1 tide, and the effect of particle drag.
| [
{
"created": "Wed, 20 Sep 2006 15:01:53 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Ciufolini",
"Ignazio",
""
]
] | This paper is motivated by the recent possibility to find an inexpensive launching vehicle for the LARES satellite, however at an altitude much lower than originally planned for the LAGEOS III/LARES satellite. We present here a preliminary error analysis corresponding to a lower, quasi-polar, orbit, in particular we analyze the effect on the LARES node of the Earth's static gravitational field, and in particular of the Earth's even zonal harmonics, the effect of the time dependent Earth's gravitational field, and in particular of the K1 tide, and the effect of particle drag. |
1905.09671 | Adam Balcerzak | Adam Balcerzak and Konrad Marosek | Emergence of multiverse in third quantized varying constants cosmologies | 6 pages, 2 figures | Eur. Phys. J. C (2019) 79: 563 | 10.1140/epjc/s10052-019-7069-9 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Although the standard cosmological model explains most of the observed
phenomena it still struggles with the problem of initial singularity. An
interesting scenario in which the problem of the initial singularity is somehow
circumvented was proposed in the context of string theory where the canonical
quantisation procedure was additionally applied. A similar effect can be
achieved in the context of the canonically quantized theory with varying speed
of light and varying gravitational constant where both quantities are
represented by non-minimally coupled scalar fields. Such theory contains both
the pre-big-bang contracting phase and the post-big-bang expanding phase and
predicts non-vanishing probability of the transition from the former to the
latter phase. In this paper we quantize such a theory once again by applying
the third quantization scheme and show that the resulting theory contains
scenario in which the whole multiverse is created from nothing. The generated
family of the universes is described by the Bose-Einstein distribution.
| [
{
"created": "Thu, 23 May 2019 14:13:51 GMT",
"version": "v1"
},
{
"created": "Fri, 24 May 2019 13:21:22 GMT",
"version": "v2"
},
{
"created": "Wed, 3 Jul 2019 17:24:38 GMT",
"version": "v3"
}
] | 2019-07-04 | [
[
"Balcerzak",
"Adam",
""
],
[
"Marosek",
"Konrad",
""
]
] | Although the standard cosmological model explains most of the observed phenomena it still struggles with the problem of initial singularity. An interesting scenario in which the problem of the initial singularity is somehow circumvented was proposed in the context of string theory where the canonical quantisation procedure was additionally applied. A similar effect can be achieved in the context of the canonically quantized theory with varying speed of light and varying gravitational constant where both quantities are represented by non-minimally coupled scalar fields. Such theory contains both the pre-big-bang contracting phase and the post-big-bang expanding phase and predicts non-vanishing probability of the transition from the former to the latter phase. In this paper we quantize such a theory once again by applying the third quantization scheme and show that the resulting theory contains scenario in which the whole multiverse is created from nothing. The generated family of the universes is described by the Bose-Einstein distribution. |
1710.02327 | LIGO Scientific Collaboration and Virgo Collaboration | The LIGO Scientific Collaboration and the Virgo Collaboration: B. P.
Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, T. Adams,
P. Addesso, R. X. Adhikari, V. B. Adya, C. Affeldt, M. Afrough, B. Agarwal,
M. Agathos, K. Agatsuma, N. Aggarwal, O. D. Aguiar, L. Aiello, A. Ain, B.
Allen, G. Allen, A. Allocca, P. A. Altin, A. Amato, A. Ananyeva, S. B.
Anderson, W. G. Anderson, S. V. Angelova, S. Antier, S. Appert, K. Arai, M.
C. Araya, J. S. Areeda, N. Arnaud, K. G. Arun, S. Ascenzi, G. Ashton, M. Ast,
S. M. Aston, P. Astone, D. V. Atallah, P. Aufmuth, C. Aulbert, K. AultONeal,
C. Austin, A. Avila-Alvarez, S. Babak, P. Bacon, M. K. M. Bader, S. Bae, P.
T. Baker, F. Baldaccini, G. Ballardin, S. W. Ballmer, S. Banagiri, J. C.
Barayoga, S. E. Barclay, B. C. Barish, D. Barker, K. Barkett, F. Barone, B.
Barr, L. Barsotti, M. Barsuglia, D. Barta, J. Bartlett, I. Bartos, R.
Bassiri, A. Basti, J. C. Batch, M. Bawaj, J. C. Bayley, M. Bazzan, B.
B\'ecsy, C. Beer, M. Bejger, I. Belahcene, A. S. Bell, B. K. Berger, G.
Bergmann, J. J. Bero, C. P. L. Berry, D. Bersanetti, A. Bertolini, J.
Betzwieser, S. Bhagwat, R. Bhandare, I. A. Bilenko, G. Billingsley, C. R.
Billman, J. Birch, R. Birney, O. Birnholtz, S. Biscans, S. Biscoveanu, A.
Bisht, M. Bitossi, C. Biwer, M. A. Bizouard, J. K. Blackburn, J. Blackman, C.
D. Blair, D. G. Blair, R. M. Blair, S. Bloemen, O. Bock, N. Bode, M. Boer, G.
Bogaert, A. Bohe, F. Bondu, E. Bonilla, R. Bonnand, B. A. Boom, R. Bork, V.
Boschi, S. Bose, K. Bossie, Y. Bouffanais, A. Bozzi, C. Bradaschia, P. R.
Brady, M. Branchesi, J. E. Brau, T. Briant, A. Brillet, M. Brinkmann, V.
Brisson, P. Brockill, J. E. Broida, A. F. Brooks, D. A. Brown, D. D. Brown,
S. Brunett, C. C. Buchanan, A. Buikema, T. Bulik, H. J. Bulten, A. Buonanno,
D. Buskulic, C. Buy, R. L. Byer, M. Cabero, L. Cadonati, G. Cagnoli, C.
Cahillane, J. Calder'on Bustillo, T. A. Callister, E. Calloni, J. B. Camp, P.
Canizares, K. C. Cannon, H. Cao, J. Cao, C. D. Capano, E. Capocasa, F.
Carbognani, S. Caride, M. F. Carney, J. Casanueva Diaz, C. Casentini, S.
Caudill, M. Cavagli\`a, F. Cavalier, R. Cavalieri, G. Cella, C. B. Cepeda, P.
Cerd'a-Dur'an, G. Cerretani, E. Cesarini, S. J. Chamberlin, M. Chan, S. Chao,
P. Charlton, E. Chase, E. Chassande-Mottin, D. Chatterjee, B. D. Cheeseboro,
H. Y. Chen, X. Chen, Y. Chen, H.-P. Cheng, H. Chia, A. Chincarini, A.
Chiummo, T. Chmiel, H. S. Cho, M. Cho, J. H. Chow, N. Christensen, Q. Chu, A.
J. K. Chua, S. Chua, A. K. W. Chung, S. Chung, G. Ciani, R. Ciolfi, C. E.
Cirelli, A. Cirone, F. Clara, J. A. Clark, P. Clearwater, F. Cleva, C.
Cocchieri, E. Coccia, P.-F. Cohadon, D. Cohen, A. Colla, C. G. Collette, L.
R. Cominsky, M. Constancio Jr., L. Conti, S. J. Cooper, P. Corban, T. R.
Corbitt, I. Cordero-Carri'on, K. R. Corley, N. Cornish, A. Corsi, S. Cortese,
C. A. Costa, M. W. Coughlin, S. B. Coughlin, J.-P. Coulon, S. T. Countryman,
P. Couvares, P. B. Covas, E. E. Cowan, D. M. Coward, M. J. Cowart, D. C.
Coyne, R. Coyne, J. D. E. Creighton, T. D. Creighton, J. Cripe, S. G.
Crowder, T. J. Cullen, A. Cumming, L. Cunningham, E. Cuoco, T. Dal Canton, G.
D'alya, S. L. Danilishin, S. D'Antonio, K. Danzmann, A. Dasgupta, C. F. Da
Silva Costa, V. Dattilo, I. Dave, M. Davier, D. Davis, E. J. Daw, B. Day, S.
De, D. DeBra, J. Degallaix, M. De Laurentis, S. Del'eglise, W. Del Pozzo, N.
Demos, T. Denker, T. Dent, R. De Pietri, V. Dergachev, R. De Rosa, R. T.
DeRosa, C. De Rossi, R. DeSalvo, O. de Varona, J. Devenson, S. Dhurandhar, M.
C. D'iaz, L. Di Fiore, M. Di Giovanni, T. Di Girolamo, A. Di Lieto, S. Di
Pace, I. Di Palma, F. Di Renzo, Z. Doctor, V. Dolique, F. Donovan, K. L.
Dooley, S. Doravari, I. Dorrington, R. Douglas, M. Dovale 'Alvarez, T. P.
Downes, M. Drago, C. Dreissigacker, J. C. Driggers, Z. Du, M. Ducrot, P.
Dupej, S. E. Dwyer, T. B. Edo, M. C. Edwards, A. Effler, H.-B. Eggenstein, P.
Ehrens, J. Eichholz, S. S. Eikenberry, R. A. Eisenstein, R. C. Essick, D.
Estevez, Z. B. Etienne, T. Etzel, M. Evans, T. M. Evans, M. Factourovich, V.
Fafone, H. Fair, S. Fairhurst, X. Fan, S. Farinon, B. Farr, W. M. Farr, E. J.
Fauchon-Jones, M. Favata, M. Fays, C. Fee, H. Fehrmann, J. Feicht, M. M.
Fejer, A. Fernandez-Galiana, I. Ferrante, E. C. Ferreira, F. Ferrini, F.
Fidecaro, D. Finstad, I. Fiori, D. Fiorucci, M. Fishbach, R. P. Fisher, M.
Fitz-Axen, R. Flaminio, M. Fletcher, H. Fong, J. A. Font, P. W. F. Forsyth,
S. S. Forsyth, J.-D. Fournier, S. Frasca, F. Frasconi, Z. Frei, A. Freise, R.
Frey, V. Frey, E. M. Fries, P. Fritschel, V. V. Frolov, P. Fulda, M. Fyffe,
H. Gabbard, B. U. Gadre, S. M. Gaebel, J. R. Gair, L. Gammaitoni, M. R.
Ganija, S. G. Gaonkar, C. Garcia-Quiros, F. Garufi, B. Gateley, S. Gaudio, G.
Gaur, V. Gayathri, N. Gehrels, G. Gemme, E. Genin, A. Gennai, D. George, J.
George, L. Gergely, V. Germain, S. Ghonge, Abhirup Ghosh, Archisman Ghosh, S.
Ghosh, J. A. Giaime, K. D. Giardina, A. Giazotto, K. Gill, L. Glover, E.
Goetz, R. Goetz, S. Gomes, B. Goncharov, G. Gonz'alez, J. M. Gonzalez Castro,
A. Gopakumar, M. L. Gorodetsky, S. E. Gossan, M. Gosselin, R. Gouaty, A.
Grado, C. Graef, M. Granata, A. Grant, S. Gras, C. Gray, G. Greco, A. C.
Green, E. M. Gretarsson, P. Groot, H. Grote, S. Grunewald, P. Gruning, G. M.
Guidi, X. Guo, A. Gupta, M. K. Gupta, K. E. Gushwa, E. K. Gustafson, R.
Gustafson, O. Halim, B. R. Hall, E. D. Hall, E. Z. Hamilton, G. Hammond, M.
Haney, M. M. Hanke, J. Hanks, C. Hanna, M. D. Hannam, O. A. Hannuksela, J.
Hanson, T. Hardwick, J. Harms, G. M. Harry, I. W. Harry, M. J. Hart, C.-J.
Haster, K. Haughian, J. Healy, A. Heidmann, M. C. Heintze, H. Heitmann, P.
Hello, G. Hemming, M. Hendry, I. S. Heng, J. Hennig, A. W. Heptonstall, M.
Heurs, S. Hild, T. Hinderer, W. C. G. Ho, D. Hoak, D. Hofman, K. Holt, D. E.
Holz, P. Hopkins, C. Horst, J. Hough, E. A. Houston, E. J. Howell, A. Hreibi,
Y. M. Hu, E. A. Huerta, D. Huet, B. Hughey, S. Husa, S. H. Huttner, T.
Huynh-Dinh, N. Indik, R. Inta, G. Intini, H. N. Isa, J.-M. Isac, M. Isi, B.
R. Iyer, K. Izumi, T. Jacqmin, K. Jani, P. Jaranowski, S. Jawahar, F.
Jim'enez-Forteza, W. W. Johnson, D. I. Jones, R. Jones, R. J. G. Jonker, L.
Ju, J. Junker, C. V. Kalaghatgi, V. Kalogera, B. Kamai, S. Kandhasamy, G.
Kang, J. B. Kanner, S. J. Kapadia, S. Karki, K. S. Karvinen, M. Kasprzack, M.
Katolik, E. Katsavounidis, W. Katzman, S. Kaufer, K. Kawabe, F. K'ef'elian,
D. Keitel, A. J. Kemball, R. Kennedy, C. Kent, J. S. Key, F. Y. Khalili, I.
Khan, S. Khan, Z. Khan, E. A. Khazanov, N. Kijbunchoo, Chunglee Kim, J. C.
Kim, K. Kim, W. Kim, W. S. Kim, Y.-M. Kim, S. J. Kimbrell, E. J. King, P. J.
King, M. Kinley-Hanlon, R. Kirchhoff, J. S. Kissel, L. Kleybolte, S.
Klimenko, T. D. Knowles, P. Koch, S. M. Koehlenbeck, S. Koley, V. Kondrashov,
A. Kontos, M. Korobko, W. Z. Korth, I. Kowalska, D. B. Kozak, C. Kr"amer, V.
Kringel, B. Krishnan, A. Kr'olak, G. Kuehn, P. Kumar, R. Kumar, S. Kumar, L.
Kuo, A. Kutynia, S. Kwang, B. D. Lackey, K. H. Lai, M. Landry, R. N. Lang, J.
Lange, B. Lantz, R. K. Lanza, A. Lartaux-Vollard, P. D. Lasky, M. Laxen, A.
Lazzarini, C. Lazzaro, P. Leaci, S. Leavey, C. H. Lee, H. K. Lee, H. M. Lee,
H. W. Lee, K. Lee, J. Lehmann, A. Lenon, M. Leonardi, N. Leroy, N. Letendre,
Y. Levin, T. G. F. Li, S. D. Linker, T. B. Littenberg, J. Liu, R. K. L. Lo,
N. A. Lockerbie, L. T. London, J. E. Lord, M. Lorenzini, V. Loriette, M.
Lormand, G. Losurdo, J. D. Lough, G. Lovelace, H. L\"uck, D. Lumaca, A. P.
Lundgren, R. Lynch, Y. Ma, R. Macas, S. Macfoy, B. Machenschalk, M. MacInnis,
D. M. Macleod, I. Maga\~na Hernandez, F. Maga\~na-Sandoval, L. Maga\~na
Zertuche, R. M. Magee, E. Majorana, I. Maksimovic, N. Man, V. Mandic, V.
Mangano, G. L. Mansell, M. Manske, M. Mantovani, F. Marchesoni, F. Marion, S.
M'arka, Z. M'arka, C. Markakis, A. S. Markosyan, A. Markowitz, E. Maros, A.
Marquina, F. Martelli, L. Martellini, I. W. Martin, R. M. Martin, D. V.
Martynov, K. Mason, E. Massera, A. Masserot, T. J. Massinger, M. Masso-Reid,
S. Mastrogiovanni, A. Matas, F. Matichard, L. Matone, N. Mavalvala, N.
Mazumder, R. McCarthy, D. E. McClelland, S. McCormick, L. McCuller, S. C.
McGuire, G. McIntyre, J. McIver, D. J. McManus, L. McNeill, T. McRae, S. T.
McWilliams, D. Meacher, G. D. Meadors, M. Mehmet, J. Meidam, E. Mejuto-Villa,
A. Melatos, G. Mendell, R. A. Mercer, E. L. Merilh, M. Merzougui, S. Meshkov,
C. Messenger, C. Messick, R. Metzdorff, P. M. Meyers, H. Miao, C. Michel, H.
Middleton, E. E. Mikhailov, L. Milano, A. L. Miller, B. B. Miller, J. Miller,
M. Millhouse, M. C. Milovich-Goff, O. Minazzoli, Y. Minenkov, J. Ming, C.
Mishra, S. Mitra, V. P. Mitrofanov, G. Mitselmakher, R. Mittleman, D. Moffa,
A. Moggi, K. Mogushi, M. Mohan, S. R. P. Mohapatra, M. Montani, C. J. Moore,
D. Moraru, G. Moreno, S. R. Morriss, B. Mours, C. M. Mow-Lowry, G. Mueller,
A. W. Muir, Arunava Mukherjee, D. Mukherjee, S. Mukherjee, N. Mukund, A.
Mullavey, J. Munch, E. A. Mu\~niz, M. Muratore, P. G. Murray, K. Napier, I.
Nardecchia, L. Naticchioni, R. K. Nayak, J. Neilson, G. Nelemans, T. J. N.
Nelson, M. Nery, A. Neunzert, L. Nevin, J. M. Newport, G. Newton, K. K. Y.
Ng, T. T. Nguyen, D. Nichols, A. B. Nielsen, S. Nissanke, A. Nitz, A. Noack,
F. Nocera, D. Nolting, C. North, L. K. Nuttall, J. Oberling, G. D. O'Dea, G.
H. Ogin, J. J. Oh, S. H. Oh, F. Ohme, M. A. Okada, M. Oliver, P. Oppermann,
Richard J. Oram, B. O'Reilly, R. Ormiston, L. F. Ortega, R. O'Shaughnessy, S.
Ossokine, D. J. Ottaway, H. Overmier, B. J. Owen, A. E. Pace, J. Page, M. A.
Page, A. Pai, S. A. Pai, J. R. Palamos, O. Palashov, C. Palomba, A.
Pal-Singh, Howard Pan, Huang-Wei Pan, B. Pang, P. T. H. Pang, C. Pankow, F.
Pannarale, B. C. Pant, F. Paoletti, A. Paoli, M. A. Papa, A. Parida, W.
Parker, D. Pascucci, A. Pasqualetti, R. Passaquieti, D. Passuello, M. Patil,
B. Patricelli, B. L. Pearlstone, M. Pedraza, R. Pedurand, L. Pekowsky, A.
Pele, S. Penn, C. J. Perez, A. Perreca, L. M. Perri, H. P. Pfeiffer, M.
Phelps, O. J. Piccinni, M. Pichot, F. Piergiovanni, V. Pierro, G. Pillant, L.
Pinard, I. M. Pinto, M. Pirello, M. Pitkin, M. Poe, R. Poggiani, P.
Popolizio, E. K. Porter, A. Post, J. Powell, J. Prasad, J. W. W. Pratt, G.
Pratten, V. Predoi, T. Prestegard, M. Prijatelj, M. Principe, S. Privitera,
G. A. Prodi, L. G. Prokhorov, O. Puncken, M. Punturo, P. Puppo, M. P"urrer,
H. Qi, V. Quetschke, E. A. Quintero, R. Quitzow-James, F. J. Raab, D. S.
Rabeling, H. Radkins, P. Raffai, S. Raja, C. Rajan, B. Rajbhandari, M.
Rakhmanov, K. E. Ramirez, A. Ramos-Buades, P. Rapagnani, V. Raymond, M.
Razzano, J. Read, T. Regimbau, L. Rei, S. Reid, D. H. Reitze, W. Ren, S. D.
Reyes, F. Ricci, P. M. Ricker, S. Rieger, K. Riles, M. Rizzo, N. A.
Robertson, R. Robie, F. Robinet, A. Rocchi, L. Rolland, J. G. Rollins, V. J.
Roma, R. Romano, C. L. Romel, J. H. Romie, D. Rosi'nska, M. P. Ross, S.
Rowan, A. R"udiger, P. Ruggi, G. Rutins, K. Ryan, S. Sachdev, T. Sadecki, L.
Sadeghian, M. Sakellariadou, L. Salconi, M. Saleem, F. Salemi, A. Samajdar,
L. Sammut, L. M. Sampson, E. J. Sanchez, L. E. Sanchez, N. Sanchis-Gual, V.
Sandberg, J. R. Sanders, B. Sassolas, B. S. Sathyaprakash, P. R. Saulson, O.
Sauter, R. L. Savage, A. Sawadsky, P. Schale, M. Scheel, J. Scheuer, J.
Schmidt, P. Schmidt, R. Schnabel, R. M. S. Schofield, A. Sch"onbeck, E.
Schreiber, D. Schuette, B. W. Schulte, B. F. Schutz, S. G. Schwalbe, J.
Scott, S. M. Scott, E. Seidel, D. Sellers, A. S. Sengupta, D. Sentenac, V.
Sequino, A. Sergeev, D. A. Shaddock, T. J. Shaffer, A. A. Shah, M. S.
Shahriar, M. B. Shaner, L. Shao, B. Shapiro, P. Shawhan, A. Sheperd, D. H.
Shoemaker, D. M. Shoemaker, K. Siellez, X. Siemens, M. Sieniawska, D. Sigg,
A. D. Silva, L. P. Singer, A. Singh, A. Singhal, A. M. Sintes, B. J. J.
Slagmolen, B. Smith, J. R. Smith, R. J. E. Smith, S. Somala, E. J. Son, J. A.
Sonnenberg, B. Sorazu, F. Sorrentino, T. Souradeep, A. P. Spencer, A. K.
Srivastava, K. Staats, A. Staley, M. Steinke, J. Steinlechner, S.
Steinlechner, D. Steinmeyer, S. P. Stevenson, R. Stone, D. J. Stops, K. A.
Strain, G. Stratta, S. E. Strigin, A. Strunk, R. Sturani, A. L. Stuver, T. Z.
Summerscales, L. Sun, S. Sunil, J. Suresh, P. J. Sutton, B. L. Swinkels, M.
J. Szczepa'nczyk, M. Tacca, S. C. Tait, C. Talbot, D. Talukder, D. B. Tanner,
M. T'apai, A. Taracchini, J. D. Tasson, J. A. Taylor, R. Taylor, S. V.
Tewari, T. Theeg, F. Thies, E. G. Thomas, M. Thomas, P. Thomas, K. A. Thorne,
E. Thrane, S. Tiwari, V. Tiwari, K. V. Tokmakov, K. Toland, M. Tonelli, Z.
Tornasi, A. Torres-Forn'e, C. I. Torrie, D. T"oyr"a, F. Travasso, G. Traylor,
J. Trinastic, M. C. Tringali, L. Trozzo, K. W. Tsang, M. Tse, R. Tso, L.
Tsukada, D. Tsuna, D. Tuyenbayev, K. Ueno, D. Ugolini, C. S. Unnikrishnan, A.
L. Urban, S. A. Usman, H. Vahlbruch, G. Vajente, G. Valdes, N. van Bakel, M.
van Beuzekom, J. F. J. van den Brand, C. Van Den Broeck, D. C. Vander-Hyde,
L. van der Schaaf, J. V. van Heijningen, A. A. van Veggel, M. Vardaro, V.
Varma, S. Vass, M. Vas'uth, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch,
K. Venkateswara, G. Venugopalan, D. Verkindt, F. Vetrano, A. Vicer'e, A. D.
Viets, S. Vinciguerra, D. J. Vine, J.-Y. Vinet, S. Vitale, T. Vo, H. Vocca,
C. Vorvick, S. P. Vyatchanin, A. R. Wade, L. E. Wade, M. Wade, R. Walet, M.
Walker, L. Wallace, S. Walsh, G. Wang, H. Wang, J. Z. Wang, W. H. Wang, Y. F.
Wang, R. L. Ward, J. Warner, M. Was, J. Watchi, B. Weaver, L.-W. Wei, M.
Weinert, A. J. Weinstein, R. Weiss, L. Wen, E. K. Wessel, P. Wessels, J.
Westerweck, T. Westphal, K. Wette, J. T. Whelan, B. F. Whiting, C. Whittle,
D. Wilken, D. Williams, R. D. Williams, A. R. Williamson, J. L. Willis, B.
Willke, M. H. Wimmer, W. Winkler, C. C. Wipf, H. Wittel, G. Woan, J. Woehler,
J. Wofford, K. W. K. Wong, J. Worden, J. L. Wright, D. S. Wu, D. M. Wysocki,
S. Xiao, H. Yamamoto, C. C. Yancey, L. Yang, M. J. Yap, M. Yazback, Hang Yu,
Haocun Yu, M. Yvert, A. Zadro.zny, M. Zanolin, T. Zelenova, J.-P. Zendri, M.
Zevin, L. Zhang, M. Zhang, T. Zhang, Y.-H. Zhang, C. Zhao, M. Zhou, Z. Zhou,
S. J. Zhu, X. J. Zhu, M. E. Zucker, J. Zweizig | First narrow-band search for continuous gravitational waves from known
pulsars in advanced detector data | 9 Figures, 7 tables, submitted to PRD | Phys. Rev. D 96, 122006 (2017) | 10.1103/PhysRevD.96.122006 | null | gr-qc astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Spinning neutron stars asymmetric with respect to their rotation axis are
potential sources of continuous gravitational waves for ground-based
interferometric detectors. In the case of known pulsars a fully coherent
search, based on matched filtering, which uses the position and rotational
parameters obtained from electromagnetic observations, can be carried out.
Matched filtering maximizes the signal-to-noise (SNR) ratio, but a large
sensitivity loss is expected in case of even a very small mismatch between the
assumed and the true signal parameters. For this reason, {\it narrow-band}
analyses methods have been developed, allowing a fully coherent search for
gravitational waves from known pulsars over a fraction of a hertz and several
spin-down values. In this paper we describe a narrow-band search of eleven
pulsars using data from Advanced LIGO's first observing run. Although we have
found several initial outliers, further studies show no significant evidence
for the presence of a gravitational wave signal. Finally, we have placed upper
limits on the signal strain amplitude lower than the spin-down limit for 5 of
the 11 targets over the bands searched: in the case of J1813-1749 the spin-down
limit has been beaten for the first time. For an additional 3 targets, the
median upper limit across the search bands is below the spin-down limit. This
is the most sensitive narrow-band search for continuous gravitational waves
carried out so far.
| [
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"M. B.",
""
],
[
"Shao",
"L.",
""
],
[
"Shapiro",
"B.",
""
],
[
"Shawhan",
"P.",
""
],
[
"Sheperd",
"A.",
""
],
[
"Shoemaker",
"D. H.",
""
],
[
"Shoemaker",
"D. M.",
""
],
[
"Siellez",
"K.",
""
],
[
"Siemens",
"X.",
""
],
[
"Sieniawska",
"M.",
""
],
[
"Sigg",
"D.",
""
],
[
"Silva",
"A. D.",
""
],
[
"Singer",
"L. P.",
""
],
[
"Singh",
"A.",
""
],
[
"Singhal",
"A.",
""
],
[
"Sintes",
"A. M.",
""
],
[
"Slagmolen",
"B. J. J.",
""
],
[
"Smith",
"B.",
""
],
[
"Smith",
"J. R.",
""
],
[
"Smith",
"R. J. E.",
""
],
[
"Somala",
"S.",
""
],
[
"Son",
"E. J.",
""
],
[
"Sonnenberg",
"J. A.",
""
],
[
"Sorazu",
"B.",
""
],
[
"Sorrentino",
"F.",
""
],
[
"Souradeep",
"T.",
""
],
[
"Spencer",
"A. P.",
""
],
[
"Srivastava",
"A. K.",
""
],
[
"Staats",
"K.",
""
],
[
"Staley",
"A.",
""
],
[
"Steinke",
"M.",
""
],
[
"Steinlechner",
"J.",
""
],
[
"Steinlechner",
"S.",
""
],
[
"Steinmeyer",
"D.",
""
],
[
"Stevenson",
"S. P.",
""
],
[
"Stone",
"R.",
""
],
[
"Stops",
"D. J.",
""
],
[
"Strain",
"K. A.",
""
],
[
"Stratta",
"G.",
""
],
[
"Strigin",
"S. E.",
""
],
[
"Strunk",
"A.",
""
],
[
"Sturani",
"R.",
""
],
[
"Stuver",
"A. L.",
""
],
[
"Summerscales",
"T. Z.",
""
],
[
"Sun",
"L.",
""
],
[
"Sunil",
"S.",
""
],
[
"Suresh",
"J.",
""
],
[
"Sutton",
"P. J.",
""
],
[
"Swinkels",
"B. L.",
""
],
[
"Szczepa'nczyk",
"M. J.",
""
],
[
"Tacca",
"M.",
""
],
[
"Tait",
"S. C.",
""
],
[
"Talbot",
"C.",
""
],
[
"Talukder",
"D.",
""
],
[
"Tanner",
"D. B.",
""
],
[
"T'apai",
"M.",
""
],
[
"Taracchini",
"A.",
""
],
[
"Tasson",
"J. D.",
""
],
[
"Taylor",
"J. A.",
""
],
[
"Taylor",
"R.",
""
],
[
"Tewari",
"S. V.",
""
],
[
"Theeg",
"T.",
""
],
[
"Thies",
"F.",
""
],
[
"Thomas",
"E. G.",
""
],
[
"Thomas",
"M.",
""
],
[
"Thomas",
"P.",
""
],
[
"Thorne",
"K. A.",
""
],
[
"Thrane",
"E.",
""
],
[
"Tiwari",
"S.",
""
],
[
"Tiwari",
"V.",
""
],
[
"Tokmakov",
"K. V.",
""
],
[
"Toland",
"K.",
""
],
[
"Tonelli",
"M.",
""
],
[
"Tornasi",
"Z.",
""
],
[
"Torres-Forn'e",
"A.",
""
],
[
"Torrie",
"C. I.",
""
],
[
"T\"oyr\"a",
"D.",
""
],
[
"Travasso",
"F.",
""
],
[
"Traylor",
"G.",
""
],
[
"Trinastic",
"J.",
""
],
[
"Tringali",
"M. C.",
""
],
[
"Trozzo",
"L.",
""
],
[
"Tsang",
"K. W.",
""
],
[
"Tse",
"M.",
""
],
[
"Tso",
"R.",
""
],
[
"Tsukada",
"L.",
""
],
[
"Tsuna",
"D.",
""
],
[
"Tuyenbayev",
"D.",
""
],
[
"Ueno",
"K.",
""
],
[
"Ugolini",
"D.",
""
],
[
"Unnikrishnan",
"C. S.",
""
],
[
"Urban",
"A. L.",
""
],
[
"Usman",
"S. A.",
""
],
[
"Vahlbruch",
"H.",
""
],
[
"Vajente",
"G.",
""
],
[
"Valdes",
"G.",
""
],
[
"van Bakel",
"N.",
""
],
[
"van Beuzekom",
"M.",
""
],
[
"Brand",
"J. F. J. van den",
""
],
[
"Broeck",
"C. Van Den",
""
],
[
"Vander-Hyde",
"D. C.",
""
],
[
"van der Schaaf",
"L.",
""
],
[
"van Heijningen",
"J. V.",
""
],
[
"van Veggel",
"A. A.",
""
],
[
"Vardaro",
"M.",
""
],
[
"Varma",
"V.",
""
],
[
"Vass",
"S.",
""
],
[
"Vas'uth",
"M.",
""
],
[
"Vecchio",
"A.",
""
],
[
"Vedovato",
"G.",
""
],
[
"Veitch",
"J.",
""
],
[
"Veitch",
"P. J.",
""
],
[
"Venkateswara",
"K.",
""
],
[
"Venugopalan",
"G.",
""
],
[
"Verkindt",
"D.",
""
],
[
"Vetrano",
"F.",
""
],
[
"Vicer'e",
"A.",
""
],
[
"Viets",
"A. D.",
""
],
[
"Vinciguerra",
"S.",
""
],
[
"Vine",
"D. J.",
""
],
[
"Vinet",
"J. -Y.",
""
],
[
"Vitale",
"S.",
""
],
[
"Vo",
"T.",
""
],
[
"Vocca",
"H.",
""
],
[
"Vorvick",
"C.",
""
],
[
"Vyatchanin",
"S. P.",
""
],
[
"Wade",
"A. R.",
""
],
[
"Wade",
"L. E.",
""
],
[
"Wade",
"M.",
""
],
[
"Walet",
"R.",
""
],
[
"Walker",
"M.",
""
],
[
"Wallace",
"L.",
""
],
[
"Walsh",
"S.",
""
],
[
"Wang",
"G.",
""
],
[
"Wang",
"H.",
""
],
[
"Wang",
"J. Z.",
""
],
[
"Wang",
"W. H.",
""
],
[
"Wang",
"Y. F.",
""
],
[
"Ward",
"R. L.",
""
],
[
"Warner",
"J.",
""
],
[
"Was",
"M.",
""
],
[
"Watchi",
"J.",
""
],
[
"Weaver",
"B.",
""
],
[
"Wei",
"L. -W.",
""
],
[
"Weinert",
"M.",
""
],
[
"Weinstein",
"A. J.",
""
],
[
"Weiss",
"R.",
""
],
[
"Wen",
"L.",
""
],
[
"Wessel",
"E. K.",
""
],
[
"Wessels",
"P.",
""
],
[
"Westerweck",
"J.",
""
],
[
"Westphal",
"T.",
""
],
[
"Wette",
"K.",
""
],
[
"Whelan",
"J. T.",
""
],
[
"Whiting",
"B. F.",
""
],
[
"Whittle",
"C.",
""
],
[
"Wilken",
"D.",
""
],
[
"Williams",
"D.",
""
],
[
"Williams",
"R. D.",
""
],
[
"Williamson",
"A. R.",
""
],
[
"Willis",
"J. L.",
""
],
[
"Willke",
"B.",
""
],
[
"Wimmer",
"M. H.",
""
],
[
"Winkler",
"W.",
""
],
[
"Wipf",
"C. C.",
""
],
[
"Wittel",
"H.",
""
],
[
"Woan",
"G.",
""
],
[
"Woehler",
"J.",
""
],
[
"Wofford",
"J.",
""
],
[
"Wong",
"K. W. K.",
""
],
[
"Worden",
"J.",
""
],
[
"Wright",
"J. L.",
""
],
[
"Wu",
"D. S.",
""
],
[
"Wysocki",
"D. M.",
""
],
[
"Xiao",
"S.",
""
],
[
"Yamamoto",
"H.",
""
],
[
"Yancey",
"C. C.",
""
],
[
"Yang",
"L.",
""
],
[
"Yap",
"M. J.",
""
],
[
"Yazback",
"M.",
""
],
[
"Yu",
"Hang",
""
],
[
"Yu",
"Haocun",
""
],
[
"Yvert",
"M.",
""
],
[
"zny",
"A. Zadro.",
""
],
[
"Zanolin",
"M.",
""
],
[
"Zelenova",
"T.",
""
],
[
"Zendri",
"J. -P.",
""
],
[
"Zevin",
"M.",
""
],
[
"Zhang",
"L.",
""
],
[
"Zhang",
"M.",
""
],
[
"Zhang",
"T.",
""
],
[
"Zhang",
"Y. -H.",
""
],
[
"Zhao",
"C.",
""
],
[
"Zhou",
"M.",
""
],
[
"Zhou",
"Z.",
""
],
[
"Zhu",
"S. J.",
""
],
[
"Zhu",
"X. J.",
""
],
[
"Zucker",
"M. E.",
""
],
[
"Zweizig",
"J.",
""
]
] | Spinning neutron stars asymmetric with respect to their rotation axis are potential sources of continuous gravitational waves for ground-based interferometric detectors. In the case of known pulsars a fully coherent search, based on matched filtering, which uses the position and rotational parameters obtained from electromagnetic observations, can be carried out. Matched filtering maximizes the signal-to-noise (SNR) ratio, but a large sensitivity loss is expected in case of even a very small mismatch between the assumed and the true signal parameters. For this reason, {\it narrow-band} analyses methods have been developed, allowing a fully coherent search for gravitational waves from known pulsars over a fraction of a hertz and several spin-down values. In this paper we describe a narrow-band search of eleven pulsars using data from Advanced LIGO's first observing run. Although we have found several initial outliers, further studies show no significant evidence for the presence of a gravitational wave signal. Finally, we have placed upper limits on the signal strain amplitude lower than the spin-down limit for 5 of the 11 targets over the bands searched: in the case of J1813-1749 the spin-down limit has been beaten for the first time. For an additional 3 targets, the median upper limit across the search bands is below the spin-down limit. This is the most sensitive narrow-band search for continuous gravitational waves carried out so far. |
1602.05609 | Daniel Boyanovsky | Daniel Boyanovsky | Fermionic influence (action) on inflationary fluctuations | matches published version. arXiv admin note: text overlap with
arXiv:1511.06649 | Phys. Rev. D 93, 083507 (2016) | 10.1103/PhysRevD.93.083507 | null | gr-qc astro-ph.CO hep-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Motivated by apparent persistent large scale anomalies in the CMB we study
the influence of fermionic degrees of freedom on the dynamics of inflaton
fluctuations as a possible source of violations of (nearly) scale invariance on
cosmological scales. We obtain the non-equilibrium effective action of an
inflaton-like scalar field with Yukawa interactions ($Y_{D,M}$) to light
\emph{fermionic} degrees of freedom both for Dirac and Majorana fields in de
Sitter space-time. The effective action leads to Langevin equations of motion
for the fluctuations of the inflaton-like field, with self-energy corrections
and a stochastic gaussian noise. We solve the Langevin equation in the
super-Hubble limit implementing a dynamical renormalization group resummation.
For a nearly massless inflaton its power spectrum of super Hubble fluctuations
is \emph{enhanced}, $\mathcal{P}(k;\eta) =
(\frac{H}{2\pi})^2\,e^{\gamma_t[-k\eta] }$ with $\gamma_t[-k\eta] =
\frac{1}{6\pi^2}
\Big[\sum_{i=1}^{N_D}{Y^2_{i,D}}+2\sum_{j=1}^{N_M}{Y^2_{j,M}}\Big]\,\Big\{\ln^2[-k\eta]-2
\ln[-k\eta]\ln[ -k\eta_0] \Big\} $ for $N_D$ Dirac and $N_M$ Majorana fermions,
and $\eta_0$ is the renormalization scale at which the inflaton mass vanishes.
The full power spectrum is shown to be renormalization group invariant. These
corrections to the super-Hubble power spectrum entail a violation of scale
invariance as a consequence of the coupling to the fermionic fields. The
effective action is argued to be \emph{exact} in a limit of large number of
fermionic fields. A cancellation between the enhancement from fermionic degrees
of freedom and suppression from light scalar degrees of freedom
\emph{conformally coupled to gravity} suggests the possibility of a finely
tuned \emph{supersymmetry} among these fields.
| [
{
"created": "Wed, 17 Feb 2016 21:53:23 GMT",
"version": "v1"
},
{
"created": "Wed, 13 Apr 2016 14:00:54 GMT",
"version": "v2"
}
] | 2016-04-20 | [
[
"Boyanovsky",
"Daniel",
""
]
] | Motivated by apparent persistent large scale anomalies in the CMB we study the influence of fermionic degrees of freedom on the dynamics of inflaton fluctuations as a possible source of violations of (nearly) scale invariance on cosmological scales. We obtain the non-equilibrium effective action of an inflaton-like scalar field with Yukawa interactions ($Y_{D,M}$) to light \emph{fermionic} degrees of freedom both for Dirac and Majorana fields in de Sitter space-time. The effective action leads to Langevin equations of motion for the fluctuations of the inflaton-like field, with self-energy corrections and a stochastic gaussian noise. We solve the Langevin equation in the super-Hubble limit implementing a dynamical renormalization group resummation. For a nearly massless inflaton its power spectrum of super Hubble fluctuations is \emph{enhanced}, $\mathcal{P}(k;\eta) = (\frac{H}{2\pi})^2\,e^{\gamma_t[-k\eta] }$ with $\gamma_t[-k\eta] = \frac{1}{6\pi^2} \Big[\sum_{i=1}^{N_D}{Y^2_{i,D}}+2\sum_{j=1}^{N_M}{Y^2_{j,M}}\Big]\,\Big\{\ln^2[-k\eta]-2 \ln[-k\eta]\ln[ -k\eta_0] \Big\} $ for $N_D$ Dirac and $N_M$ Majorana fermions, and $\eta_0$ is the renormalization scale at which the inflaton mass vanishes. The full power spectrum is shown to be renormalization group invariant. These corrections to the super-Hubble power spectrum entail a violation of scale invariance as a consequence of the coupling to the fermionic fields. The effective action is argued to be \emph{exact} in a limit of large number of fermionic fields. A cancellation between the enhancement from fermionic degrees of freedom and suppression from light scalar degrees of freedom \emph{conformally coupled to gravity} suggests the possibility of a finely tuned \emph{supersymmetry} among these fields. |
gr-qc/0606023 | Yaneer Bar-Yam | Yaneer Bar-Yam | ZM theory IV: Introduction to quantum concepts, Klein-Gordon and Dirac's
equations | 28 pages, 0 figures | null | null | NECSI Report 2006-06-01 | gr-qc hep-th | null | We describe a general approach to the correspondence of ZM theory with
quantum electrodynamics. As a first step, we show the correspondence of helical
clock-field states with plane wave states of the Dirac equation. Specifically,
defining the direction of time as the gradient of the field in the combined
field and space dimensions, for constant gradients, results in states that are
consistent with conventional plane wave Dirac equation eigenfunctions.
Particles and antiparticles, as well as up and down spins are related by axis
inversions. The Dirac wavefunction represents the clock-field and the observer
defined direction of time and spatial coordinate axes rotation relative to the
region of observation. Additional steps showing the correspondence of ZM theory
to quantum mechanics and the Dirac equation are deferred to subsequent papers.
| [
{
"created": "Mon, 5 Jun 2006 02:32:46 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Bar-Yam",
"Yaneer",
""
]
] | We describe a general approach to the correspondence of ZM theory with quantum electrodynamics. As a first step, we show the correspondence of helical clock-field states with plane wave states of the Dirac equation. Specifically, defining the direction of time as the gradient of the field in the combined field and space dimensions, for constant gradients, results in states that are consistent with conventional plane wave Dirac equation eigenfunctions. Particles and antiparticles, as well as up and down spins are related by axis inversions. The Dirac wavefunction represents the clock-field and the observer defined direction of time and spatial coordinate axes rotation relative to the region of observation. Additional steps showing the correspondence of ZM theory to quantum mechanics and the Dirac equation are deferred to subsequent papers. |
1506.05813 | Ambrish Raghoonundun | Ambrish M. Raghoonundun and David W. Hobill | Possible Physical Realizations of the Tolman VII solution | Accepted and published in PRD | Phys. Rev. D 92(12) 124005 | 10.1103/PhysRevD.92.124005 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Tolman VII solution (an exact static spherically symmetric perfect fluid
solution) to the Einstein equations is reexamined, and a closed form equation
of state (EOS) is deduced for the first time. This EOS allows further analysis
leading to a viable model for compact stars to be obtained. Explicit
application of causality conditions places further constraints on the model,
and recent measurements of masses and radii of neutron stars prove to be within
the predictions of the model. It is found that the adiabatic index ${\gamma}
\geq 2$, and self-bound crust solutions are not excluded. The solution is also
shown to obey known stability criteria. It is argued that this solution
provides realistic limits on models of compact stars.
| [
{
"created": "Thu, 18 Jun 2015 20:23:15 GMT",
"version": "v1"
},
{
"created": "Tue, 1 Dec 2015 21:26:47 GMT",
"version": "v2"
}
] | 2015-12-03 | [
[
"Raghoonundun",
"Ambrish M.",
""
],
[
"Hobill",
"David W.",
""
]
] | The Tolman VII solution (an exact static spherically symmetric perfect fluid solution) to the Einstein equations is reexamined, and a closed form equation of state (EOS) is deduced for the first time. This EOS allows further analysis leading to a viable model for compact stars to be obtained. Explicit application of causality conditions places further constraints on the model, and recent measurements of masses and radii of neutron stars prove to be within the predictions of the model. It is found that the adiabatic index ${\gamma} \geq 2$, and self-bound crust solutions are not excluded. The solution is also shown to obey known stability criteria. It is argued that this solution provides realistic limits on models of compact stars. |
0812.0012 | Yi-Zen Chu | Yi-Zen Chu | The n-body problem in General Relativity up to the second post-Newtonian
order from perturbative field theory | 39 pages. The Mathematica code used in this paper can be found at
http://www.stargazing.net/yizen/PN.html Version 2: Slight re-wording of
section on removal of accelerations in 2 PN lagrangian; comments added in
conclusion; and typographical errors fixed. Article is similar to that
published in PRD | Phys.Rev.D79:044031,2009 | 10.1103/PhysRevD.79.044031 | null | gr-qc astro-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Motivated by experimental probes of general relativity, we adopt methods from
perturbative (quantum) field theory to compute, up to certain integrals, the
effective lagrangian for its n-body problem. Perturbation theory is performed
about a background Minkowski spacetime to O[(v/c)^4] beyond Newtonian gravity,
where v is the typical speed of these n particles in their center of energy
frame. For the specific case of the 2 body problem, the major efforts underway
to measure gravitational waves produced by in-spiraling compact astrophysical
binaries require their gravitational interactions to be computed beyond the
currently known O[(v/c)^7]. We argue that such higher order post-Newtonian
calculations must be automated for these field theoretic methods to be applied
successfully to achieve this goal. In view of this, we outline an algorithm
that would in principle generate the relevant Feynman diagrams to an arbitrary
order in v/c and take steps to develop the necessary software. The Feynman
diagrams contributing to the n-body effective action at O[(v/c)^6] beyond
Newton are derived.
| [
{
"created": "Sat, 29 Nov 2008 02:15:09 GMT",
"version": "v1"
},
{
"created": "Wed, 25 Feb 2009 17:19:46 GMT",
"version": "v2"
}
] | 2009-03-12 | [
[
"Chu",
"Yi-Zen",
""
]
] | Motivated by experimental probes of general relativity, we adopt methods from perturbative (quantum) field theory to compute, up to certain integrals, the effective lagrangian for its n-body problem. Perturbation theory is performed about a background Minkowski spacetime to O[(v/c)^4] beyond Newtonian gravity, where v is the typical speed of these n particles in their center of energy frame. For the specific case of the 2 body problem, the major efforts underway to measure gravitational waves produced by in-spiraling compact astrophysical binaries require their gravitational interactions to be computed beyond the currently known O[(v/c)^7]. We argue that such higher order post-Newtonian calculations must be automated for these field theoretic methods to be applied successfully to achieve this goal. In view of this, we outline an algorithm that would in principle generate the relevant Feynman diagrams to an arbitrary order in v/c and take steps to develop the necessary software. The Feynman diagrams contributing to the n-body effective action at O[(v/c)^6] beyond Newton are derived. |
2201.04135 | Konstantin Zloshchastiev | Konstantin G. Zloshchastiev | On asymptotic behaviour of galactic rotation curves in superfluid vacuum
theory | 5 pages, 1 figure | Astron. Rep. 65, 1078 (2021) | 10.1134/S1063772921100437 | null | gr-qc astro-ph.GA | http://creativecommons.org/licenses/by/4.0/ | The logarithmic superfluid theory of physical vacuum predicts that gravity is
an induced phenomenon, which has a multiple-scale structure. At astronomical
scales, as the distance from a gravitating center increases, gravitational
potential and corresponding spacetime metric are dominated by a Newtonian
(Schwarzschild) term, followed by a logarithmic term, finally by linear and
quadratic (de Sitter) terms. Correspondingly, rotation curves are predicted to
be Keplerian in the inner regions of galaxies, mostly flat in the outer
regions, and non-flat in the utmost outer regions. We compare theory's
predictions with the furthest rotation curves data points available for a
number of galaxies: using a two-parameter fit, we perform a preliminary
estimate which disregards the combined effect of gas and stellar disc, but is
relatively simple and uses minimal assumptions for galactic luminous matter.
The data strongly points out at the existence of a crossover transition from
flat to non-flat regimes at galactic outskirts.
| [
{
"created": "Tue, 11 Jan 2022 08:30:32 GMT",
"version": "v1"
}
] | 2022-01-13 | [
[
"Zloshchastiev",
"Konstantin G.",
""
]
] | The logarithmic superfluid theory of physical vacuum predicts that gravity is an induced phenomenon, which has a multiple-scale structure. At astronomical scales, as the distance from a gravitating center increases, gravitational potential and corresponding spacetime metric are dominated by a Newtonian (Schwarzschild) term, followed by a logarithmic term, finally by linear and quadratic (de Sitter) terms. Correspondingly, rotation curves are predicted to be Keplerian in the inner regions of galaxies, mostly flat in the outer regions, and non-flat in the utmost outer regions. We compare theory's predictions with the furthest rotation curves data points available for a number of galaxies: using a two-parameter fit, we perform a preliminary estimate which disregards the combined effect of gas and stellar disc, but is relatively simple and uses minimal assumptions for galactic luminous matter. The data strongly points out at the existence of a crossover transition from flat to non-flat regimes at galactic outskirts. |
0709.3074 | Patrick Peter | F. Finelli, P. Peter and N. Pinto-Neto | Spectra of primordial fluctuations in two-perfect-fluid regular bounces | 11 pages, 5 figures | Phys.Rev.D77:103508,2008 | 10.1103/PhysRevD.77.103508 | null | gr-qc | null | We introduce analytic solutions for a class of two components bouncing
models, where the bounce is triggered by a negative energy density perfect
fluid. The equation of state of the two components are constant in time, but
otherwise unrelated. By numerically integrating regular equations for scalar
cosmological perturbations, we find that the (would be) growing mode of the
Newtonian potential before the bounce never matches with the the growing mode
in the expanding stage. For the particular case of a negative energy density
component with a stiff equation of state we give a detailed analytic study,
which is in complete agreement with the numerical results. We also perform
analytic and numerical calculations for long wavelength tensor perturbations,
obtaining that, in most cases of interest, the tensor spectral index is
independent of the negative energy fluid and given by the spectral index of the
growing mode in the contracting stage. We compare our results with previous
investigations in the literature.
| [
{
"created": "Wed, 19 Sep 2007 17:24:00 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Finelli",
"F.",
""
],
[
"Peter",
"P.",
""
],
[
"Pinto-Neto",
"N.",
""
]
] | We introduce analytic solutions for a class of two components bouncing models, where the bounce is triggered by a negative energy density perfect fluid. The equation of state of the two components are constant in time, but otherwise unrelated. By numerically integrating regular equations for scalar cosmological perturbations, we find that the (would be) growing mode of the Newtonian potential before the bounce never matches with the the growing mode in the expanding stage. For the particular case of a negative energy density component with a stiff equation of state we give a detailed analytic study, which is in complete agreement with the numerical results. We also perform analytic and numerical calculations for long wavelength tensor perturbations, obtaining that, in most cases of interest, the tensor spectral index is independent of the negative energy fluid and given by the spectral index of the growing mode in the contracting stage. We compare our results with previous investigations in the literature. |
1310.8312 | Pierre-Henry Lambert | Pierre-Henry Lambert | Introduction to Black Hole Evaporation | 31 pages, 13 figures, 1 table. Conference proceedings. v2: misprints
corrected | PoS(Modave 2013)001 | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | These lecture notes are an elementary and pedagogical introduction to the
black hole evaporation, based on a lecture given by the author at the Ninth
Modave Summer School in Mathematical Physics and are intended for PhD students.
First, quantum field theory in curved spacetime is studied and tools needed for
the remaining of the course are introduced. Then, quantum field theory in
Rindler spacetime in 1+1 dimensions and in the spacetime of a spherically
collapsing star are considered, leading to Unruh and Hawking effects,
respectively. Finally, some consequences such as thermodynamics of black holes
and information loss paradox are discussed.
| [
{
"created": "Wed, 30 Oct 2013 20:21:07 GMT",
"version": "v1"
},
{
"created": "Thu, 16 Jan 2014 16:06:16 GMT",
"version": "v2"
}
] | 2014-01-17 | [
[
"Lambert",
"Pierre-Henry",
""
]
] | These lecture notes are an elementary and pedagogical introduction to the black hole evaporation, based on a lecture given by the author at the Ninth Modave Summer School in Mathematical Physics and are intended for PhD students. First, quantum field theory in curved spacetime is studied and tools needed for the remaining of the course are introduced. Then, quantum field theory in Rindler spacetime in 1+1 dimensions and in the spacetime of a spherically collapsing star are considered, leading to Unruh and Hawking effects, respectively. Finally, some consequences such as thermodynamics of black holes and information loss paradox are discussed. |
1212.0263 | James Kentosh | James Kentosh | Localized gravitational energy in a Schwarzschild field | 10 pages, 2 figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | An interpretation of general relativity is developed in which the energy used
to lift a body in a static gravitational field increases its rest mass.
Observers at different gravitational potentials would experience different mass
reference frames. It is shown that bodies falling in a Schwarzschild field
exhibit the relativistic mass/energy relationship from special relativity. This
new result is independent of the choice of coordinates. The proposed approach
provides a physical explanation for gravitational energy, which is localized as
a scalar function intrinsic to general relativity. Applying this model to the
Robertson-Walker metric demonstrates that time-varying fields induce a net
energy transfer between bodies that is not exhibited in static fields.
| [
{
"created": "Tue, 27 Nov 2012 05:44:51 GMT",
"version": "v1"
}
] | 2012-12-04 | [
[
"Kentosh",
"James",
""
]
] | An interpretation of general relativity is developed in which the energy used to lift a body in a static gravitational field increases its rest mass. Observers at different gravitational potentials would experience different mass reference frames. It is shown that bodies falling in a Schwarzschild field exhibit the relativistic mass/energy relationship from special relativity. This new result is independent of the choice of coordinates. The proposed approach provides a physical explanation for gravitational energy, which is localized as a scalar function intrinsic to general relativity. Applying this model to the Robertson-Walker metric demonstrates that time-varying fields induce a net energy transfer between bodies that is not exhibited in static fields. |
2103.07342 | Abhik Kumar Sanyal Dr. | A. Banerjee, S. B. Duttachoudhury and Abhik Kumar Sanyal | Bianchi type I cosmological model with a viscous fluid | 9 pages, 0 figures | Journal of Mathematical Physics 26, 3010 (1985) | 10.1063/1.526676 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Bianchi I cosmological models consisting of a fluid with both bulk and shear
viscosity are studied. It is shown how the dynamical importance of the shear
and the fluid density change in the course of evolution. Exact solutions with
an equation of state $\rho = p$ for a stiff fluid are also obtained in several
special cases, assuming the viscosity coefficients to be the power functions of
the density. The results are, in some relevant cases, compared with those of
Belinskii and Khalatnikov (1976) in the asymptotic limits and are seen to agree
with them in that the models start with $\rho = 0$ at the beginning and evolve
with the creation of matter by the gravitational field, finally approaching the
Friedmann universe.
| [
{
"created": "Fri, 12 Mar 2021 15:20:28 GMT",
"version": "v1"
}
] | 2021-03-15 | [
[
"Banerjee",
"A.",
""
],
[
"Duttachoudhury",
"S. B.",
""
],
[
"Sanyal",
"Abhik Kumar",
""
]
] | Bianchi I cosmological models consisting of a fluid with both bulk and shear viscosity are studied. It is shown how the dynamical importance of the shear and the fluid density change in the course of evolution. Exact solutions with an equation of state $\rho = p$ for a stiff fluid are also obtained in several special cases, assuming the viscosity coefficients to be the power functions of the density. The results are, in some relevant cases, compared with those of Belinskii and Khalatnikov (1976) in the asymptotic limits and are seen to agree with them in that the models start with $\rho = 0$ at the beginning and evolve with the creation of matter by the gravitational field, finally approaching the Friedmann universe. |
0710.5366 | Debashis Gangopadhyay | Debashis Gangopadhyay and Somnath Mukherjee | Logarithm of the scale factor as a generalised coordinate in a
lagrangian for dark matter and dark energy | 16 pages, latex, paper shortened by 2 pages for journal publication | Phys.Lett.B665:121-124,2008 | 10.1016/j.physletb.2008.06.025 | null | gr-qc astro-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A lagrangian for the $k-$ essence field is set up with canonical kinetic
terms and incorporating the scaling relation of [1]. There are two degrees of
freedom, {\it viz.},$q(t)= ln\enskip a(t)$ ($a(t)$ is the scale factor) and the
scalar field $\phi$, and an interaction term involving $\phi$ and $q(t)$.The
Euler-Lagrange equations are solved for $q$ and $\phi$. Using these solutions
quantities of cosmological interest are determined. The energy density $\rho$
has a constant component which we identify as dark energy and a component
behaving as $a^{-3}$ which we call dark matter. The pressure $p$ is {\it
negative} for time $t\to \infty$ and the sound velocity $c_{s}^{2}={\partial
p\over\partial\rho} << 1$. When dark energy dominates, the deceleration
parameter $Q\to -1$ while in the matter dominated era $Q\sim {1\over 2}$. The
equation of state parameter $w={p\over \rho}$ is shown to be consistent with
$w={p\over\rho}\sim -1$ for dark energy domination and during the matter
dominated era we have $w\sim 0$. Bounds for the parameters of the theory are
estimated from observational data.
Keywords: k-essence models, dark matter, dark energy
PACS No: 98.80.-k
| [
{
"created": "Mon, 29 Oct 2007 09:51:45 GMT",
"version": "v1"
},
{
"created": "Thu, 14 Aug 2008 05:33:46 GMT",
"version": "v2"
}
] | 2008-11-26 | [
[
"Gangopadhyay",
"Debashis",
""
],
[
"Mukherjee",
"Somnath",
""
]
] | A lagrangian for the $k-$ essence field is set up with canonical kinetic terms and incorporating the scaling relation of [1]. There are two degrees of freedom, {\it viz.},$q(t)= ln\enskip a(t)$ ($a(t)$ is the scale factor) and the scalar field $\phi$, and an interaction term involving $\phi$ and $q(t)$.The Euler-Lagrange equations are solved for $q$ and $\phi$. Using these solutions quantities of cosmological interest are determined. The energy density $\rho$ has a constant component which we identify as dark energy and a component behaving as $a^{-3}$ which we call dark matter. The pressure $p$ is {\it negative} for time $t\to \infty$ and the sound velocity $c_{s}^{2}={\partial p\over\partial\rho} << 1$. When dark energy dominates, the deceleration parameter $Q\to -1$ while in the matter dominated era $Q\sim {1\over 2}$. The equation of state parameter $w={p\over \rho}$ is shown to be consistent with $w={p\over\rho}\sim -1$ for dark energy domination and during the matter dominated era we have $w\sim 0$. Bounds for the parameters of the theory are estimated from observational data. Keywords: k-essence models, dark matter, dark energy PACS No: 98.80.-k |
1705.04359 | Mario Llerena | Andr\'es Ace\~na, Ericson L\'opez, Mario Llerena | An Extreme Rotating Black Hole in New Massive Gravity Theory | null | Revista Polit\'ecnica - Abril 2017, Vol. 39, No. 1 | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | New Massive Gravity is an alternative theory to General Relativity that is
used to describe the gravitational field in a (2+1)-dimensional spacetime.
Black hole solutions have been found in this theory, in particular an
asymptotically anti-de Sitter rotating black hole. We analyse some features of
this solution as its event horizon, black hole area and distance to the
horizon, specially in the rotating extreme case, showing that they have shared
features with extreme black holes in 4-dimensional General relativity. This
limit case is interesting in the search of geometric inequalities as the ones
found for the Kerr black hole in (3+1)-General Relativity.
| [
{
"created": "Thu, 11 May 2017 19:26:30 GMT",
"version": "v1"
}
] | 2017-05-15 | [
[
"Aceña",
"Andrés",
""
],
[
"López",
"Ericson",
""
],
[
"Llerena",
"Mario",
""
]
] | New Massive Gravity is an alternative theory to General Relativity that is used to describe the gravitational field in a (2+1)-dimensional spacetime. Black hole solutions have been found in this theory, in particular an asymptotically anti-de Sitter rotating black hole. We analyse some features of this solution as its event horizon, black hole area and distance to the horizon, specially in the rotating extreme case, showing that they have shared features with extreme black holes in 4-dimensional General relativity. This limit case is interesting in the search of geometric inequalities as the ones found for the Kerr black hole in (3+1)-General Relativity. |
2206.13588 | Octavian Micu | Roberto Casadio, Iber\^e Kuntz, Octavian Micu | Binary mergers in bootstrapped Newtonian gravity: mass gap and black
hole area law | 14 pages, 1 figure, to appear in Phys.Lett.B | null | 10.1016/j.physletb.2022.137455 | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | We study binary mergers in bootstrapped Newtonian gravity, where higher-order
couplings are added to the non-relativistic Lagrangian for the Newtonian
potential. In this theory, the Arnowitt-Deser-Misner (ADM) mass differs from
both the proper mass of Newtonian gravity and the proper mass of general
relativity, which affects the interpretation of astrophysical and cosmological
events. The aforementioned difference particularly provides important
phenomenological constraints for the mass of the emitted matter and the
compactness of the final object after the merger. The interpretation of the
GW150914 signal in this theory also shows that LIGO's findings do not violate
the mass gap, contrary to usual claims. We indeed find that typical stellar
black hole masses can fit LIGO's data for a considerable range of compactness
values. We calculate the black hole entropy in this context, which leads to a
generalised black hole area law. Non-linear effects are found to effectively
change only the gravitational strength via the renormalization of Newton's
constant in this case.
| [
{
"created": "Mon, 27 Jun 2022 19:08:15 GMT",
"version": "v1"
},
{
"created": "Wed, 14 Sep 2022 08:24:41 GMT",
"version": "v2"
}
] | 2022-09-21 | [
[
"Casadio",
"Roberto",
""
],
[
"Kuntz",
"Iberê",
""
],
[
"Micu",
"Octavian",
""
]
] | We study binary mergers in bootstrapped Newtonian gravity, where higher-order couplings are added to the non-relativistic Lagrangian for the Newtonian potential. In this theory, the Arnowitt-Deser-Misner (ADM) mass differs from both the proper mass of Newtonian gravity and the proper mass of general relativity, which affects the interpretation of astrophysical and cosmological events. The aforementioned difference particularly provides important phenomenological constraints for the mass of the emitted matter and the compactness of the final object after the merger. The interpretation of the GW150914 signal in this theory also shows that LIGO's findings do not violate the mass gap, contrary to usual claims. We indeed find that typical stellar black hole masses can fit LIGO's data for a considerable range of compactness values. We calculate the black hole entropy in this context, which leads to a generalised black hole area law. Non-linear effects are found to effectively change only the gravitational strength via the renormalization of Newton's constant in this case. |
gr-qc/9609013 | Ramy Brustein | Bruce Allen, Ram Brustein | Detecting relic gravitational radiation from string cosmology with LIGO | 6 pages, 5 eps figures, Revtex | Phys.Rev.D55:3260-3264,1997 | 10.1103/PhysRevD.55.3260 | WISC-MILW-96-TH-34,BGU-PH-96/09 | gr-qc astro-ph hep-th | null | A characteristic spectrum of relic gravitational radiation is produced by a
period of ``stringy inflation" in the early universe. This spectrum is unusual,
because the energy-density rises rapidly with frequency. We show that
correlation experiments with the two gravitational wave detectors being built
for the Laser Interferometric Gravitational Observatory (LIGO) could detect
this relic radiation, for certain ranges of the parameters that characterize
the underlying string cosmology model.
| [
{
"created": "Thu, 5 Sep 1996 06:03:38 GMT",
"version": "v1"
}
] | 2009-12-30 | [
[
"Allen",
"Bruce",
""
],
[
"Brustein",
"Ram",
""
]
] | A characteristic spectrum of relic gravitational radiation is produced by a period of ``stringy inflation" in the early universe. This spectrum is unusual, because the energy-density rises rapidly with frequency. We show that correlation experiments with the two gravitational wave detectors being built for the Laser Interferometric Gravitational Observatory (LIGO) could detect this relic radiation, for certain ranges of the parameters that characterize the underlying string cosmology model. |
2010.04943 | Shao-Jiang Wang | Rong-Gen Cai, Shao-Jiang Wang, Su Yi, Jiang-Hao Yu | Testing weakest force with coldest spot | v1, 10 pages, 3 figures; v2, references added, discussion extended
for enlarged parameter space of Yukawa interaction, version accepted by EPJC | Eur. Phys. J. C 81, 318 (2021) | 10.1140/epjc/s10052-021-09102-y | null | gr-qc cond-mat.quant-gas | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Ultra-cold atom experiment in space with microgravity allows for realization
of dilute atomic-gas Bose-Einstein condensate (BEC) with macroscopically large
occupation number and significantly long condensate lifetime, which allows for
a precise measurement on the shape oscillation frequency by calibrating itself
over numerous oscillation periods. In this paper, we propose to measure the
Newtonian gravitational constant via ultra-cold atom BEC with shape
oscillation, although it is experimentally challenging. We also make a
preliminary perspective on constraining the modified Newtonian potential such
as the power-law potential, Yukawa interaction, and fat graviton. A resolution
of frequency measurement of $(1-100)\,\mathrm{nHz}$ at most for the occupation
number $10^9$, just one order above experimentally achievable number
$N\sim10^6-10^8$, is feasible to constrain the modified Newtonian potential
with Yukawa interaction greatly beyond the current exclusion limits.
| [
{
"created": "Sat, 10 Oct 2020 08:41:05 GMT",
"version": "v1"
},
{
"created": "Wed, 31 Mar 2021 02:43:50 GMT",
"version": "v2"
}
] | 2021-04-20 | [
[
"Cai",
"Rong-Gen",
""
],
[
"Wang",
"Shao-Jiang",
""
],
[
"Yi",
"Su",
""
],
[
"Yu",
"Jiang-Hao",
""
]
] | Ultra-cold atom experiment in space with microgravity allows for realization of dilute atomic-gas Bose-Einstein condensate (BEC) with macroscopically large occupation number and significantly long condensate lifetime, which allows for a precise measurement on the shape oscillation frequency by calibrating itself over numerous oscillation periods. In this paper, we propose to measure the Newtonian gravitational constant via ultra-cold atom BEC with shape oscillation, although it is experimentally challenging. We also make a preliminary perspective on constraining the modified Newtonian potential such as the power-law potential, Yukawa interaction, and fat graviton. A resolution of frequency measurement of $(1-100)\,\mathrm{nHz}$ at most for the occupation number $10^9$, just one order above experimentally achievable number $N\sim10^6-10^8$, is feasible to constrain the modified Newtonian potential with Yukawa interaction greatly beyond the current exclusion limits. |
2303.00297 | Umananda Dev Goswami | Ronit Karmakar, Dhruba Jyoti Gogoi and Umananda Dev Goswami | Thermodynamics and Shadows of GUP-corrected Black Holes with Topological
Defects in Bumblebee Gravity | 20 pages, 10 figures; Accepted version of Physics of the Dark
Universe | Phys. Dark Universe 41, 101249 (2023) | 10.1016/j.dark.2023.101249 | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | In this work we investigate a Schwarzschild-type black hole that is corrected
by the Generalized Uncertainty Principle (GUP) and possesses topological
defects within the framework of Bumblebee gravity. Our focus is on the
thermodynamic characteristics of the black hole, such as temperature, entropy
and heat capacity, which vary as functions of the horizon radius, and also on
shadow as an optical feature. Our investigation reveals significant changes in
the thermodynamic behavior of the black hole due to violations of Lorentz
symmetry, GUP corrections, and the presence of monopoles. However, the shadow
of the black hole is unaffected by violations of Lorentz symmetry. In addition,
we provide a limit on the parameters of Lorentz symmetry violation, GUP and
topological defects based on a classical test involving the precession of
planetary orbits and the advancement of perihelion in the solar system.
| [
{
"created": "Wed, 1 Mar 2023 07:47:07 GMT",
"version": "v1"
},
{
"created": "Sun, 14 May 2023 11:39:27 GMT",
"version": "v2"
}
] | 2023-05-16 | [
[
"Karmakar",
"Ronit",
""
],
[
"Gogoi",
"Dhruba Jyoti",
""
],
[
"Goswami",
"Umananda Dev",
""
]
] | In this work we investigate a Schwarzschild-type black hole that is corrected by the Generalized Uncertainty Principle (GUP) and possesses topological defects within the framework of Bumblebee gravity. Our focus is on the thermodynamic characteristics of the black hole, such as temperature, entropy and heat capacity, which vary as functions of the horizon radius, and also on shadow as an optical feature. Our investigation reveals significant changes in the thermodynamic behavior of the black hole due to violations of Lorentz symmetry, GUP corrections, and the presence of monopoles. However, the shadow of the black hole is unaffected by violations of Lorentz symmetry. In addition, we provide a limit on the parameters of Lorentz symmetry violation, GUP and topological defects based on a classical test involving the precession of planetary orbits and the advancement of perihelion in the solar system. |
1602.04779 | Shantanu Desai | Emre O. Kahya, Shantanu Desai | Constraints on frequency-dependent violations of Shapiro delay from
GW150914 | 3 pages, accepted for publication in Phys. Lett. B. This paper is
dedicated to the memory of Prof. Steven Detweiler | Phys. Lett. B 756, 265 (2016) | 10.1016/j.physletb.2016.03.033 | null | gr-qc astro-ph.CO astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | On 14th September 2015, a transient gravitational wave (GW150914) was
detected by the two LIGO detectors at Hanford and Livingston from the
coalescence of a binary black hole system located at a distance of about 400
Mpc. We point out that GW150914 experienced a Shapiro delay due to the
gravitational potential of the mass distribution along the line of sight of
about 1800 days. Also, the near-simultaneous arrival of gravitons over a
frequency range of about 100 Hz within a 0.2 second window allows us to
constrain any violations of Shapiro delay and Einstein's equivalence principle
between the gravitons at different frequencies. From the calculated Shapiro
delay and the observed duration of the signal, frequency-dependent violations
of the equivalence principle for gravitons are constrained to an accuracy of
$\mathcal{O}(10^{-9})$
| [
{
"created": "Mon, 15 Feb 2016 19:54:36 GMT",
"version": "v1"
},
{
"created": "Wed, 17 Feb 2016 21:24:59 GMT",
"version": "v2"
},
{
"created": "Wed, 16 Mar 2016 22:37:36 GMT",
"version": "v3"
}
] | 2016-03-25 | [
[
"Kahya",
"Emre O.",
""
],
[
"Desai",
"Shantanu",
""
]
] | On 14th September 2015, a transient gravitational wave (GW150914) was detected by the two LIGO detectors at Hanford and Livingston from the coalescence of a binary black hole system located at a distance of about 400 Mpc. We point out that GW150914 experienced a Shapiro delay due to the gravitational potential of the mass distribution along the line of sight of about 1800 days. Also, the near-simultaneous arrival of gravitons over a frequency range of about 100 Hz within a 0.2 second window allows us to constrain any violations of Shapiro delay and Einstein's equivalence principle between the gravitons at different frequencies. From the calculated Shapiro delay and the observed duration of the signal, frequency-dependent violations of the equivalence principle for gravitons are constrained to an accuracy of $\mathcal{O}(10^{-9})$ |
0801.1204 | Narayan Banerjee | Narayan Banerjee, Sudipta Das, Koyel Ganguly | Chameleon field and the late time acceleration of the universe | 7 pages, 2 figures | Pramana 74:L481-L489,2010 | 10.1007/s12043-010-0044-5 | null | gr-qc astro-ph | null | In the present work, it is shown that a chameleon scalar field having a
nonminimal coupling with dark matter can give rise to a smooth transition from
a decelerated to an accelerated phase of expansion for the universe. It is
surprising to note that the coupling with the chameleon scalar field hardly
affects the evolution of the dark matter sector, which still redshifts as
$a^{-3}$.
| [
{
"created": "Tue, 8 Jan 2008 11:09:56 GMT",
"version": "v1"
}
] | 2015-05-13 | [
[
"Banerjee",
"Narayan",
""
],
[
"Das",
"Sudipta",
""
],
[
"Ganguly",
"Koyel",
""
]
] | In the present work, it is shown that a chameleon scalar field having a nonminimal coupling with dark matter can give rise to a smooth transition from a decelerated to an accelerated phase of expansion for the universe. It is surprising to note that the coupling with the chameleon scalar field hardly affects the evolution of the dark matter sector, which still redshifts as $a^{-3}$. |
gr-qc/0102051 | Carlo Rovelli | Etera R. Livine, Alejandro Perez, Carlo Rovelli | 2d manifold-independent spinfoam theory | 31 pages, five figures; v2: details and one reference added | null | null | null | gr-qc | null | A number of background independent quantizations procedures have recently
been employed in 4d nonperturbative quantum gravity. We investigate and
illustrate these techniques and their relation in the context of a simple 2d
topological theory. We discuss canonical quantization, loop or spin network
states, path integral quantization over a discretization of the manifold, spin
foam formulation, as well as the fully background independent definition of the
theory using an auxiliary field theory on a group manifold. While several of
these techniques have already been applied to this theory by Witten, the last
one is novel: it allows us to give a precise meaning to the sum over
topologies, and to compute background-independent and, in fact,
"manifold-independent" transition amplitudes. These transition amplitudes play
the role of Wightman functions of the theory. They are physical observable
quantities, and the canonical structure of the theory can be reconstructed from
them via a C* algebraic GNS construction. We expect an analogous structure to
be relevant in 4d quantum gravity.
| [
{
"created": "Mon, 12 Feb 2001 19:38:15 GMT",
"version": "v1"
},
{
"created": "Fri, 16 May 2003 09:25:09 GMT",
"version": "v2"
}
] | 2007-05-23 | [
[
"Livine",
"Etera R.",
""
],
[
"Perez",
"Alejandro",
""
],
[
"Rovelli",
"Carlo",
""
]
] | A number of background independent quantizations procedures have recently been employed in 4d nonperturbative quantum gravity. We investigate and illustrate these techniques and their relation in the context of a simple 2d topological theory. We discuss canonical quantization, loop or spin network states, path integral quantization over a discretization of the manifold, spin foam formulation, as well as the fully background independent definition of the theory using an auxiliary field theory on a group manifold. While several of these techniques have already been applied to this theory by Witten, the last one is novel: it allows us to give a precise meaning to the sum over topologies, and to compute background-independent and, in fact, "manifold-independent" transition amplitudes. These transition amplitudes play the role of Wightman functions of the theory. They are physical observable quantities, and the canonical structure of the theory can be reconstructed from them via a C* algebraic GNS construction. We expect an analogous structure to be relevant in 4d quantum gravity. |
1104.4972 | Michael Reiterer | Michael Reiterer (ETH Zurich), Eugene Trubowitz (ETH Zurich) | A class of gauges for the Einstein equations | 12 pages, Subsection 4.4 simplified | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A class of gauges for the Einstein vacuum equations is introduced, along with
three symmetric hyperbolic systems. The first implies the local realizability
of the gauge. The second is the dynamical subset of the field equations. The
third is used to show that the constraints propagate. The gauges are for an
orthonormal frame formalism, with first order, quadratically nonlinear
equations. The unknowns are 16 frame components and 28 connection components.
After gauge-fixing, a total of 33 remain.
| [
{
"created": "Tue, 26 Apr 2011 17:19:10 GMT",
"version": "v1"
},
{
"created": "Sat, 30 Apr 2011 17:08:46 GMT",
"version": "v2"
}
] | 2011-05-03 | [
[
"Reiterer",
"Michael",
"",
"ETH Zurich"
],
[
"Trubowitz",
"Eugene",
"",
"ETH Zurich"
]
] | A class of gauges for the Einstein vacuum equations is introduced, along with three symmetric hyperbolic systems. The first implies the local realizability of the gauge. The second is the dynamical subset of the field equations. The third is used to show that the constraints propagate. The gauges are for an orthonormal frame formalism, with first order, quadratically nonlinear equations. The unknowns are 16 frame components and 28 connection components. After gauge-fixing, a total of 33 remain. |
1609.01477 | Chandra Prakash Singh | C P Singh and Pankaj Kumar | Holographic dark energy in Brans-Dicke theory with logarithmic form of
scalar field | 9 pages, 5 figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, an interacting holographic dark energy model with Hubble
horizon as an infra-red cut-off is considered in the framework of Brans-Dicke
theory. We propose a logarithmic form $\phi \propto ln(\alpha+\beta a)$ of the
Brans-Dicke scalar field to alleviate the problems of interacting holographic
dark energy models in Brans-Dicke theory. We find that the equation of state
parameter $w_h$ and deceleration parameter $q$ are negative in the early time
which shows the early time inflation. During the evolution the sign of
parameter $q$ changes from negative to positive which means that the Universe
expands with decelerated rate whereas the sign of $w_h$ may change or remain
negative throughout the evolution depending on the values of parameters. It is
also observed that $w_h$ may cross the phantom divide line in the late time
evolution. The sign of $q$ changes from positive to negative during late time
of evolution which explains the late time accelerated expansion of the
Universe. Thus, we present a unified model of holographic dark energy which
explains the early time acceleration (inflation), medieval time deceleration
and late time acceleration. We also discuss the cosmic coincidence problem. We
obtain a time-varying density ratio of holographic dark energy to dark matter
which is a constant of order one ($r\sim \mathcal{O}(1)$) during early and late
time evolution. Therefore, our model successfully resolves the cosmic
coincidence problem.
| [
{
"created": "Tue, 6 Sep 2016 10:22:58 GMT",
"version": "v1"
}
] | 2016-09-07 | [
[
"Singh",
"C P",
""
],
[
"Kumar",
"Pankaj",
""
]
] | In this paper, an interacting holographic dark energy model with Hubble horizon as an infra-red cut-off is considered in the framework of Brans-Dicke theory. We propose a logarithmic form $\phi \propto ln(\alpha+\beta a)$ of the Brans-Dicke scalar field to alleviate the problems of interacting holographic dark energy models in Brans-Dicke theory. We find that the equation of state parameter $w_h$ and deceleration parameter $q$ are negative in the early time which shows the early time inflation. During the evolution the sign of parameter $q$ changes from negative to positive which means that the Universe expands with decelerated rate whereas the sign of $w_h$ may change or remain negative throughout the evolution depending on the values of parameters. It is also observed that $w_h$ may cross the phantom divide line in the late time evolution. The sign of $q$ changes from positive to negative during late time of evolution which explains the late time accelerated expansion of the Universe. Thus, we present a unified model of holographic dark energy which explains the early time acceleration (inflation), medieval time deceleration and late time acceleration. We also discuss the cosmic coincidence problem. We obtain a time-varying density ratio of holographic dark energy to dark matter which is a constant of order one ($r\sim \mathcal{O}(1)$) during early and late time evolution. Therefore, our model successfully resolves the cosmic coincidence problem. |
2004.13492 | S. I. Kruglov | S. I. Kruglov | Universe Inflation Based on Nonlinear Electrodynamics | 22 pages, 7 figures. 1 table | Eur. Phys. J. Plus 135, 370 (2020) | 10.1140/epjp/s13360-020-00377-w | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A new model of nonlinear electrodynamics with dimensional parameters $\beta$
and $\gamma$ is proposed. The principles of causality and unitarity are
studied. We show that a singularity of the electric field at the origin of
charges is absent and the maximum of the electric field in the center is
$E(0)=1/\sqrt{\beta}$. The dual symmetry is broken in our model. Corrections to
the Coulomb law as $r\rightarrow\infty$ are in the order of ${\cal O}(r^{-4})$.
The source of the gravitation field and inflation of the universe is
electromagnetic fields. It is supposed that the universe is filled by
stochastic magnetic fields. We demonstrate that after the universe inflation
the universe decelerates approaching the Minkowski spacetime. The singularities
of the Ricci scalar, the Ricci tensor squared and the Kretschmann scalar are
absent. We calculate the speed of sound. The spectral index, the
tensor-to-scalar ratio, and the running of the spectral index, which
approximately agree with the PLANK and WMAP data, are evaluated.
| [
{
"created": "Sun, 26 Apr 2020 22:37:31 GMT",
"version": "v1"
}
] | 2020-04-29 | [
[
"Kruglov",
"S. I.",
""
]
] | A new model of nonlinear electrodynamics with dimensional parameters $\beta$ and $\gamma$ is proposed. The principles of causality and unitarity are studied. We show that a singularity of the electric field at the origin of charges is absent and the maximum of the electric field in the center is $E(0)=1/\sqrt{\beta}$. The dual symmetry is broken in our model. Corrections to the Coulomb law as $r\rightarrow\infty$ are in the order of ${\cal O}(r^{-4})$. The source of the gravitation field and inflation of the universe is electromagnetic fields. It is supposed that the universe is filled by stochastic magnetic fields. We demonstrate that after the universe inflation the universe decelerates approaching the Minkowski spacetime. The singularities of the Ricci scalar, the Ricci tensor squared and the Kretschmann scalar are absent. We calculate the speed of sound. The spectral index, the tensor-to-scalar ratio, and the running of the spectral index, which approximately agree with the PLANK and WMAP data, are evaluated. |
1110.3878 | Shinji Tsujikawa | Antonio De Felice, Shinji Tsujikawa | Conditions for the cosmological viability of the most general
scalar-tensor theories and their applications to extended Galileon dark
energy models | 18 pages, 6 figures | JCAP 1202:007, 2012 | 10.1088/1475-7516/2012/02/007 | null | gr-qc astro-ph.CO hep-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In the Horndeski's most general scalar-tensor theories with second-order
field equations, we derive the conditions for the avoidance of ghosts and
Laplacian instabilities associated with scalar, tensor, and vector
perturbations in the presence of two perfect fluids on the flat
Friedmann-Lemaitre-Robertson-Walker (FLRW) background. Our general results are
useful for the construction of theoretically consistent models of dark energy.
We apply our formulas to extended Galileon models in which a tracker solution
with an equation of state smaller than -1 is present. We clarify the allowed
parameter space in which the ghosts and Laplacian instabilities are absent and
we numerically confirm that such models are indeed cosmologically viable.
| [
{
"created": "Tue, 18 Oct 2011 05:22:45 GMT",
"version": "v1"
}
] | 2015-05-30 | [
[
"De Felice",
"Antonio",
""
],
[
"Tsujikawa",
"Shinji",
""
]
] | In the Horndeski's most general scalar-tensor theories with second-order field equations, we derive the conditions for the avoidance of ghosts and Laplacian instabilities associated with scalar, tensor, and vector perturbations in the presence of two perfect fluids on the flat Friedmann-Lemaitre-Robertson-Walker (FLRW) background. Our general results are useful for the construction of theoretically consistent models of dark energy. We apply our formulas to extended Galileon models in which a tracker solution with an equation of state smaller than -1 is present. We clarify the allowed parameter space in which the ghosts and Laplacian instabilities are absent and we numerically confirm that such models are indeed cosmologically viable. |
2206.08037 | Ulf Lindstr\"om | Ulf Lindstr\"om and \"Ozg\"ur Sar{\i}o\u{g}lu | Geometry, conformal Killing-Yano tensors and conserved "currents" | 15 pages; This version considerably reworked relative to previous
ones, prompted by a number of comments from various researchers | JHEP 05 (2023) 176 | 10.1007/JHEP05(2023)176 | Uppsala Theoretical Physics preprint UUUIP-27/22 | gr-qc hep-th | http://creativecommons.org/licenses/by/4.0/ | In this paper we discuss the construction of conserved tensors (currents)
involving conformal Killing-Yano tensors (CKYTs), generalising the
corresponding constructions for Killing-Yano tensors (KYTs). As a useful
preparation for this, but also of intrinsic interest, we derive identities
relating CKYTs and geometric quantities. The behaviour of CKYTs under conformal
transformations is also given, correcting formulae in the literature. We then
use the identities derived to construct covariantly conserved ``currents''. We
find several new CKYT currents and also include a known one by Penrose which
shows that ``trivial'' currents are also useful. We further find that rank-$n$
currents based on rank-$n$ CKYTs $k$ must have a simple form in terms of $dk$.
By construction, these currents are covariant under a general conformal
rescaling of the metric. How currents lead to conserved charges is then
illustrated using the Kerr-Newman and the C-metric in four dimensions.
Separately, we study a rank-1 current, construct its charge and discuss its
relation to the recently constructed Cotton current for the Kerr-Newman black
hole.
| [
{
"created": "Thu, 16 Jun 2022 09:42:36 GMT",
"version": "v1"
},
{
"created": "Sun, 5 Mar 2023 16:15:20 GMT",
"version": "v2"
}
] | 2023-05-24 | [
[
"Lindström",
"Ulf",
""
],
[
"Sarıoğlu",
"Özgür",
""
]
] | In this paper we discuss the construction of conserved tensors (currents) involving conformal Killing-Yano tensors (CKYTs), generalising the corresponding constructions for Killing-Yano tensors (KYTs). As a useful preparation for this, but also of intrinsic interest, we derive identities relating CKYTs and geometric quantities. The behaviour of CKYTs under conformal transformations is also given, correcting formulae in the literature. We then use the identities derived to construct covariantly conserved ``currents''. We find several new CKYT currents and also include a known one by Penrose which shows that ``trivial'' currents are also useful. We further find that rank-$n$ currents based on rank-$n$ CKYTs $k$ must have a simple form in terms of $dk$. By construction, these currents are covariant under a general conformal rescaling of the metric. How currents lead to conserved charges is then illustrated using the Kerr-Newman and the C-metric in four dimensions. Separately, we study a rank-1 current, construct its charge and discuss its relation to the recently constructed Cotton current for the Kerr-Newman black hole. |
1008.2768 | Stephen D. H. Hsu | Roberto Casadio, Stephen D.H. Hsu, Behrouz Mirza | Asymptotic Safety, Singularities, and Gravitational Collapse | 6 pages, latex. Version to appear in Physics Letters B | Phys.Lett.B695:317-319,2011 | 10.1016/j.physletb.2010.10.060 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Asymptotic safety (an ultraviolet fixed point with finite-dimensional
critical surface) offers the possibility that a predictive theory of quantum
gravity can be obtained from the quantization of classical general relativity.
However, it is unclear what becomes of the singularities of classical general
relativity, which, it is hoped, might be resolved by quantum effects. We study
dust collapse with a running gravitational coupling and find that a future
singularity can be avoided if the coupling becomes exactly zero at some finite
energy scale. The singularity can also be avoided (pushed off to infinite
proper time) if the coupling approaches zero sufficiently rapidly at high
energies. However, the evolution deduced from perturbation theory still implies
a singularity at finite proper time.
| [
{
"created": "Mon, 16 Aug 2010 20:18:47 GMT",
"version": "v1"
},
{
"created": "Wed, 3 Nov 2010 08:35:30 GMT",
"version": "v2"
}
] | 2011-06-27 | [
[
"Casadio",
"Roberto",
""
],
[
"Hsu",
"Stephen D. H.",
""
],
[
"Mirza",
"Behrouz",
""
]
] | Asymptotic safety (an ultraviolet fixed point with finite-dimensional critical surface) offers the possibility that a predictive theory of quantum gravity can be obtained from the quantization of classical general relativity. However, it is unclear what becomes of the singularities of classical general relativity, which, it is hoped, might be resolved by quantum effects. We study dust collapse with a running gravitational coupling and find that a future singularity can be avoided if the coupling becomes exactly zero at some finite energy scale. The singularity can also be avoided (pushed off to infinite proper time) if the coupling approaches zero sufficiently rapidly at high energies. However, the evolution deduced from perturbation theory still implies a singularity at finite proper time. |
2406.01998 | Andronikos Paliathanasis | Andronikos Paliathanasis | The Common Solution Space of General Relativity | 20 pages, no figures | null | null | null | gr-qc hep-th math-ph math.MP | http://creativecommons.org/licenses/by/4.0/ | We review the solution space for the field equations of Einstein's General
Relativity for various static, spherically symmetric spacetimes. We consider
the vacuum case, represented by the Schwarzschild black hole; the de
Sitter-Schwarzschild geometry, which includes a cosmological constant; the
Reissner-Nordstr\"{o}m geometry, which accounts for the presence of charge.
Additionally we consider the homogenenous and anisotropic locally rotational
Bianchi II spacetime in the vacuum. Our analysis reveals that the field
equations for these scenarios share a common three-dimensional group of point
transformations, with the generators being the elements of the
$D\otimes_{s}T_{2}$ Lie algebra, known as the semidirect product of dilations
and translations in the plane. Due to this algebraic property the field
equations for the aforementioned gravitational models can be expressed in the
equivalent form of the null geodesic equations for conformally flat geometries.
Consequently, the solution space for the field equations is common, and it is
the solution space for the free particle in a flat space. This appoach open new
directions on the construction of analytic solutions in gravitational physics
and cosmology.
| [
{
"created": "Tue, 4 Jun 2024 06:28:15 GMT",
"version": "v1"
}
] | 2024-06-05 | [
[
"Paliathanasis",
"Andronikos",
""
]
] | We review the solution space for the field equations of Einstein's General Relativity for various static, spherically symmetric spacetimes. We consider the vacuum case, represented by the Schwarzschild black hole; the de Sitter-Schwarzschild geometry, which includes a cosmological constant; the Reissner-Nordstr\"{o}m geometry, which accounts for the presence of charge. Additionally we consider the homogenenous and anisotropic locally rotational Bianchi II spacetime in the vacuum. Our analysis reveals that the field equations for these scenarios share a common three-dimensional group of point transformations, with the generators being the elements of the $D\otimes_{s}T_{2}$ Lie algebra, known as the semidirect product of dilations and translations in the plane. Due to this algebraic property the field equations for the aforementioned gravitational models can be expressed in the equivalent form of the null geodesic equations for conformally flat geometries. Consequently, the solution space for the field equations is common, and it is the solution space for the free particle in a flat space. This appoach open new directions on the construction of analytic solutions in gravitational physics and cosmology. |
2206.02046 | Valerio Faraoni | Valerio Faraoni, Andrea Giusti, Sonia Jose, Serena Giardino | Peculiar thermal states in the first-order thermodynamics of gravity | 10 pages, latex | null | 10.1103/PhysRevD.106.024049 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In the context of the recently proposed first-order thermodynamics of
scalar-tensor gravity, we discuss the possibility of zero-temperature states of
equilibrium other than Einstein gravity, including pathological Brans-Dicke
theory, Palatini $f(R)$ gravity, and cuscuton gravity, all with non-dynamical
scalar fields. The formalism is extended to Nordstr\"om gravity, which contains
only a scalar degree of freedom and has negative temperature relative to
general relativity.
| [
{
"created": "Sat, 4 Jun 2022 19:20:26 GMT",
"version": "v1"
}
] | 2022-08-17 | [
[
"Faraoni",
"Valerio",
""
],
[
"Giusti",
"Andrea",
""
],
[
"Jose",
"Sonia",
""
],
[
"Giardino",
"Serena",
""
]
] | In the context of the recently proposed first-order thermodynamics of scalar-tensor gravity, we discuss the possibility of zero-temperature states of equilibrium other than Einstein gravity, including pathological Brans-Dicke theory, Palatini $f(R)$ gravity, and cuscuton gravity, all with non-dynamical scalar fields. The formalism is extended to Nordstr\"om gravity, which contains only a scalar degree of freedom and has negative temperature relative to general relativity. |
2310.14411 | Andrei Lebed G | Andrei G. Lebed | Violation of the Einstein's Equivalence Principle for a Composite
Quantum Body | 4 pages | AIP Conf. Proc. 2872, 120048 (2023) | null | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | Recently, we have started to investigate behavior of a composite quantum body
in an external gravitational field in the framework of General Relativity [see,
for a review, A. G. Lebed, Mod. Phys. Lett. A, {\bf 35}, 2030010 (2020)]. As
the simplest example, we have considered a hydrogen atom in a weak
gravitational field. Our results are the following. The Einstein's Equivalence
Principle survives for the most of macroscopic ensembles of the atoms,
containing the stationary quantum states. On the other hand, we have
demonstrated that this principle is sometimes broken. In particular, it is
broken for the so-called Gravitational demons, which are the coherent
macroscopic ensembles of two or more stationary quantum states in the hydrogen
atoms. In the above cited paper we have considered the Gedanken experiment,
where the gravitational field is suddenly switched on in a free from
gravitation space. In the current paper we consider the much more realistic
from experimental point of view Gedanken experiment and come to the same
conclusion about violations of the Einstein's Equivalence Principle for the
Gravitational demons.
| [
{
"created": "Sun, 22 Oct 2023 20:52:20 GMT",
"version": "v1"
}
] | 2023-10-24 | [
[
"Lebed",
"Andrei G.",
""
]
] | Recently, we have started to investigate behavior of a composite quantum body in an external gravitational field in the framework of General Relativity [see, for a review, A. G. Lebed, Mod. Phys. Lett. A, {\bf 35}, 2030010 (2020)]. As the simplest example, we have considered a hydrogen atom in a weak gravitational field. Our results are the following. The Einstein's Equivalence Principle survives for the most of macroscopic ensembles of the atoms, containing the stationary quantum states. On the other hand, we have demonstrated that this principle is sometimes broken. In particular, it is broken for the so-called Gravitational demons, which are the coherent macroscopic ensembles of two or more stationary quantum states in the hydrogen atoms. In the above cited paper we have considered the Gedanken experiment, where the gravitational field is suddenly switched on in a free from gravitation space. In the current paper we consider the much more realistic from experimental point of view Gedanken experiment and come to the same conclusion about violations of the Einstein's Equivalence Principle for the Gravitational demons. |
gr-qc/0608074 | John W. Moffat | J. W. Moffat | A Modified Gravity and its Consequences for the Solar System,
Astrophysics and Cosmology | 16 pages. Latex file. Talk given at the International Workshop "From
Quantum to Cosmos: Fundamental Physics in Space", 22-24 May, 2006, Warrenton,
Virginia, USA. To be published in Int. J. Mod. Phys D. Equation corrected | Int.J.Mod.Phys.D16:2075-2090,2008 | 10.1142/S0218271807011577 | null | gr-qc | null | A relativistic modified gravity (MOG) theory leads to a self-consistent,
stable gravity theory that can describe the solar system, galaxy and clusters
of galaxies data and cosmology.
| [
{
"created": "Tue, 15 Aug 2006 22:41:03 GMT",
"version": "v1"
},
{
"created": "Sun, 17 Dec 2006 21:56:02 GMT",
"version": "v2"
}
] | 2008-11-26 | [
[
"Moffat",
"J. W.",
""
]
] | A relativistic modified gravity (MOG) theory leads to a self-consistent, stable gravity theory that can describe the solar system, galaxy and clusters of galaxies data and cosmology. |
1608.07521 | Arick Shao | Gustav Holzegel, Arick Shao | Unique continuation from infinity in asympotically Anti-de Sitter
spacetimes II: Non-static boundaries | 45 pages. Newest version incorporated changes from referee comments
and fixed minor typos | null | 10.1080/03605302.2017.1390677 | null | gr-qc math.AP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We generalize our unique continuation results recently established for a
class of linear and nonlinear wave equations $\Box_g \phi + \sigma \phi =
\mathcal{G} ( \phi, \partial \phi )$ on asymptotically anti-de Sitter (aAdS)
spacetimes to aAdS spacetimes admitting non-static boundary metrics. The new
Carleman estimates established in this setting constitute an essential
ingredient in proving unique continuation results for the full nonlinear
Einstein equations, which will be addressed in forthcoming papers. Key to the
proof is a new geometrically adapted construction of foliations of pseudoconvex
hypersurfaces near the conformal boundary.
| [
{
"created": "Fri, 26 Aug 2016 16:53:24 GMT",
"version": "v1"
},
{
"created": "Tue, 28 Nov 2017 16:59:08 GMT",
"version": "v2"
}
] | 2017-11-29 | [
[
"Holzegel",
"Gustav",
""
],
[
"Shao",
"Arick",
""
]
] | We generalize our unique continuation results recently established for a class of linear and nonlinear wave equations $\Box_g \phi + \sigma \phi = \mathcal{G} ( \phi, \partial \phi )$ on asymptotically anti-de Sitter (aAdS) spacetimes to aAdS spacetimes admitting non-static boundary metrics. The new Carleman estimates established in this setting constitute an essential ingredient in proving unique continuation results for the full nonlinear Einstein equations, which will be addressed in forthcoming papers. Key to the proof is a new geometrically adapted construction of foliations of pseudoconvex hypersurfaces near the conformal boundary. |
gr-qc/0209112 | Barrabes | C. Barrabes, P.A. Hogan | A Class of Collisions of Plane Impulsive Light--Like Signals in General
Relativity | 14 pages, lateX | Int.J.Mod.Phys. D11 (2002) 933-945 | 10.1142/S0218271802002116 | null | gr-qc | null | We present a systematic study of collisions of homogeneous, plane--fronted,
impulsive light--like signals which do not interact after head--on collision.
For the head--on collision of two such signals, six real parameters are
involved, three from each of the incoming signals. We find two necessary
conditions to be satisfied by these six parameters for the signals to be
non--interacting after collision. We then solve the collision problem in
general when these necessary conditions hold. After collision the two signals
focus each other at Weyl curvature singularities on each others signal front.
Our family of solutions contains some known collision solutions as special
cases.
| [
{
"created": "Mon, 30 Sep 2002 09:45:06 GMT",
"version": "v1"
}
] | 2009-11-07 | [
[
"Barrabes",
"C.",
""
],
[
"Hogan",
"P. A.",
""
]
] | We present a systematic study of collisions of homogeneous, plane--fronted, impulsive light--like signals which do not interact after head--on collision. For the head--on collision of two such signals, six real parameters are involved, three from each of the incoming signals. We find two necessary conditions to be satisfied by these six parameters for the signals to be non--interacting after collision. We then solve the collision problem in general when these necessary conditions hold. After collision the two signals focus each other at Weyl curvature singularities on each others signal front. Our family of solutions contains some known collision solutions as special cases. |
0803.3442 | Alexei Zayats | Alexander B. Balakin, Heinz Dehnen, Alexei E. Zayats | Non-minimal pp-wave Einstein-Yang-Mills-Higgs model: color cross-effects
induced by curvature | 19 pages, accepted to Gen. Rel. Grav | Gen.Rel.Grav.40:2493-2513,2008 | 10.1007/s10714-008-0634-4 | null | gr-qc astro-ph hep-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Non-minimal interactions in the pp-wave Einstein - Yang - Mills - Higgs
(EYMH) model are shown to give rise to color cross-effects analogous to the
magneto-electricity in the Maxwell theory. In order to illustrate the
significance of these color cross-effects, we reconstruct the effective
(associated, color and color-acoustic) metrics for the pp-wave non-minimal
seven-parameter EYMH model with parallel gauge and scalar background fields.
Then these metrics are used as hints for obtaining explicit exact solutions of
the non-minimally extended Yang-Mills and Higgs equations for the test fields
propagating in the vacuum interacting with curvature. The influence of the
non-minimal coupling on the test particle motion is interpreted in terms of the
so-called trapped surfaces, introduced in the Analog Gravity theory.
| [
{
"created": "Mon, 24 Mar 2008 18:14:58 GMT",
"version": "v1"
}
] | 2008-12-18 | [
[
"Balakin",
"Alexander B.",
""
],
[
"Dehnen",
"Heinz",
""
],
[
"Zayats",
"Alexei E.",
""
]
] | Non-minimal interactions in the pp-wave Einstein - Yang - Mills - Higgs (EYMH) model are shown to give rise to color cross-effects analogous to the magneto-electricity in the Maxwell theory. In order to illustrate the significance of these color cross-effects, we reconstruct the effective (associated, color and color-acoustic) metrics for the pp-wave non-minimal seven-parameter EYMH model with parallel gauge and scalar background fields. Then these metrics are used as hints for obtaining explicit exact solutions of the non-minimally extended Yang-Mills and Higgs equations for the test fields propagating in the vacuum interacting with curvature. The influence of the non-minimal coupling on the test particle motion is interpreted in terms of the so-called trapped surfaces, introduced in the Analog Gravity theory. |
gr-qc/0208001 | Anzhong Wang | Paulo R.C.T. Pereira and A.Z. Wang | Collapsing and Expanding Cylindrically Symmetric Fields with Ligh-tlike
Wave-Fronts in General Relativity | 3 figures, prepared in Latex. Inter. J. Mod. Phys. D11, 561-579
(2002) | Int.J.Mod.Phys. D11 (2002) 561-579 | 10.1142/S0218271802001664 | null | gr-qc | null | The dynamics of collapsing and expanding cylindrically symmetric
gravitational and matter fields with lightlike wave-fronts is studied in
General Relativity, using the Barrabes-Israel method. As an application of the
general formulae developed, the collapse of a matter field that satisfies the
condition R_{AB}g^{AB} = 0, (A, B = z, phi), in an otherwise flat spacetime
background is studied. In particular, it is found that the gravitational
collapse of a purely gravitational wave or a null dust fluid cannot be realized
in a flat spacetime background. The studies are further specified to the
collapse of purely gravitational waves and the general conditions for such
collapse are found. It is shown that after the waves arrive at the axis, in
general, part of them is reflected to spacelike infinity along the future light
cone, and part of it is focused to form spacetime singularities on the symmetry
axis. The cases where the collapse does not result in the formation of
spacetime singularities are also identified.
| [
{
"created": "Thu, 1 Aug 2002 19:02:48 GMT",
"version": "v1"
}
] | 2009-11-07 | [
[
"Pereira",
"Paulo R. C. T.",
""
],
[
"Wang",
"A. Z.",
""
]
] | The dynamics of collapsing and expanding cylindrically symmetric gravitational and matter fields with lightlike wave-fronts is studied in General Relativity, using the Barrabes-Israel method. As an application of the general formulae developed, the collapse of a matter field that satisfies the condition R_{AB}g^{AB} = 0, (A, B = z, phi), in an otherwise flat spacetime background is studied. In particular, it is found that the gravitational collapse of a purely gravitational wave or a null dust fluid cannot be realized in a flat spacetime background. The studies are further specified to the collapse of purely gravitational waves and the general conditions for such collapse are found. It is shown that after the waves arrive at the axis, in general, part of them is reflected to spacelike infinity along the future light cone, and part of it is focused to form spacetime singularities on the symmetry axis. The cases where the collapse does not result in the formation of spacetime singularities are also identified. |
1008.0248 | Martin Scholtz | Ji\v{r}\'i Bi\v{c}\'ak and Martin Scholtz and Paul Tod | On asymptotically flat solutions of Einstein's equations periodic in
time II. Spacetimes with scalar-field sources | 29 pages, published in Class. Quant. Grav. Replaced. Typos corrected,
version which appeared in Class. Quant.Grav | Class.Quant.Grav.27:175011,2010 | 10.1088/0264-9381/27/17/175011 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We extend the work in our earlier article [4] to show that time-periodic,
asymptotically-flat solutions of the Einstein equations analytic at scri, whose
source is one of a range of scalar-field models, are necessarily stationary. We
also show that, for some of these scalar-field sources, in stationary,
asymptotically-flat solutions analytic at scri, the scalar field necessarily
inherits the symmetry. To prove these results we investigate miscellaneous
properties of massless and conformal scalar fields coupled to gravity, in
particular Bondi mass and its loss.
| [
{
"created": "Mon, 2 Aug 2010 08:07:20 GMT",
"version": "v1"
},
{
"created": "Fri, 6 Aug 2010 10:08:48 GMT",
"version": "v2"
}
] | 2011-01-18 | [
[
"Bičák",
"Jiří",
""
],
[
"Scholtz",
"Martin",
""
],
[
"Tod",
"Paul",
""
]
] | We extend the work in our earlier article [4] to show that time-periodic, asymptotically-flat solutions of the Einstein equations analytic at scri, whose source is one of a range of scalar-field models, are necessarily stationary. We also show that, for some of these scalar-field sources, in stationary, asymptotically-flat solutions analytic at scri, the scalar field necessarily inherits the symmetry. To prove these results we investigate miscellaneous properties of massless and conformal scalar fields coupled to gravity, in particular Bondi mass and its loss. |
2010.15079 | Javlon Rayimbaev Javlon | Javlon Rayimbaev, Ahmadjon Abdujabbarov, Mubasher Jamil, Bobomurat
Ahmedov, Wen-Biao Han | Dynamics of test particles around renormalization group improved
Schwarzschild black holes | 16 pages, 16 figures. arXiv admin note: text overlap with
arXiv:2010.12863 | Phys. Rev. D 102, 084016 (2020) | 10.1103/PhysRevD.102.084016 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper we have investigated the dynamics of neutral, electrically
charged and magnetized particles around renormalized group improved (RGI)
Schwarzschild black hole in the presence of external asymptotically uniform
magnetic field. We have analyzed the spacetime structure around RGI black hole
by investigating Ricci, the square of Ricci tensor and Kretschmann curvature
scalars and shown that only in the case when the parameter $\gamma=0$ the
curvature becomes infinite at the center of the black hole, while for non-zero
values of $\gamma$ parameter the black hole curvature reflects the properties
of regular black hole. Analyzing the innermost stable circular orbits of test
neutral particles around RGI black hole and comparing with the results for
rotating Kerr black hole we have shown that RGI black hole parameters can mimic
the rotation parameter of Kerr black hole upto $a/M \lesssim 0.31$ providing
the same ISCO radius. Since according to the astronomical observations of the
accretion disks confirm that the astrophysical black holes are rapidly rotating
with the spin parameter upto $a/M \sim 0.99$ one may conclude that the effects
of parameters of RGI Schwarzschild black hole on the circular orbits of the
neutral particles can not mimic the Kerr black hole. Then the Hamilton-Jacobi
equation has been used to analyze the charged and magnetized particles motion
near the RGI black hole in the presence of the strong interaction between
external asymptotically uniform magnetic (electromagnetic) field and magnetized
(electrically charged) particle. We have shown that RGI black hole parameters
quantitatively change the dynamics of the charged and magnetized particles, in
particular ISCO radius of the particles decreases with increasing the parameter
$\lambda$, while the increase of the parameter $\gamma$ causes to increase of
it.
| [
{
"created": "Mon, 26 Oct 2020 08:58:33 GMT",
"version": "v1"
}
] | 2020-11-02 | [
[
"Rayimbaev",
"Javlon",
""
],
[
"Abdujabbarov",
"Ahmadjon",
""
],
[
"Jamil",
"Mubasher",
""
],
[
"Ahmedov",
"Bobomurat",
""
],
[
"Han",
"Wen-Biao",
""
]
] | In this paper we have investigated the dynamics of neutral, electrically charged and magnetized particles around renormalized group improved (RGI) Schwarzschild black hole in the presence of external asymptotically uniform magnetic field. We have analyzed the spacetime structure around RGI black hole by investigating Ricci, the square of Ricci tensor and Kretschmann curvature scalars and shown that only in the case when the parameter $\gamma=0$ the curvature becomes infinite at the center of the black hole, while for non-zero values of $\gamma$ parameter the black hole curvature reflects the properties of regular black hole. Analyzing the innermost stable circular orbits of test neutral particles around RGI black hole and comparing with the results for rotating Kerr black hole we have shown that RGI black hole parameters can mimic the rotation parameter of Kerr black hole upto $a/M \lesssim 0.31$ providing the same ISCO radius. Since according to the astronomical observations of the accretion disks confirm that the astrophysical black holes are rapidly rotating with the spin parameter upto $a/M \sim 0.99$ one may conclude that the effects of parameters of RGI Schwarzschild black hole on the circular orbits of the neutral particles can not mimic the Kerr black hole. Then the Hamilton-Jacobi equation has been used to analyze the charged and magnetized particles motion near the RGI black hole in the presence of the strong interaction between external asymptotically uniform magnetic (electromagnetic) field and magnetized (electrically charged) particle. We have shown that RGI black hole parameters quantitatively change the dynamics of the charged and magnetized particles, in particular ISCO radius of the particles decreases with increasing the parameter $\lambda$, while the increase of the parameter $\gamma$ causes to increase of it. |
2108.08242 | Despoina Pazouli | Despoina Pazouli | High-harmonic cosmic strings and gravitational waves | PhD thesis, School of Physics and Astronomy, Faculty of Science,
University of Nottingham, October 2020 | null | null | null | gr-qc astro-ph.CO hep-th | http://creativecommons.org/licenses/by/4.0/ | In this thesis we describe high-harmonic cosmic string loops in a general
relativistic context, and study the implications of high-harmonic content for
the predicted gravitational wave signal from cosmic string networks. Initially,
we introduce the variational principle, spacetime concepts and other
mathematical tools that we will need for the calculations in the following
chapters. We introduce the FLRW universe and the $\Lambda CDM$ universe. We
then describe the Nambu-Goto cosmic string in a curved spacetime, its equations
of motion and its energy-momentum tensor. Fixing the spacetime to be flat, and
fixing the gauge, we find the motion of the cosmic string and we present and
discuss special solutions. Using the odd-harmonic family of cosmic string
loops, we calculate the number of cusps per period and the values of the second
derivatives of the left- and right-moving harmonic modes at the cusp, and study
their dependence on the harmonic order. We then develop a toy model that
calculates the stable daughter loops produced from a parent loop using a
statistical approach based on a binary tree description of the loop chopping.
We also use the toy model to calculate the average number of cusps produced
from a system of loops that self intersect over their course of existence. We
derive the gravitational waveform emitted from a cusp as observed away from the
cusp, in any direction of observation. We then propagate this result in an FLRW
spacetime to reach an expression of its amplitude on Earth. Assuming two
different cosmic string network models, we implement our above mentioned
high-harmonic results to find the amplitude of the signal and the rate at which
these signals reach an observer on Earth.
| [
{
"created": "Wed, 18 Aug 2021 17:02:36 GMT",
"version": "v1"
}
] | 2021-08-19 | [
[
"Pazouli",
"Despoina",
""
]
] | In this thesis we describe high-harmonic cosmic string loops in a general relativistic context, and study the implications of high-harmonic content for the predicted gravitational wave signal from cosmic string networks. Initially, we introduce the variational principle, spacetime concepts and other mathematical tools that we will need for the calculations in the following chapters. We introduce the FLRW universe and the $\Lambda CDM$ universe. We then describe the Nambu-Goto cosmic string in a curved spacetime, its equations of motion and its energy-momentum tensor. Fixing the spacetime to be flat, and fixing the gauge, we find the motion of the cosmic string and we present and discuss special solutions. Using the odd-harmonic family of cosmic string loops, we calculate the number of cusps per period and the values of the second derivatives of the left- and right-moving harmonic modes at the cusp, and study their dependence on the harmonic order. We then develop a toy model that calculates the stable daughter loops produced from a parent loop using a statistical approach based on a binary tree description of the loop chopping. We also use the toy model to calculate the average number of cusps produced from a system of loops that self intersect over their course of existence. We derive the gravitational waveform emitted from a cusp as observed away from the cusp, in any direction of observation. We then propagate this result in an FLRW spacetime to reach an expression of its amplitude on Earth. Assuming two different cosmic string network models, we implement our above mentioned high-harmonic results to find the amplitude of the signal and the rate at which these signals reach an observer on Earth. |
1012.5619 | Yurii Ignatyev | Yu.G.Ignatyev, K.Alsmadi | The complete relativistic kinetic model of violation of symmetry in
isotopic expanding plasma and production of baryons in hot Universe. I. Exact
model | 12 pages | Grav.Cosmol.11:1-12,2005 | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The complete model of production of baryons in expanding primordial
symmetrical hot Universe is constructed in terms of general relativistic
kinetic theory
| [
{
"created": "Mon, 27 Dec 2010 14:41:21 GMT",
"version": "v1"
}
] | 2011-01-28 | [
[
"Ignatyev",
"Yu. G.",
""
],
[
"Alsmadi",
"K.",
""
]
] | The complete model of production of baryons in expanding primordial symmetrical hot Universe is constructed in terms of general relativistic kinetic theory |
gr-qc/9912023 | Alessandro Fabbri | G. Clement and A. Fabbri | The cosmological gravitating $\sigma$ model: solitons and black holes | 10 pages, latex | Class.Quant.Grav. 17 (2000) 2537-2546 | 10.1088/0264-9381/17/13/307 | null | gr-qc hep-th | null | We derive and analyze exact static solutions to the gravitating O(3) $\sigma$
model with cosmological constant in (2+1) dimensions. Both signs of the
gravitational and cosmological constants are considered. Our solutions include
geodesically complete spacetimes, and two classes of black holes.
| [
{
"created": "Tue, 7 Dec 1999 22:32:53 GMT",
"version": "v1"
},
{
"created": "Wed, 8 Dec 1999 12:06:58 GMT",
"version": "v2"
}
] | 2009-10-31 | [
[
"Clement",
"G.",
""
],
[
"Fabbri",
"A.",
""
]
] | We derive and analyze exact static solutions to the gravitating O(3) $\sigma$ model with cosmological constant in (2+1) dimensions. Both signs of the gravitational and cosmological constants are considered. Our solutions include geodesically complete spacetimes, and two classes of black holes. |
gr-qc/0406116 | Manuel Tiglio | Luis Lehner, David Neilsen, Oscar Reula, and Manuel Tiglio | The discrete energy method in numerical relativity: Towards long-term
stability | 18 pages, 22 figures | Class.Quant.Grav. 21 (2004) 5819-5848 | 10.1088/0264-9381/21/24/009 | LSU-REL-062804 | gr-qc | null | The energy method can be used to identify well-posed initial boundary value
problems for quasi-linear, symmetric hyperbolic partial differential equations
with maximally dissipative boundary conditions. A similar analysis of the
discrete system can be used to construct stable finite difference equations for
these problems at the linear level. In this paper we apply these techniques to
some test problems commonly used in numerical relativity and observe that while
we obtain convergent schemes, fast growing modes, or ``artificial
instabilities,'' contaminate the solution. We find that these growing modes can
partially arise from the lack of a Leibnitz rule for discrete derivatives and
discuss ways to limit this spurious growth.
| [
{
"created": "Tue, 29 Jun 2004 00:02:38 GMT",
"version": "v1"
}
] | 2009-11-10 | [
[
"Lehner",
"Luis",
""
],
[
"Neilsen",
"David",
""
],
[
"Reula",
"Oscar",
""
],
[
"Tiglio",
"Manuel",
""
]
] | The energy method can be used to identify well-posed initial boundary value problems for quasi-linear, symmetric hyperbolic partial differential equations with maximally dissipative boundary conditions. A similar analysis of the discrete system can be used to construct stable finite difference equations for these problems at the linear level. In this paper we apply these techniques to some test problems commonly used in numerical relativity and observe that while we obtain convergent schemes, fast growing modes, or ``artificial instabilities,'' contaminate the solution. We find that these growing modes can partially arise from the lack of a Leibnitz rule for discrete derivatives and discuss ways to limit this spurious growth. |
1809.09554 | Tatyana P. Shestakova | T. P. Shestakova | Is the Copenhagen interpretation inapplicable to Quantum Cosmology? | 23 pages, no figures, the version of the paper that has been
published in the journal Universe | Universe 6 (2020) 128 | 10.3390/universe6090128 | null | gr-qc physics.hist-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | It is generally accepted that the Copenhagen interpretation is inapplicable
to quantum cosmology, by contrast with the many worlds interpretation. I shall
demonstrate that the two basic principles of the Copenhagen interpretation, the
principle of wholeness and the principle of complementarity, do make sense in
quantum gravity, since we can judge about quantum gravitational processes in
the Very Early Universe by their vestiges in our macroscopic Universe. I shall
present the extended phase space approach to quantum gravity and show that it
can be interpreted in the spirit of the Everett's `relative states'
formulation, while there is no contradiction between the `relative states'
formulation and the mentioned basic principles of the Copenhagen
interpretation.
| [
{
"created": "Tue, 25 Sep 2018 15:36:40 GMT",
"version": "v1"
},
{
"created": "Mon, 24 Aug 2020 13:14:51 GMT",
"version": "v2"
}
] | 2020-08-25 | [
[
"Shestakova",
"T. P.",
""
]
] | It is generally accepted that the Copenhagen interpretation is inapplicable to quantum cosmology, by contrast with the many worlds interpretation. I shall demonstrate that the two basic principles of the Copenhagen interpretation, the principle of wholeness and the principle of complementarity, do make sense in quantum gravity, since we can judge about quantum gravitational processes in the Very Early Universe by their vestiges in our macroscopic Universe. I shall present the extended phase space approach to quantum gravity and show that it can be interpreted in the spirit of the Everett's `relative states' formulation, while there is no contradiction between the `relative states' formulation and the mentioned basic principles of the Copenhagen interpretation. |
1504.04173 | Behnam Pourhassan | B. Pourhassan | Unified universe history through phantom extended Chaplygin gas | 25 pages, 16 figures | Canadian Journal of Physics 94 (2016) 659 | 10.1139/cjp-2016-0154 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We investigate the universe evolution from inflation to late-time
acceleration in a unified way, using a two-component fluid constituted from
extended Chaplygin gas alongside a phantom scalar field. We extract solutions
for the various cosmological eras, focusing on the behavior of the scale
factor, the various density parameters and the equation-of-state parameter.
Furthermore, we extract and discuss bouncing solutions. Finally, we examine the
perturbations of the model, ensuring about their stability and extracting the
predictions for the tensor-to-scalar ratio.
| [
{
"created": "Wed, 15 Apr 2015 19:49:58 GMT",
"version": "v1"
}
] | 2016-07-15 | [
[
"Pourhassan",
"B.",
""
]
] | We investigate the universe evolution from inflation to late-time acceleration in a unified way, using a two-component fluid constituted from extended Chaplygin gas alongside a phantom scalar field. We extract solutions for the various cosmological eras, focusing on the behavior of the scale factor, the various density parameters and the equation-of-state parameter. Furthermore, we extract and discuss bouncing solutions. Finally, we examine the perturbations of the model, ensuring about their stability and extracting the predictions for the tensor-to-scalar ratio. |
2105.05050 | Adam Zenon Kaczmarek | Adam Zenon Kaczmarek and Dominik Szcz\k{e}\'sniak | Cosmology in the mimetic higher-curvature $f(R, R_{\mu\nu}R^{\mu\nu})$
gravity | 12 pages, 2 figures | null | 10.1038/s41598-021-97907-y | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | In the framework of the mimetic approach, we study the
$f(R,R_{\mu\nu}R^{\mu\nu})$ gravity with the Lagrange multiplier constraint and
the scalar potential. We introduce field equations for the discussed theory and
overview their properties. By using the general reconstruction scheme we obtain
the power law cosmology model for the
$f(R,R_{\mu\nu}R^{\mu\nu})=R+d(R_{\mu\nu}R^{\mu\nu})^p$ case as well as the
model that describes symmetric bounce. Moreover, we reconstruct model, unifying
both matter dominated and accelerated phases, where ordinary matter is
neglected. Using inverted reconstruction scheme we recover specific
$f(R,R_{\mu\nu}R^{\mu\nu})$ function which give rise to the de-Sitter
evolution. Finally, by employing the perfect fluid approach, we demonstrate
that this model can realize inflation consistent with the bounds coming from
the BICEP2/Keck array and the Planck data. Thus, it is suggested that the
introduced extension of the mimetic regime may describe any given cosmological
model.
| [
{
"created": "Sun, 9 May 2021 10:29:42 GMT",
"version": "v1"
}
] | 2021-11-18 | [
[
"Kaczmarek",
"Adam Zenon",
""
],
[
"Szczęśniak",
"Dominik",
""
]
] | In the framework of the mimetic approach, we study the $f(R,R_{\mu\nu}R^{\mu\nu})$ gravity with the Lagrange multiplier constraint and the scalar potential. We introduce field equations for the discussed theory and overview their properties. By using the general reconstruction scheme we obtain the power law cosmology model for the $f(R,R_{\mu\nu}R^{\mu\nu})=R+d(R_{\mu\nu}R^{\mu\nu})^p$ case as well as the model that describes symmetric bounce. Moreover, we reconstruct model, unifying both matter dominated and accelerated phases, where ordinary matter is neglected. Using inverted reconstruction scheme we recover specific $f(R,R_{\mu\nu}R^{\mu\nu})$ function which give rise to the de-Sitter evolution. Finally, by employing the perfect fluid approach, we demonstrate that this model can realize inflation consistent with the bounds coming from the BICEP2/Keck array and the Planck data. Thus, it is suggested that the introduced extension of the mimetic regime may describe any given cosmological model. |
gr-qc/0412131 | Plamen Fiziev | Plamen Fiziev | The Gravitational Field of Massive Non-Charged Point Source in General
Relativity | 12 pages, latex file, no figures | in Proceedings of the Conference Contemporary Aspects of
Astronomy, Theoretical and Gravitational Physics, May 20-22, 2004, Sofia,
Bulgaria | null | SU-TH-22-04 | gr-qc | null | Utilizing various gauges of the radial coordinate we give a description of
static spherically symmetric space-times with point singularity at the center
and vacuum outside the singularity. We show that in general relativity (GR)
there exist a two-parameters family of such solutions to the Einstein equations
which are physically distinguishable but only some of them describe the
gravitational field of a single massive point particle with nonzero bare mass
$M_0$. In particular, the widespread Hilbert's form of Schwarzschild solution,
which depends only on the Keplerian mass $M<M_0$, does not solve the Einstein
equations with a massive point particle's stress-energy tensor as a source.
Novel normal coordinates for the field and a new physical class of gauges are
proposed, in this way achieving a correct description of a point mass source in
GR. We also introduce a gravitational mass defect of a point particle and
determine the dependence of the solutions on this mass defect. The result can
be described as a change of the Newton potential $\phi_{{}_N}=-G_{{}_N}M/r$ to
a modified one: $\phi_{{}_G}=-G_{{}_N}M/ (r+G_{{}_N} M/c^2\ln{{M_0}\over M})$
and a corresponding modification of the four-interval. In addition we give
invariant characteristics of the physically and geometrically different classes
of spherically symmetric static space-times created by one point mass. These
space-times are analytic manifolds with a definite singularity at the place of
the matter particle.
| [
{
"created": "Thu, 30 Dec 2004 12:22:45 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Fiziev",
"Plamen",
""
]
] | Utilizing various gauges of the radial coordinate we give a description of static spherically symmetric space-times with point singularity at the center and vacuum outside the singularity. We show that in general relativity (GR) there exist a two-parameters family of such solutions to the Einstein equations which are physically distinguishable but only some of them describe the gravitational field of a single massive point particle with nonzero bare mass $M_0$. In particular, the widespread Hilbert's form of Schwarzschild solution, which depends only on the Keplerian mass $M<M_0$, does not solve the Einstein equations with a massive point particle's stress-energy tensor as a source. Novel normal coordinates for the field and a new physical class of gauges are proposed, in this way achieving a correct description of a point mass source in GR. We also introduce a gravitational mass defect of a point particle and determine the dependence of the solutions on this mass defect. The result can be described as a change of the Newton potential $\phi_{{}_N}=-G_{{}_N}M/r$ to a modified one: $\phi_{{}_G}=-G_{{}_N}M/ (r+G_{{}_N} M/c^2\ln{{M_0}\over M})$ and a corresponding modification of the four-interval. In addition we give invariant characteristics of the physically and geometrically different classes of spherically symmetric static space-times created by one point mass. These space-times are analytic manifolds with a definite singularity at the place of the matter particle. |
2207.04720 | Alejandro Garc\'ia-Quismondo | Alejandro Garc\'ia-Quismondo and Guillermo A. Mena Marug\'an | Two-time alternative to the Ashtekar-Olmedo-Singh black hole interior | 21 pages and 5 figures | Phys. Rev. D 106, 023532 (2022) | 10.1103/PhysRevD.106.023532 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We investigate the viability of a recently proposed generalization of the
Ashtekar-Olmedo-Singh spacetime for the effective description of the interior
region of a Schwarzschild black hole within the framework of loop quantum
cosmology. The approach is based on a choice of polymerization parameters that
is more general than the ones previously considered in the literature and that
results in the natural appearance of two times to describe the solutions. If
one is interested in examining the physics derived from this model, it is
fundamental to ensure that one can attain a well-defined effective geometry in
the whole region under consideration, in particular as regards the redundancy
of the two times, which one needs to express in terms of a single time
coordinate. In order to determine whether this requirement is met, we analyze
the definition of these times and their relation. We show that one can reach an
acceptable interior spacetime geometry by exploiting the freedom to define the
origins of the two times independently.
| [
{
"created": "Mon, 11 Jul 2022 08:59:50 GMT",
"version": "v1"
}
] | 2022-09-07 | [
[
"García-Quismondo",
"Alejandro",
""
],
[
"Marugán",
"Guillermo A. Mena",
""
]
] | We investigate the viability of a recently proposed generalization of the Ashtekar-Olmedo-Singh spacetime for the effective description of the interior region of a Schwarzschild black hole within the framework of loop quantum cosmology. The approach is based on a choice of polymerization parameters that is more general than the ones previously considered in the literature and that results in the natural appearance of two times to describe the solutions. If one is interested in examining the physics derived from this model, it is fundamental to ensure that one can attain a well-defined effective geometry in the whole region under consideration, in particular as regards the redundancy of the two times, which one needs to express in terms of a single time coordinate. In order to determine whether this requirement is met, we analyze the definition of these times and their relation. We show that one can reach an acceptable interior spacetime geometry by exploiting the freedom to define the origins of the two times independently. |
1501.01641 | Olivier Sarbach | Eliana Chaverra and Olivier Sarbach | Radial accretion flows on static spherically symmetric black holes | 25 pages, 5 figures. Typos corrected, additional references, new
figure showing accretion flow in deformed Schwarzschild black hole. To appear
in Classical and Quantum Gravity | null | 10.1088/0264-9381/32/15/155006 | null | gr-qc astro-ph.SR | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We analyze the steady radial accretion of matter into a nonrotating black
hole. Neglecting the self-gravity of the accreting matter, we consider a rather
general class of static, spherically symmetric and asymptotically flat
background spacetimes with a regular horizon. In addition to the Schwarzschild
metric, this class contains certain deformation of it which could arise in
alternative gravity theories or from solutions of the classical Einstein
equations in the presence of external matter fields. Modeling the ambient
matter surrounding the black hole by a relativistic perfect fluid, we
reformulate the accretion problem as a dynamical system, and under rather
general assumptions on the fluid equation of state, we determine the local and
global qualitative behavior of its phase flow. Based on our analysis and
generalizing previous work by Michel, we prove that for any given positive
particle density number at infinity, there exists a unique radial, steady-state
accretion flow which is regular at the horizon. We determine the physical
parameters of the flow, including its accretion and compression rates, and
discuss their dependency on the background metric.
| [
{
"created": "Wed, 7 Jan 2015 21:00:33 GMT",
"version": "v1"
},
{
"created": "Tue, 9 Jun 2015 17:45:07 GMT",
"version": "v2"
}
] | 2015-08-06 | [
[
"Chaverra",
"Eliana",
""
],
[
"Sarbach",
"Olivier",
""
]
] | We analyze the steady radial accretion of matter into a nonrotating black hole. Neglecting the self-gravity of the accreting matter, we consider a rather general class of static, spherically symmetric and asymptotically flat background spacetimes with a regular horizon. In addition to the Schwarzschild metric, this class contains certain deformation of it which could arise in alternative gravity theories or from solutions of the classical Einstein equations in the presence of external matter fields. Modeling the ambient matter surrounding the black hole by a relativistic perfect fluid, we reformulate the accretion problem as a dynamical system, and under rather general assumptions on the fluid equation of state, we determine the local and global qualitative behavior of its phase flow. Based on our analysis and generalizing previous work by Michel, we prove that for any given positive particle density number at infinity, there exists a unique radial, steady-state accretion flow which is regular at the horizon. We determine the physical parameters of the flow, including its accretion and compression rates, and discuss their dependency on the background metric. |
2304.10623 | Adnan Malik | Zoya Asghar, M. Farasat Shamir, Ammara Usman, Adnan Malik | Study of Embedded Class-I Fluid Spheres in $f(R,T)$ Gravity with
Karmarkar Condition | 12 pages, 10 figures, Accepted for publication in Chinese Journal of
Physics | null | 10.1016/j.cjph.2023.04.009 | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | In this article, we explore some emerging properties of the stellar objects
in the frame of the $f(R,T)$ gravity by employing the well-known Karmarkar
condition, where $R$ and $T$ represent Ricci scalar and trace of energy
momentum tensor respectively. It is worthy to highlight here that we assume the
exponential type model of $f(R,T)$ theory of gravity $f(R,T)=R+\alpha(e^{-\beta
R}-1)+\gamma T$ along with the matter Lagrangian
$\mathcal{L}_{m}=-\frac{1}{3}(p_{r}+2 p_{t})$ to classify the complete set of
modified field equations. We demonstrate the embedded class-I technique by
using the static spherically symmetric line element along with anisotropic
fluid matter distribution. Further, to achieve our goal, we consider a specific
expression of metric potential $g_{rr}$, already presented in literature, and
proceed by using the Karmarkar condition to obtain the second metric potential.
In particular, we use four different compact stars, namely $LMC~X-4,$
$EXO~1785-248,$ $Cen~X-3$ and $4U~1820-30$ and compute the corresponding values
of the unknown parameters appearing in metric potentials. Moreover, we conduct
various physical evolutions such as graphical nature of energy density and
pressure progression, energy constraints, mass function, adiabatic index,
stability and equilibrium conditions to ensure the viability and consistency of
our proposed model. Our analysis indicates that the obtained anisotropic
outcomes are physically acceptable with the finest degree of accuracy.
| [
{
"created": "Wed, 19 Apr 2023 14:09:47 GMT",
"version": "v1"
}
] | 2023-05-24 | [
[
"Asghar",
"Zoya",
""
],
[
"Shamir",
"M. Farasat",
""
],
[
"Usman",
"Ammara",
""
],
[
"Malik",
"Adnan",
""
]
] | In this article, we explore some emerging properties of the stellar objects in the frame of the $f(R,T)$ gravity by employing the well-known Karmarkar condition, where $R$ and $T$ represent Ricci scalar and trace of energy momentum tensor respectively. It is worthy to highlight here that we assume the exponential type model of $f(R,T)$ theory of gravity $f(R,T)=R+\alpha(e^{-\beta R}-1)+\gamma T$ along with the matter Lagrangian $\mathcal{L}_{m}=-\frac{1}{3}(p_{r}+2 p_{t})$ to classify the complete set of modified field equations. We demonstrate the embedded class-I technique by using the static spherically symmetric line element along with anisotropic fluid matter distribution. Further, to achieve our goal, we consider a specific expression of metric potential $g_{rr}$, already presented in literature, and proceed by using the Karmarkar condition to obtain the second metric potential. In particular, we use four different compact stars, namely $LMC~X-4,$ $EXO~1785-248,$ $Cen~X-3$ and $4U~1820-30$ and compute the corresponding values of the unknown parameters appearing in metric potentials. Moreover, we conduct various physical evolutions such as graphical nature of energy density and pressure progression, energy constraints, mass function, adiabatic index, stability and equilibrium conditions to ensure the viability and consistency of our proposed model. Our analysis indicates that the obtained anisotropic outcomes are physically acceptable with the finest degree of accuracy. |
gr-qc/9911112 | Abel Camacho Quintana | Abel Camacho Quintana (Astrophysikalisches Institut Potsdam) | Flavor-oscillation clocks, continuous quantum measurements and a
violation of Einstein equivalence principle | 16 pages, accepted in Mod. Phys. Letts.A | Mod.Phys.Lett. A14 (1999) 2545-2556 | 10.1142/S0217732399002662 | null | gr-qc quant-ph | null | The relation between Einstein equivalence principle and a continuous quantum
measurement is analyzed in the context of the recently proposed
flavor-oscillation clocks, an idea pioneered by Ahluwalia and Burgard (Gen. Rel
Grav. Errata 29, 681 (1997)). We will calculate the measurement outputs if a
flavor-oscillation clock, which is immersed in a gravitational field, is
subject to a continuous quantum measurement. Afterwards, resorting to the weak
equivalence principle, we obtain the corresponding quantities in a freely
falling reference frame. Finally, comparing this last result with the
measurement outputs that would appear in a Minkowskian spacetime it will be
found that they do not coincide, in other words, we have a violation of
Einstein equivalence principle. This violation appears in two different forms,
namely: (i) the oscillation frequency in a freely falling reference frame does
not match with the case predicted by general relativity, a feature previously
obtained by Ahluwalia; (ii) the probability distribution of the measurement
outputs, obtained by an observer in a freely falling reference frame, does not
coincide with the results that would appear in the case of a Minkowskian
spacetime.
| [
{
"created": "Sun, 28 Nov 1999 15:31:27 GMT",
"version": "v1"
}
] | 2009-10-31 | [
[
"Quintana",
"Abel Camacho",
"",
"Astrophysikalisches Institut Potsdam"
]
] | The relation between Einstein equivalence principle and a continuous quantum measurement is analyzed in the context of the recently proposed flavor-oscillation clocks, an idea pioneered by Ahluwalia and Burgard (Gen. Rel Grav. Errata 29, 681 (1997)). We will calculate the measurement outputs if a flavor-oscillation clock, which is immersed in a gravitational field, is subject to a continuous quantum measurement. Afterwards, resorting to the weak equivalence principle, we obtain the corresponding quantities in a freely falling reference frame. Finally, comparing this last result with the measurement outputs that would appear in a Minkowskian spacetime it will be found that they do not coincide, in other words, we have a violation of Einstein equivalence principle. This violation appears in two different forms, namely: (i) the oscillation frequency in a freely falling reference frame does not match with the case predicted by general relativity, a feature previously obtained by Ahluwalia; (ii) the probability distribution of the measurement outputs, obtained by an observer in a freely falling reference frame, does not coincide with the results that would appear in the case of a Minkowskian spacetime. |
1911.09892 | Patrick Peter | Przemyslaw Malkiewicz, Patrick Peter, S. D. P. Vitenti | Quantum empty Bianchi I spacetime with internal time | 16 pages, 13 figures, matches version to appear in Phys. Rev. D | Phys. Rev. D 101, 046012 (2020) | 10.1103/PhysRevD.101.046012 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We discuss the question of time in a Bianchi I quantum cosmology in the
framework of singularity avoidance. We show that time parameters fall into two
distinct classes, that are such that the time development of the wave function
either always leads to the appearance of a singularity (fast-gauge time) or
that always prevents it from occurring (slow-gauge time). Furthermore, we find
that, in the latter case, there exists an asymptotic regime, independent of the
clock choice. This may point to a possible solution of the clock issue in
quantum cosmology if there exists a suitable class of clocks all yielding
identical relevant physical consequences.
| [
{
"created": "Fri, 22 Nov 2019 07:12:28 GMT",
"version": "v1"
},
{
"created": "Mon, 20 Jan 2020 09:57:52 GMT",
"version": "v2"
},
{
"created": "Fri, 7 Feb 2020 14:02:19 GMT",
"version": "v3"
}
] | 2020-02-18 | [
[
"Malkiewicz",
"Przemyslaw",
""
],
[
"Peter",
"Patrick",
""
],
[
"Vitenti",
"S. D. P.",
""
]
] | We discuss the question of time in a Bianchi I quantum cosmology in the framework of singularity avoidance. We show that time parameters fall into two distinct classes, that are such that the time development of the wave function either always leads to the appearance of a singularity (fast-gauge time) or that always prevents it from occurring (slow-gauge time). Furthermore, we find that, in the latter case, there exists an asymptotic regime, independent of the clock choice. This may point to a possible solution of the clock issue in quantum cosmology if there exists a suitable class of clocks all yielding identical relevant physical consequences. |
gr-qc/0306125 | Daniel A. Shaddock | Daniel A. Shaddock | Operating LISA as a Sagnac interferometer | 8 pages, 2 figures | Phys.Rev. D69 (2004) 022001 | 10.1103/PhysRevD.69.022001 | null | gr-qc | null | A phase-locking configuration for LISA is proposed that provides a
significantly simpler mode of operation. The scheme provides one Sagnac signal
readout inherently insensitive to laser frequency noise and optical bench
motion for a non-rotating LISA array. This Sagnac output is also insensitive to
clock noise, requires no time shifting of data, nor absolute arm length
knowledge. As all measurements are made at one spacecraft, neither clock
synchronization nor exchange of phase information between spacecraft is
required. The phase-locking configuration provides these advantages for only
one Sagnac variable yet retains compatibility with the baseline approach for
obtaining the other TDI variables. The orbital motion of the LISA constellation
is shown to produce a 14 km path length difference between the
counter-propagating beams in the Sagnac interferometer. With this length
difference a laser frequency noise spectral density of 1 Hz/$\sqrt{\rm Hz}$
would consume the entire optical path noise budget of the Sagnac variables. A
significant improvement of laser frequency stability (currently at 30
Hz/$\sqrt{\rm Hz}$) would be needed for full-sensitivity LISA operation in the
Sagnac mode. Alternatively, an additional level of time-delay processing could
be applied to remove the laser frequency noise. The new time-delayed
combinations of the phase measurements are presented.
| [
{
"created": "Sun, 29 Jun 2003 18:28:42 GMT",
"version": "v1"
}
] | 2009-11-10 | [
[
"Shaddock",
"Daniel A.",
""
]
] | A phase-locking configuration for LISA is proposed that provides a significantly simpler mode of operation. The scheme provides one Sagnac signal readout inherently insensitive to laser frequency noise and optical bench motion for a non-rotating LISA array. This Sagnac output is also insensitive to clock noise, requires no time shifting of data, nor absolute arm length knowledge. As all measurements are made at one spacecraft, neither clock synchronization nor exchange of phase information between spacecraft is required. The phase-locking configuration provides these advantages for only one Sagnac variable yet retains compatibility with the baseline approach for obtaining the other TDI variables. The orbital motion of the LISA constellation is shown to produce a 14 km path length difference between the counter-propagating beams in the Sagnac interferometer. With this length difference a laser frequency noise spectral density of 1 Hz/$\sqrt{\rm Hz}$ would consume the entire optical path noise budget of the Sagnac variables. A significant improvement of laser frequency stability (currently at 30 Hz/$\sqrt{\rm Hz}$) would be needed for full-sensitivity LISA operation in the Sagnac mode. Alternatively, an additional level of time-delay processing could be applied to remove the laser frequency noise. The new time-delayed combinations of the phase measurements are presented. |
1711.07259 | Mariana Penna-Lima Vitenti | M.E.S. Alves, F.C. Carvalho, J.C.N. de Araujo, M. Penna-Lima, S.D.P.
Vitenti | Cosmological constant constraints from observation-derived energy
condition bounds and their application to bimetric massive gravity | 11 pages, 4 figures, 1 table | Eur. Phys. J. C (2018) 78: 710 | 10.1140/epjc/s10052-018-6190-5 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Among the various possibilities to probe the theory behind the recent
accelerated expansion of the universe, the energy conditions (ECs) are of
particular interest, since it is possible to confront and constrain the many
models, including different theories of gravity, with observational data. In
this context, we use the ECs to probe any alternative theory whose extra term
acts as a cosmological constant. For this purpose, we apply a model-independent
approach to reconstruct the recent expansion of the universe. Using Type Ia
supernova, baryon acoustic oscillations and cosmic-chronometer data, we perform
a Markov Chain Monte Carlo analysis to put constraints on the effective
cosmological constant $\Omega^0_{\rm eff}$. By imposing that the cosmological
constant is the only component that possibly violates the ECs, we derive lower
and upper bounds for its value. For instance, we obtain that $0.59 <
\Omega^0_{\rm eff} < 0.91$ and $0.40 < \Omega^0_{\rm eff} < 0.93$ within,
respectively, $1\sigma$ and $3\sigma$ confidence levels. In addition, about
30\% of the posterior distribution is incompatible with a cosmological
constant, showing that this method can potentially rule it out as a mechanism
for the accelerated expansion. We also study the consequence of these
constraints for two particular formulations of the bimetric massive gravity.
Namely, we consider the Visser's theory and the Hassan and Roses's massive
gravity by choosing a background metric such that both theories mimic General
Relativity with a cosmological constant. Using the $\Omega^0_{\rm eff}$
observational bounds along with the upper bounds on the graviton mass we obtain
constraints on the parameter spaces of both theories.
| [
{
"created": "Mon, 20 Nov 2017 11:30:24 GMT",
"version": "v1"
}
] | 2018-09-17 | [
[
"Alves",
"M. E. S.",
""
],
[
"Carvalho",
"F. C.",
""
],
[
"de Araujo",
"J. C. N.",
""
],
[
"Penna-Lima",
"M.",
""
],
[
"Vitenti",
"S. D. P.",
""
]
] | Among the various possibilities to probe the theory behind the recent accelerated expansion of the universe, the energy conditions (ECs) are of particular interest, since it is possible to confront and constrain the many models, including different theories of gravity, with observational data. In this context, we use the ECs to probe any alternative theory whose extra term acts as a cosmological constant. For this purpose, we apply a model-independent approach to reconstruct the recent expansion of the universe. Using Type Ia supernova, baryon acoustic oscillations and cosmic-chronometer data, we perform a Markov Chain Monte Carlo analysis to put constraints on the effective cosmological constant $\Omega^0_{\rm eff}$. By imposing that the cosmological constant is the only component that possibly violates the ECs, we derive lower and upper bounds for its value. For instance, we obtain that $0.59 < \Omega^0_{\rm eff} < 0.91$ and $0.40 < \Omega^0_{\rm eff} < 0.93$ within, respectively, $1\sigma$ and $3\sigma$ confidence levels. In addition, about 30\% of the posterior distribution is incompatible with a cosmological constant, showing that this method can potentially rule it out as a mechanism for the accelerated expansion. We also study the consequence of these constraints for two particular formulations of the bimetric massive gravity. Namely, we consider the Visser's theory and the Hassan and Roses's massive gravity by choosing a background metric such that both theories mimic General Relativity with a cosmological constant. Using the $\Omega^0_{\rm eff}$ observational bounds along with the upper bounds on the graviton mass we obtain constraints on the parameter spaces of both theories. |
2105.01716 | Muhammed Saleem C | M. Saleem, Javed Rana, V. Gayathri, Aditya Vijaykumar, Srashti Goyal,
Surabhi Sachdev, Jishnu Suresh, S. Sudhagar, Arunava Mukherjee, Gurudatt
Gaur, Bangalore Sathyaprakash, Archana Pai, Rana X Adhikari, P. Ajith,
Sukanta Bose | The Science Case for LIGO-India | 29 pages, 8 figures | Class. Quantum Grav. 39 025004 (2022) | 10.1088/1361-6382/ac3b99 | null | gr-qc astro-ph.HE | http://creativecommons.org/publicdomain/zero/1.0/ | The global network of gravitational-wave detectors has completed three
observing runs with $\sim 50$ detections of merging compact binaries. A third
LIGO detector, with comparable astrophysical reach, is to be built in India
(LIGO-Aundha) and expected to be operational during the latter part of this
decade. Multiple detectors operating at different parts of the globe will
provide several pairs of interferometers with longer baselines and an increased
network SNR. This will improve the sky localisation of GW events. Multiple
detectors simultaneously in operation will also increase the baseline duty
factor, thereby, leading to an improvement in the detection rates and, hence,
the completeness of surveys. In this paper, we quantify the improvements due to
the expansion of the LIGO Global Network (LGN) in the precision with which
source properties will be measured. We also present examples of how this
expansion will give a boost to tests of fundamental physics.
| [
{
"created": "Tue, 4 May 2021 19:15:26 GMT",
"version": "v1"
},
{
"created": "Fri, 31 Dec 2021 19:28:34 GMT",
"version": "v2"
}
] | 2022-01-04 | [
[
"Saleem",
"M.",
""
],
[
"Rana",
"Javed",
""
],
[
"Gayathri",
"V.",
""
],
[
"Vijaykumar",
"Aditya",
""
],
[
"Goyal",
"Srashti",
""
],
[
"Sachdev",
"Surabhi",
""
],
[
"Suresh",
"Jishnu",
""
],
[
"Sudhagar",
"S.",
""
],
[
"Mukherjee",
"Arunava",
""
],
[
"Gaur",
"Gurudatt",
""
],
[
"Sathyaprakash",
"Bangalore",
""
],
[
"Pai",
"Archana",
""
],
[
"Adhikari",
"Rana X",
""
],
[
"Ajith",
"P.",
""
],
[
"Bose",
"Sukanta",
""
]
] | The global network of gravitational-wave detectors has completed three observing runs with $\sim 50$ detections of merging compact binaries. A third LIGO detector, with comparable astrophysical reach, is to be built in India (LIGO-Aundha) and expected to be operational during the latter part of this decade. Multiple detectors operating at different parts of the globe will provide several pairs of interferometers with longer baselines and an increased network SNR. This will improve the sky localisation of GW events. Multiple detectors simultaneously in operation will also increase the baseline duty factor, thereby, leading to an improvement in the detection rates and, hence, the completeness of surveys. In this paper, we quantify the improvements due to the expansion of the LIGO Global Network (LGN) in the precision with which source properties will be measured. We also present examples of how this expansion will give a boost to tests of fundamental physics. |
0802.1972 | Ion I. Cot{\ba}escu | Ion I. Cotaescu, Cosmin Crucean, Adrian Pop | The quantum theory of scalar fields on the de Sitter expanding universe | 16 pages, no figures | Int.J.Mod.Phys.A23:2563-2577,2008 | 10.1142/S0217751X08040494 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | New quantum modes of the free scalar field are derived in a special
time-evolution picture that may be introduced in moving charts of de Sitter
backgrounds. The wave functions of these new modes are solutions of the
Klein-Gordon equation and energy eigenfunctions, defining the energy basis.
This completes the scalar quantum mechanics where the momentum basis is
well-known from long time. In this enlarged framework the quantization of the
scalar field can be done in canonical way obtaining the principal conserved
one-particle operators and the Green functions.
| [
{
"created": "Thu, 14 Feb 2008 08:11:20 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Cotaescu",
"Ion I.",
""
],
[
"Crucean",
"Cosmin",
""
],
[
"Pop",
"Adrian",
""
]
] | New quantum modes of the free scalar field are derived in a special time-evolution picture that may be introduced in moving charts of de Sitter backgrounds. The wave functions of these new modes are solutions of the Klein-Gordon equation and energy eigenfunctions, defining the energy basis. This completes the scalar quantum mechanics where the momentum basis is well-known from long time. In this enlarged framework the quantization of the scalar field can be done in canonical way obtaining the principal conserved one-particle operators and the Green functions. |
2405.03431 | David Fajman | David Fajman, Maciej Maliborski, Maximilian Ofner, Todd Oliynyk, Zoe
Wyatt | Phase transition between shock formation and stability in cosmological
fluids | 6 pages, 3 figures | null | null | null | gr-qc math-ph math.MP | http://creativecommons.org/licenses/by/4.0/ | We demonstrate a novel phase transition from stable to unstable fluid
behaviour for fluid-filled cosmological spacetimes undergoing decelerated
expansion. This transition occurs when the fluid speed of sound $c_S$ exceeds a
critical value relative to the expansion rate $a(t) = t^\alpha$ of spacetime.
We present an explicit relationship between $\alpha$ and $c_S$ , which
subdivides the $(\alpha,c_S)$-parameter space into two regions. Using rigorous
techniques, we establish stability of quiet fluid solutions in the first stable
region. Numerical experiments reveal that the complement of the stable region
consists of unstable solutions, implying sharpness of our stability result. We
provide a definitive analytical bound and high-precision numerical evidence for
the exact location of the critical line separating the stable from the unstable
region.
| [
{
"created": "Mon, 6 May 2024 12:53:02 GMT",
"version": "v1"
}
] | 2024-05-07 | [
[
"Fajman",
"David",
""
],
[
"Maliborski",
"Maciej",
""
],
[
"Ofner",
"Maximilian",
""
],
[
"Oliynyk",
"Todd",
""
],
[
"Wyatt",
"Zoe",
""
]
] | We demonstrate a novel phase transition from stable to unstable fluid behaviour for fluid-filled cosmological spacetimes undergoing decelerated expansion. This transition occurs when the fluid speed of sound $c_S$ exceeds a critical value relative to the expansion rate $a(t) = t^\alpha$ of spacetime. We present an explicit relationship between $\alpha$ and $c_S$ , which subdivides the $(\alpha,c_S)$-parameter space into two regions. Using rigorous techniques, we establish stability of quiet fluid solutions in the first stable region. Numerical experiments reveal that the complement of the stable region consists of unstable solutions, implying sharpness of our stability result. We provide a definitive analytical bound and high-precision numerical evidence for the exact location of the critical line separating the stable from the unstable region. |
1504.06321 | Cristian Martinez | Cristian Erices and Cristian Martinez | Stationary cylindrically symmetric spacetimes with a massless scalar
field and a non-positive cosmological constant | 7 pages | Phys. Rev. D 92, 044051 (2015) | 10.1103/PhysRevD.92.044051 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The general stationary cylindrically symmetric solution of Einstein-massless
scalar field system with a non-positive cosmological constant is presented. It
is shown that the general solution is characterized by four integration
constants. Two of these essential parameters have a local meaning and
characterize the gravitational field strength. The other two have a topological
origin, as they define an improper coordinate transformation that provides the
stationary solution from the static one. The Petrov scheme is considered to
explore the effects of the scalar field on the algebraic classification of the
solutions. In general, these spacetimes are of type I. However, the presence of
the scalar field allows us to find a non-vacuum type O solution and a wider
family of type D spacetimes, in comparison with the vacuum case. The mass and
angular momentum of the solution are computed using the Regge-Teitelboim method
in the case of a negative cosmological constant. In absence of a cosmological
constant, the curvature singularities in the vacuum solutions can be removed by
including a phantom scalar field, yielding non-trivial locally homogeneous
spacetimes. These spacetimes are of particular interest, as they have all their
curvature invariants constant.
| [
{
"created": "Thu, 23 Apr 2015 20:00:13 GMT",
"version": "v1"
}
] | 2015-09-02 | [
[
"Erices",
"Cristian",
""
],
[
"Martinez",
"Cristian",
""
]
] | The general stationary cylindrically symmetric solution of Einstein-massless scalar field system with a non-positive cosmological constant is presented. It is shown that the general solution is characterized by four integration constants. Two of these essential parameters have a local meaning and characterize the gravitational field strength. The other two have a topological origin, as they define an improper coordinate transformation that provides the stationary solution from the static one. The Petrov scheme is considered to explore the effects of the scalar field on the algebraic classification of the solutions. In general, these spacetimes are of type I. However, the presence of the scalar field allows us to find a non-vacuum type O solution and a wider family of type D spacetimes, in comparison with the vacuum case. The mass and angular momentum of the solution are computed using the Regge-Teitelboim method in the case of a negative cosmological constant. In absence of a cosmological constant, the curvature singularities in the vacuum solutions can be removed by including a phantom scalar field, yielding non-trivial locally homogeneous spacetimes. These spacetimes are of particular interest, as they have all their curvature invariants constant. |
1910.03546 | Vasilis Oikonomou | Shin'ichi Nojiri, S.D. Odintsov, V.K. Oikonomou, Tanmoy Paul | Non-singular Bounce Cosmology from Lagrange Multiplier $F(R)$ Gravity | PRD Accepted | null | 10.1103/PhysRevD.100.084056 | null | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work we study non-singular{ bounce cosmology} in the context of the
Lagrange multiplier generalized $F(R)$ gravity theory of gravity. We specify
our study by using a specific variant form of the well known matter{ bounce
cosmology}, with scale factor $a(t) = \left(a_0t^2 + 1 \right)^n$, and we
demonstrate that for $n < 1/2$, the primordial curvature perturbations are
generated deeply in the contraction era. Particularly, we show explicitly that
the perturbation modes exit the horizon at a large negative time during the
contraction era, which in turn makes the ``low-curvature'' regime, the era for
which the calculations of observational indices related to the primordial power
spectrum can be considered reliable. Using the reconstruction techniques for
the Lagrange multiplier $F(R)$ gravity, we construct the form of effective
$F(R)$ gravity that can realize such a cosmological evolution, and we determine
the power spectrum of the primordial curvature perturbations. Accordingly, we
calculate the spectral index of the primordial curvature perturbations and the
tensor-to-scalar ratio, and we confront these with the latest observational
data. We also address the issue of stability of the primordial metric
perturbations, and to this end, we determine the form of $F(R)$ which realizes
the non-singular cosmology for the whole range of cosmic time $-\infty < t <
\infty$, by solving the Friedmann equations without the ``low-curvature''
approximation. This study is performed numerically though, due to the high
complexity of the resulting differential equations. We also investigate the
energy conditions in the present context. The phenomenology of the non-singular
bounce is also studied in the context of a standard $F(R)$ gravity.
| [
{
"created": "Tue, 8 Oct 2019 17:11:41 GMT",
"version": "v1"
}
] | 2020-01-08 | [
[
"Nojiri",
"Shin'ichi",
""
],
[
"Odintsov",
"S. D.",
""
],
[
"Oikonomou",
"V. K.",
""
],
[
"Paul",
"Tanmoy",
""
]
] | In this work we study non-singular{ bounce cosmology} in the context of the Lagrange multiplier generalized $F(R)$ gravity theory of gravity. We specify our study by using a specific variant form of the well known matter{ bounce cosmology}, with scale factor $a(t) = \left(a_0t^2 + 1 \right)^n$, and we demonstrate that for $n < 1/2$, the primordial curvature perturbations are generated deeply in the contraction era. Particularly, we show explicitly that the perturbation modes exit the horizon at a large negative time during the contraction era, which in turn makes the ``low-curvature'' regime, the era for which the calculations of observational indices related to the primordial power spectrum can be considered reliable. Using the reconstruction techniques for the Lagrange multiplier $F(R)$ gravity, we construct the form of effective $F(R)$ gravity that can realize such a cosmological evolution, and we determine the power spectrum of the primordial curvature perturbations. Accordingly, we calculate the spectral index of the primordial curvature perturbations and the tensor-to-scalar ratio, and we confront these with the latest observational data. We also address the issue of stability of the primordial metric perturbations, and to this end, we determine the form of $F(R)$ which realizes the non-singular cosmology for the whole range of cosmic time $-\infty < t < \infty$, by solving the Friedmann equations without the ``low-curvature'' approximation. This study is performed numerically though, due to the high complexity of the resulting differential equations. We also investigate the energy conditions in the present context. The phenomenology of the non-singular bounce is also studied in the context of a standard $F(R)$ gravity. |
1101.1690 | Hanno Sahlmann | Hanno Sahlmann and Thomas Thiemann | Chern-Simons theory, Stokes' Theorem, and the Duflo map | 26 pages, 8 figures | J.Geom.Phys.61:1104-1121,2011 | 10.1016/j.geomphys.2011.02.013 | APCTP Pre2010-007 | gr-qc math-ph math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We consider a novel derivation of the expectation values of holonomies in
Chern-Simons theory, based on Stokes' Theorem and the functional properties of
the Chern-Simons action. It involves replacing the connection by certain
functional derivatives under the path integral integral. It turns out that
ordering choices have to be made in the process, and we demonstrate that, quite
surprisingly, the Duflo isomorphism gives the right ordering, at least in the
simple cases that we consider. In this way, we determine the expectation values
of unknotted, but possibly linked, holonomy loops for SU(2) and SU(3), and
sketch how the method may be applied to more complicated cases. Our
manipulations of the path integral are formal but well motivated by a rigorous
calculus of integration on spaces of generalized connections which has been
developed in the context of loop quantum gravity.
| [
{
"created": "Mon, 10 Jan 2011 00:21:00 GMT",
"version": "v1"
}
] | 2011-05-26 | [
[
"Sahlmann",
"Hanno",
""
],
[
"Thiemann",
"Thomas",
""
]
] | We consider a novel derivation of the expectation values of holonomies in Chern-Simons theory, based on Stokes' Theorem and the functional properties of the Chern-Simons action. It involves replacing the connection by certain functional derivatives under the path integral integral. It turns out that ordering choices have to be made in the process, and we demonstrate that, quite surprisingly, the Duflo isomorphism gives the right ordering, at least in the simple cases that we consider. In this way, we determine the expectation values of unknotted, but possibly linked, holonomy loops for SU(2) and SU(3), and sketch how the method may be applied to more complicated cases. Our manipulations of the path integral are formal but well motivated by a rigorous calculus of integration on spaces of generalized connections which has been developed in the context of loop quantum gravity. |
gr-qc/9703008 | Renaud Parentani | Renaud Parentani | The interpretation of the solutions of the Wheeler De Witt equation | 11 pages, latex, no figures | Phys.Rev. D56 (1997) 4618-4624 | 10.1103/PhysRevD.56.4618 | null | gr-qc | null | We extract transition amplitudes among matter constituents of the universe
from the solutions of the Wheeler De Witt equation. The physical interpretation
of these solutions is then reached by an analysis of the properties of the
transition amplitudes. The interpretation so obtained is based on the current
carried by these solutions and confirms ideas put forward by Vilenkin.
| [
{
"created": "Tue, 4 Mar 1997 11:14:32 GMT",
"version": "v1"
}
] | 2009-10-30 | [
[
"Parentani",
"Renaud",
""
]
] | We extract transition amplitudes among matter constituents of the universe from the solutions of the Wheeler De Witt equation. The physical interpretation of these solutions is then reached by an analysis of the properties of the transition amplitudes. The interpretation so obtained is based on the current carried by these solutions and confirms ideas put forward by Vilenkin. |
2007.05988 | Grigory Volovik | G.E. Volovik | Double Hawking temperature in de Sitter Universe and cosmological
constant problem | 7 pages, no figures | null | null | null | gr-qc cond-mat.other hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | As distinct from the black hole physics, the de Sitter thermodynamics is not
determined by the cosmological horizon, the effective temperature differs from
the Hawking temperature. In particular, the atom in the de Sitter universe
experiences thermal activation corresponding to the local temperature, which is
twice larger than the Hawking temperature, $T_{\rm loc}=2T_{\rm Hawking}$. The
same double Hawking temperature describes the decay of massive scalar field in
the de Sitter universe. The reason, why the local temperature is exactly twice
the Hawking temperature, follows from the geometry of the de Sitter spacetime.
The weakening of the role of the cosmological horizon in de Sitter universe is
confirmed by considering Hawking radiation. We discuss the difference between
the radiation of particles in the de Sitter spacetime and the Schwinger pair
creation in the electric field. We use the stationary Painleve-Gullstrand
metric for the de Sitter spacetime, where the particles are created by Hawking
radiation from the cosmological horizon, and time independent gauge for the
electric field. In these stationary frames the Hamiltonians and the energy
spectra of massive particles look rather similar. However, the final results
are essentially different. In case of Schwinger pair production the number
density of the created pairs grows with time, while in the de Sitter vacuum the
number density of the created pairs is finite. The latter suggests that Hawking
radiation from the cosmological horizon does not lead to instability of the de
Sitter vacuum. The other mechanisms of instability are required for the
dynamical solution of the cosmological constant problem. We consider the
possible role of the local temperature $T_{\rm loc}=2T_{\rm H}$ in the decay of
the de Sitter space-time due to the energy exchange between the vacuum energy
and relativistic matter with this temperature.
| [
{
"created": "Sun, 12 Jul 2020 13:37:22 GMT",
"version": "v1"
},
{
"created": "Sat, 29 Aug 2020 15:01:50 GMT",
"version": "v2"
},
{
"created": "Mon, 7 Sep 2020 13:12:44 GMT",
"version": "v3"
},
{
"created": "Mon, 26 Oct 2020 09:26:03 GMT",
"version": "v4"
},
{
"created": "Sun, 6 Dec 2020 11:11:30 GMT",
"version": "v5"
},
{
"created": "Mon, 19 Apr 2021 09:34:34 GMT",
"version": "v6"
},
{
"created": "Wed, 21 Apr 2021 12:16:26 GMT",
"version": "v7"
}
] | 2021-04-22 | [
[
"Volovik",
"G. E.",
""
]
] | As distinct from the black hole physics, the de Sitter thermodynamics is not determined by the cosmological horizon, the effective temperature differs from the Hawking temperature. In particular, the atom in the de Sitter universe experiences thermal activation corresponding to the local temperature, which is twice larger than the Hawking temperature, $T_{\rm loc}=2T_{\rm Hawking}$. The same double Hawking temperature describes the decay of massive scalar field in the de Sitter universe. The reason, why the local temperature is exactly twice the Hawking temperature, follows from the geometry of the de Sitter spacetime. The weakening of the role of the cosmological horizon in de Sitter universe is confirmed by considering Hawking radiation. We discuss the difference between the radiation of particles in the de Sitter spacetime and the Schwinger pair creation in the electric field. We use the stationary Painleve-Gullstrand metric for the de Sitter spacetime, where the particles are created by Hawking radiation from the cosmological horizon, and time independent gauge for the electric field. In these stationary frames the Hamiltonians and the energy spectra of massive particles look rather similar. However, the final results are essentially different. In case of Schwinger pair production the number density of the created pairs grows with time, while in the de Sitter vacuum the number density of the created pairs is finite. The latter suggests that Hawking radiation from the cosmological horizon does not lead to instability of the de Sitter vacuum. The other mechanisms of instability are required for the dynamical solution of the cosmological constant problem. We consider the possible role of the local temperature $T_{\rm loc}=2T_{\rm H}$ in the decay of the de Sitter space-time due to the energy exchange between the vacuum energy and relativistic matter with this temperature. |
gr-qc/0512005 | Sang Pyo Kim | Sang Pyo Kim (Kunsan Nat'l Univ.) | Quasinormal modes of black holes and dissipative open systems | RevTex 9 pages, one figure; Talks at Black Hole V, Canada, 2005 and
9th Italian-Korean Symposium, Korea, 2005; note and references added in proof | J.Korean Phys.Soc. 49 (2006) 764-772 | null | null | gr-qc astro-ph hep-th | null | After explaining the physical origin of the quasinormal modes of
perturbations in the background geometry of a black hole, I critically review
the recent proposal for the quantization of the black-hole area based on the
real part of quasinormal modes. As instantons due to the barriers of black-hole
potentials lie at the root of a discrete set of complex quasinormal modes
frequencies, it is likely that the physics of quasinormal modes can be learned
from quantum theory. I propose a connection of a system of quasinormal modes of
black holes with a dissipative open system, in particular, the
Feshbach-Tikochinsky oscillator. This argument is supported in part by the fact
that these two systems have the same group structure SU(1,1) and the same group
representation of Hamiltonians; thereby, their quantum states exhibit the same
behavior.
| [
{
"created": "Thu, 1 Dec 2005 01:08:09 GMT",
"version": "v1"
},
{
"created": "Tue, 3 Jan 2006 13:15:14 GMT",
"version": "v2"
}
] | 2007-05-23 | [
[
"Kim",
"Sang Pyo",
"",
"Kunsan Nat'l Univ."
]
] | After explaining the physical origin of the quasinormal modes of perturbations in the background geometry of a black hole, I critically review the recent proposal for the quantization of the black-hole area based on the real part of quasinormal modes. As instantons due to the barriers of black-hole potentials lie at the root of a discrete set of complex quasinormal modes frequencies, it is likely that the physics of quasinormal modes can be learned from quantum theory. I propose a connection of a system of quasinormal modes of black holes with a dissipative open system, in particular, the Feshbach-Tikochinsky oscillator. This argument is supported in part by the fact that these two systems have the same group structure SU(1,1) and the same group representation of Hamiltonians; thereby, their quantum states exhibit the same behavior. |
2012.02432 | Matsuno Satsuki | Hideki Ishihara, Satsuki Matsuno | Solutions to the Einstein-Maxwell-Current System with Sasakian maifolds | 16 pages, no figures | null | null | null | gr-qc math.DG | http://creativecommons.org/publicdomain/zero/1.0/ | We construct stationary solutions to the Einstein-Maxwell-current system by
using the Sasakian manifold for the three-dimensional space. Both the magnetic
field and the electric current in the solution are specified by the contact
form of the Sasakian manifold. The solutions contain an arbitrary function that
describes inhomogeneity of the number density of the charged particles, and the
function determines the curvature of the space.
| [
{
"created": "Fri, 4 Dec 2020 07:02:28 GMT",
"version": "v1"
}
] | 2020-12-07 | [
[
"Ishihara",
"Hideki",
""
],
[
"Matsuno",
"Satsuki",
""
]
] | We construct stationary solutions to the Einstein-Maxwell-current system by using the Sasakian manifold for the three-dimensional space. Both the magnetic field and the electric current in the solution are specified by the contact form of the Sasakian manifold. The solutions contain an arbitrary function that describes inhomogeneity of the number density of the charged particles, and the function determines the curvature of the space. |
1709.05577 | Marcos Ramirez | Marcos A. Ramirez | Vacuum thin shells in Einstein-Gauss-Bonnet brane-world cosmology | 20 pages, 5 figures | Class.Quant.Grav. 35 (2018) no.8, 085004 | 10.1088/1361-6382/aab0da | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper we construct new solutions of the Einstein-Gauss-Bonnet field
equations in an isotropic Shiromizu-Maeda-Sasaki brane-world setting which
represent a couple of $Z_2$-symmetric vacuum thin shells splitting from the
central brane, and explore the main properties of the dynamics of the system.
The matching of the separating vacuum shells with the brane-world is as smooth
as possible and all matter fields are restricted to the brane. We prove the
existence of these solutions, derive the criteria for their existence, analyse
some fundamental aspects or their evolution and demonstrate the possibility of
constructing cosmological examples that exhibit this feature at early times. We
also comment on the possible implications for cosmology and the relation of
this system with the thermodynamic instability of highly symmetric vacuum
solutions of Lovelock theory.
| [
{
"created": "Sat, 16 Sep 2017 22:59:50 GMT",
"version": "v1"
},
{
"created": "Fri, 16 Feb 2018 17:51:45 GMT",
"version": "v2"
}
] | 2018-03-26 | [
[
"Ramirez",
"Marcos A.",
""
]
] | In this paper we construct new solutions of the Einstein-Gauss-Bonnet field equations in an isotropic Shiromizu-Maeda-Sasaki brane-world setting which represent a couple of $Z_2$-symmetric vacuum thin shells splitting from the central brane, and explore the main properties of the dynamics of the system. The matching of the separating vacuum shells with the brane-world is as smooth as possible and all matter fields are restricted to the brane. We prove the existence of these solutions, derive the criteria for their existence, analyse some fundamental aspects or their evolution and demonstrate the possibility of constructing cosmological examples that exhibit this feature at early times. We also comment on the possible implications for cosmology and the relation of this system with the thermodynamic instability of highly symmetric vacuum solutions of Lovelock theory. |
1508.04943 | Oleg Evnin | Ben Craps, Oleg Evnin, Joris Vanhoof | Ultraviolet asymptotics and singular dynamics of AdS perturbations | 15 pages; v4: typos in equation (33) corrected | JHEP 1510 (2015) 079 | 10.1007/JHEP10(2015)079 | null | gr-qc hep-th nlin.CD | http://creativecommons.org/licenses/by-nc-sa/4.0/ | Important insights into the dynamics of spherically symmetric AdS-scalar
field perturbations can be obtained by considering a simplified time-averaged
theory accurately describing perturbations of amplitude epsilon on time-scales
of order 1/epsilon^2. The coefficients of the time-averaged equations are
complicated expressions in terms of the AdS scalar field mode functions, which
are in turn related to the Jacobi polynomials. We analyze the behavior of these
coefficients for high frequency modes. The resulting asymptotics can be useful
for understanding the properties of the finite-time singularity in solutions of
the time-averaged theory recently reported in the literature. We highlight, in
particular, the gauge dependence of this asymptotics, with respect to the two
most commonly used gauges. The harsher growth of the coefficients at large
frequencies in higher-dimensional AdS suggests strengthening of turbulent
instabilities in higher dimensions. In the course of our derivations, we arrive
at recursive relations for the coefficients of the time-averaged theory that
are likely to be useful for evaluating them more efficiently in numerical
simulations.
| [
{
"created": "Thu, 20 Aug 2015 10:27:17 GMT",
"version": "v1"
},
{
"created": "Fri, 4 Sep 2015 04:47:14 GMT",
"version": "v2"
},
{
"created": "Thu, 29 Oct 2015 05:47:01 GMT",
"version": "v3"
},
{
"created": "Thu, 12 Nov 2015 01:27:58 GMT",
"version": "v4"
}
] | 2015-11-13 | [
[
"Craps",
"Ben",
""
],
[
"Evnin",
"Oleg",
""
],
[
"Vanhoof",
"Joris",
""
]
] | Important insights into the dynamics of spherically symmetric AdS-scalar field perturbations can be obtained by considering a simplified time-averaged theory accurately describing perturbations of amplitude epsilon on time-scales of order 1/epsilon^2. The coefficients of the time-averaged equations are complicated expressions in terms of the AdS scalar field mode functions, which are in turn related to the Jacobi polynomials. We analyze the behavior of these coefficients for high frequency modes. The resulting asymptotics can be useful for understanding the properties of the finite-time singularity in solutions of the time-averaged theory recently reported in the literature. We highlight, in particular, the gauge dependence of this asymptotics, with respect to the two most commonly used gauges. The harsher growth of the coefficients at large frequencies in higher-dimensional AdS suggests strengthening of turbulent instabilities in higher dimensions. In the course of our derivations, we arrive at recursive relations for the coefficients of the time-averaged theory that are likely to be useful for evaluating them more efficiently in numerical simulations. |
gr-qc/0007025 | Izumi Tanaka | T.Kawai, K. Shibata, I.Tanaka | Generalized Equivalence Principle in Extended New General Relativity | 35 pages | Prog.Theor.Phys. 104 (2000) 505-530; Erratum-ibid. 104 (2000)
1115-1116 | 10.1143/PTP.104.505 | null | gr-qc | null | In extended new general relativity, which is formulated as a reduction of
$\bar{Poincar\'e} $gauge theory of gravity whose gauge group is the covering
group of the Poincar\'e group, we study the problem of whether the total
energy-momentum, total angular momentum and total charge are equal to the
corresponding quantities of the gravitational source. We examine this for
charged axi-symmetric solutions of gravitational field equations. Our main
concern is the restriction on the asymptotic form of the gravitational field
variables imposed by the requirement that physical quantities of the total
system are equivalent to the corresponding quantities of the charged rotating
source body. This requirement can be regarded as an equivalence principle in a
generalized sense.
| [
{
"created": "Thu, 13 Jul 2000 04:37:52 GMT",
"version": "v1"
},
{
"created": "Fri, 1 Dec 2000 04:12:21 GMT",
"version": "v2"
}
] | 2009-10-31 | [
[
"Kawai",
"T.",
""
],
[
"Shibata",
"K.",
""
],
[
"Tanaka",
"I.",
""
]
] | In extended new general relativity, which is formulated as a reduction of $\bar{Poincar\'e} $gauge theory of gravity whose gauge group is the covering group of the Poincar\'e group, we study the problem of whether the total energy-momentum, total angular momentum and total charge are equal to the corresponding quantities of the gravitational source. We examine this for charged axi-symmetric solutions of gravitational field equations. Our main concern is the restriction on the asymptotic form of the gravitational field variables imposed by the requirement that physical quantities of the total system are equivalent to the corresponding quantities of the charged rotating source body. This requirement can be regarded as an equivalence principle in a generalized sense. |
2306.00870 | Aneta Wojnar | Eva Lope-Oter, Aneta Wojnar | Constraining Palatini gravity with GR-independent equations of state for
neutron stars | 39 pages, 20 figures, 4 tables, accepted to JCAP | JCAP 02 (2024) 017 | 10.1088/1475-7516/2024/02/017 | null | gr-qc astro-ph.HE hep-ph nucl-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We demonstrate how to construct GR-independent equations of state. We
emphasize the importance of using theory-based principles instead of relying
solely on astrophysical observables and General Relativity (GR). We build a set
of equations of state based on first principles, including chiral perturbation
theory and perturbation theory in quantum chromodynamics. Interpolation methods
are employed to assume thermodynamic stability and causality in the
intermediate region. These equations of state are then used to constrain
quadratic Palatini $f(\mathcal R)$ gravity, indicating that the parameter lies
within the range $-6.47 \lesssim \beta \lesssim 1.99$ km$^2$. Additionally, we
briefly discuss the problem of phase transitions and twin stars.
| [
{
"created": "Thu, 1 Jun 2023 16:30:05 GMT",
"version": "v1"
},
{
"created": "Fri, 19 Jan 2024 11:59:10 GMT",
"version": "v2"
}
] | 2024-02-12 | [
[
"Lope-Oter",
"Eva",
""
],
[
"Wojnar",
"Aneta",
""
]
] | We demonstrate how to construct GR-independent equations of state. We emphasize the importance of using theory-based principles instead of relying solely on astrophysical observables and General Relativity (GR). We build a set of equations of state based on first principles, including chiral perturbation theory and perturbation theory in quantum chromodynamics. Interpolation methods are employed to assume thermodynamic stability and causality in the intermediate region. These equations of state are then used to constrain quadratic Palatini $f(\mathcal R)$ gravity, indicating that the parameter lies within the range $-6.47 \lesssim \beta \lesssim 1.99$ km$^2$. Additionally, we briefly discuss the problem of phase transitions and twin stars. |
1409.4680 | Michael Coughlin | Michael Coughlin and Jan Harms | Constraining the gravitational wave energy density of the Universe in
the Range 0.1 Hz to 1 Hz using the Apollo Seismic Array | null | null | 10.1103/PhysRevD.90.102001 | null | gr-qc astro-ph.IM | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, we describe an analysis of Apollo era lunar seismic data that
places an upper limit on an isotropic stochastic gravitational-wave background
integrated over a year in the frequency range 0.1\,Hz -- 1\,Hz. We find that
because the Moon's ambient noise background is much quieter than that of the
Earth, significant improvements over an Earth based analysis were made. We find
an upper limit of $\Omega_{\rm GW}<1.2\times 10^{5}$, which is three orders of
magnitude smaller than a similar analysis of a global network of broadband
seismometers on Earth and the best limits in this band to date. We also discuss
the benefits of a potential Earth-Moon correlation search and compute the
time-dependent overlap reduction function required for such an analysis. For
this search, we find an upper limit an order of magnitude larger than the
Moon-Moon search.
| [
{
"created": "Tue, 16 Sep 2014 15:55:01 GMT",
"version": "v1"
},
{
"created": "Tue, 7 Oct 2014 18:15:02 GMT",
"version": "v2"
},
{
"created": "Sat, 11 Oct 2014 20:22:43 GMT",
"version": "v3"
}
] | 2015-06-22 | [
[
"Coughlin",
"Michael",
""
],
[
"Harms",
"Jan",
""
]
] | In this paper, we describe an analysis of Apollo era lunar seismic data that places an upper limit on an isotropic stochastic gravitational-wave background integrated over a year in the frequency range 0.1\,Hz -- 1\,Hz. We find that because the Moon's ambient noise background is much quieter than that of the Earth, significant improvements over an Earth based analysis were made. We find an upper limit of $\Omega_{\rm GW}<1.2\times 10^{5}$, which is three orders of magnitude smaller than a similar analysis of a global network of broadband seismometers on Earth and the best limits in this band to date. We also discuss the benefits of a potential Earth-Moon correlation search and compute the time-dependent overlap reduction function required for such an analysis. For this search, we find an upper limit an order of magnitude larger than the Moon-Moon search. |
gr-qc/0602009 | Pavel Krtous | Jiri Bicak, Pavel Krtous | Fields of accelerated sources: Born in de Sitter | 37 pages, 23 figures, reformatted version of the paper published in
JMP; low-resolution figures due to arXiv size restrictions; for the version
with high-resolution figures see http://utf.mff.cuni.cz/~krtous/papers/ | J.Math.Phys. 46 (2005) 102504 | 10.1063/1.2009647 | null | gr-qc | null | This paper deals thoroughly with the scalar and electromagnetic fields of
uniformly accelerated charges in de Sitter spacetime. It gives details and
makes various extensions of our Physical Review Letter from 2002. The basic
properties of the classical Born solutions representing two uniformly
accelerated charges in flat spacetime are first summarized. The worldlines of
uniformly accelerated particles in de Sitter universe are defined and described
in a number of coordinate frames, some of them being of cosmological
significance, the other are tied naturally to the particles. The scalar and
electromagnetic fields due to the accelerated charges are constructed by using
conformal relations between Minkowski and de Sitter space. The properties of
the generalized `cosmological' Born solutions are analyzed and elucidated in
various coordinate systems. In particular, a limiting procedure is demonstrated
which brings the cosmological Born fields in de Sitter space back to the
classical Born solutions in Minkowski space. In an extensive Appendix, which
can be used independently of the main text, nine families of coordinate systems
in de Sitter spacetime are described analytically and illustrated graphically
in a number of conformal diagrams.
| [
{
"created": "Thu, 2 Feb 2006 14:12:59 GMT",
"version": "v1"
}
] | 2015-06-25 | [
[
"Bicak",
"Jiri",
""
],
[
"Krtous",
"Pavel",
""
]
] | This paper deals thoroughly with the scalar and electromagnetic fields of uniformly accelerated charges in de Sitter spacetime. It gives details and makes various extensions of our Physical Review Letter from 2002. The basic properties of the classical Born solutions representing two uniformly accelerated charges in flat spacetime are first summarized. The worldlines of uniformly accelerated particles in de Sitter universe are defined and described in a number of coordinate frames, some of them being of cosmological significance, the other are tied naturally to the particles. The scalar and electromagnetic fields due to the accelerated charges are constructed by using conformal relations between Minkowski and de Sitter space. The properties of the generalized `cosmological' Born solutions are analyzed and elucidated in various coordinate systems. In particular, a limiting procedure is demonstrated which brings the cosmological Born fields in de Sitter space back to the classical Born solutions in Minkowski space. In an extensive Appendix, which can be used independently of the main text, nine families of coordinate systems in de Sitter spacetime are described analytically and illustrated graphically in a number of conformal diagrams. |
1506.06153 | Carlos O. Lousto | James Healy, Ian Ruchlin, Carlos O. Lousto, and Yosef Zlochower | High Energy Collisions of Black Holes Numerically Revisited | 11 pages, 10 figures | Phys. Rev. D 94, 104020 (2016) | 10.1103/PhysRevD.94.104020 | null | gr-qc astro-ph.HE hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We use fully nonlinear numerical relativity techniques to study high energy
head-on collision of nonspinning, equal-mass black holes to estimate the
maximum gravitational radiation emitted by these systems. Our simulations
include improvements in the construction of initial data, subsequent full
numerical evolutions, and the computation of waveforms at infinity. The new
initial data significantly reduces the spurious radiation content, allowing for
initial speeds much closer to the speed of light, i.e. $v\sim0.99c$. Using
these new techniques, We estimate the maximum radiated energy from head-on
collisions to be $E_{\text{max}}/M_{\text{ADM}}=0.13\pm0.01$. This value
differs from the second-order perturbative $(0.164)$ and zero-frequency-limit
$(0.17)$ analytic computations, but is close to those obtained by thermodynamic
arguments $(0.134)$ and by previous numerical estimates $(0.14\pm0.03)$.
| [
{
"created": "Fri, 19 Jun 2015 20:36:58 GMT",
"version": "v1"
},
{
"created": "Wed, 24 Aug 2016 20:00:37 GMT",
"version": "v2"
}
] | 2016-11-15 | [
[
"Healy",
"James",
""
],
[
"Ruchlin",
"Ian",
""
],
[
"Lousto",
"Carlos O.",
""
],
[
"Zlochower",
"Yosef",
""
]
] | We use fully nonlinear numerical relativity techniques to study high energy head-on collision of nonspinning, equal-mass black holes to estimate the maximum gravitational radiation emitted by these systems. Our simulations include improvements in the construction of initial data, subsequent full numerical evolutions, and the computation of waveforms at infinity. The new initial data significantly reduces the spurious radiation content, allowing for initial speeds much closer to the speed of light, i.e. $v\sim0.99c$. Using these new techniques, We estimate the maximum radiated energy from head-on collisions to be $E_{\text{max}}/M_{\text{ADM}}=0.13\pm0.01$. This value differs from the second-order perturbative $(0.164)$ and zero-frequency-limit $(0.17)$ analytic computations, but is close to those obtained by thermodynamic arguments $(0.134)$ and by previous numerical estimates $(0.14\pm0.03)$. |
0905.0789 | Salvatore Antoci | Salvatore Antoci | The propagation of waves in Einstein's unified field theory as shown by
two exact solutions | 12 pages. Added footnote 6 details proof of propagation with the
fundamental velocity in the wave zone | Nuovo Cim.B124:619-630,2010 | 10.1393/ncb/i2009-10783-9 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The propagation of waves in two space dimensions exhibited by two exact
solutions to the field equations of Einstein's unified field theory is
investigated under the assumption that the metric s_{ik} is the one already
chosen by Kursunoglu and by H\'ely in the years 1952-1954. It is shown that,
for both exact solutions, with this choice of the metric the propagation of the
waves occurs in the wave zone with the fundamental velocity (ds^2=0).
| [
{
"created": "Wed, 6 May 2009 09:30:08 GMT",
"version": "v1"
},
{
"created": "Tue, 29 Sep 2009 10:34:52 GMT",
"version": "v2"
}
] | 2010-11-11 | [
[
"Antoci",
"Salvatore",
""
]
] | The propagation of waves in two space dimensions exhibited by two exact solutions to the field equations of Einstein's unified field theory is investigated under the assumption that the metric s_{ik} is the one already chosen by Kursunoglu and by H\'ely in the years 1952-1954. It is shown that, for both exact solutions, with this choice of the metric the propagation of the waves occurs in the wave zone with the fundamental velocity (ds^2=0). |
1405.5334 | Prasobh C.B | C.B. Prasobh, V.C. Kuriakose | Quasinormal Modes of Lovelock Black Holes | null | null | 10.1140/epjc/s10052-014-3136-4 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The quasinormal modes of metric perturbations in asymptotically flat black
hole spacetimes in the Lovelock model are calculated for different spacetime
dimensions and higher orders of curvature. It is analytically established that
in the asymptotic limit $l \rightarrow \infty$, the imaginary parts of the
quasi normal frequencies become constant for tensor, scalar as well as vector
perturbations. Numerical calculation shows that this indeed is the case. Also,
the real and imaginary parts of the quasinormal modes are seen to increase as
the order of the theory $k$ increases. The real part of the modes decreases as
the spacetime dimension $d$ increases, indicating the presence of lower
frequency modes in higher dimensions. Also, it is seen that the modes are
roughly isospectral at very high values of the spacetime dimension $d$.
| [
{
"created": "Wed, 21 May 2014 08:50:25 GMT",
"version": "v1"
}
] | 2015-06-19 | [
[
"Prasobh",
"C. B.",
""
],
[
"Kuriakose",
"V. C.",
""
]
] | The quasinormal modes of metric perturbations in asymptotically flat black hole spacetimes in the Lovelock model are calculated for different spacetime dimensions and higher orders of curvature. It is analytically established that in the asymptotic limit $l \rightarrow \infty$, the imaginary parts of the quasi normal frequencies become constant for tensor, scalar as well as vector perturbations. Numerical calculation shows that this indeed is the case. Also, the real and imaginary parts of the quasinormal modes are seen to increase as the order of the theory $k$ increases. The real part of the modes decreases as the spacetime dimension $d$ increases, indicating the presence of lower frequency modes in higher dimensions. Also, it is seen that the modes are roughly isospectral at very high values of the spacetime dimension $d$. |
2101.00785 | Junji Jia | Haotian Liu and Junji Jia | Time delay in the strong field limit for null and timelike signals and
its simple interpretation | 24 pages, 3 figures | null | 10.1140/epjc/s10052-021-09659-8 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Gravitational lensing can happen not only for null signal but also timelike
signals such as neutrinos and massive gravitational waves in some theories
beyond GR. In this work we study the time delay between different relativistic
images formed by signals with arbitrary asymptotic velocity $v$ in general
static and spherically symmetric spacetimes. A perturbative method is used to
calculate the total travel time in the strong field limit, which is found to be
in quasi-series of the small parameter $a=1-b_c/b$ where $b$ is the impact
parameter and $b_c$ is its critical value. The coefficients of the series are
completely fixed by the behaviour of the metric functions near the particle
sphere $r_c$ and only the first term of the series contains a weak logarithmic
divergence. The time delay $\Delta t_{n,m}$ to the leading non-trivial order
was shown to equal the particle sphere circumference divided by the local
signal velocity and multiplied by the winding number and the redshift factor.
By assuming the Sgr A* supermassive black hole is a Hayward one, we were able
to validate the quasi-series form of the total time, and reveal the effects of
the spacetime parameter $l$, the signal velocity $v$ and the source/detector
coordinate difference $\Delta\phi_{sd}$ on the time delay. It is found that as
$l$ increase from 0 to its critical value $l_c$, both $r_c$ and $\Delta
t_{n,m}$ decrease. The variation of $\Delta t_{n+1,n}$ for $l$ from 0 to $l_c$
can be as large as $7.2\times 10^1$ [s], whose measurement then can be used to
constrain the value of $l$. While for ultra-relativistic neutrino or
gravitational wave, the variation of $\Delta t_{n,m}$ is too small to be
resolved. The dependence of $\Delta t_{n,-n}$ on $\Delta \phi_{sd}$ shows that
to temporally resolve the two sequences of images from opposite sides of the
lens, $|\Delta \phi_{sd}-\pi|$ has to be larger than certain value.
| [
{
"created": "Mon, 4 Jan 2021 05:54:47 GMT",
"version": "v1"
}
] | 2021-10-27 | [
[
"Liu",
"Haotian",
""
],
[
"Jia",
"Junji",
""
]
] | Gravitational lensing can happen not only for null signal but also timelike signals such as neutrinos and massive gravitational waves in some theories beyond GR. In this work we study the time delay between different relativistic images formed by signals with arbitrary asymptotic velocity $v$ in general static and spherically symmetric spacetimes. A perturbative method is used to calculate the total travel time in the strong field limit, which is found to be in quasi-series of the small parameter $a=1-b_c/b$ where $b$ is the impact parameter and $b_c$ is its critical value. The coefficients of the series are completely fixed by the behaviour of the metric functions near the particle sphere $r_c$ and only the first term of the series contains a weak logarithmic divergence. The time delay $\Delta t_{n,m}$ to the leading non-trivial order was shown to equal the particle sphere circumference divided by the local signal velocity and multiplied by the winding number and the redshift factor. By assuming the Sgr A* supermassive black hole is a Hayward one, we were able to validate the quasi-series form of the total time, and reveal the effects of the spacetime parameter $l$, the signal velocity $v$ and the source/detector coordinate difference $\Delta\phi_{sd}$ on the time delay. It is found that as $l$ increase from 0 to its critical value $l_c$, both $r_c$ and $\Delta t_{n,m}$ decrease. The variation of $\Delta t_{n+1,n}$ for $l$ from 0 to $l_c$ can be as large as $7.2\times 10^1$ [s], whose measurement then can be used to constrain the value of $l$. While for ultra-relativistic neutrino or gravitational wave, the variation of $\Delta t_{n,m}$ is too small to be resolved. The dependence of $\Delta t_{n,-n}$ on $\Delta \phi_{sd}$ shows that to temporally resolve the two sequences of images from opposite sides of the lens, $|\Delta \phi_{sd}-\pi|$ has to be larger than certain value. |
gr-qc/0309038 | Alessandro D. A. M. Spallicci | Marco Ferraris (1), Alessandro D.A.M. Spallicci (2) ((1) Dip.
Matematica, Univ. di Torino, (2) Observatoire de la Cote d'Azur, Nice) | Solutions of all one-dimensional wave equations with time independent
potential and separable variables | 10 pages, 1 figure. Accepted by Gen. Rel. Grav. J. | Gen.Rel.Grav. 36 (2004) 1955-1963 | 10.1023/B:GERG.0000036053.75204.a2 | null | gr-qc math-ph math.AP math.MP | null | Exact solutions, in terms of special functions, of all wave equations $%
u_{xx} - u_{tt} = V(x) u(t,x)$, characterised by eight inequivalent time
independent potentials and by variable separation, have been found. The real
valueness of the solutions from computer algebra programs is not always
manifest and in this work we provide ready to use solutions. We discussed
especially the potential $\cosh^{-2}x (m_1 + m_2 \sinh x)$. Such potential
approximates the Schwarzschild black hole potential for even parity.
| [
{
"created": "Sun, 7 Sep 2003 08:37:53 GMT",
"version": "v1"
},
{
"created": "Wed, 21 Jan 2004 13:55:15 GMT",
"version": "v2"
}
] | 2009-11-10 | [
[
"Ferraris",
"Marco",
""
],
[
"Spallicci",
"Alessandro D. A. M.",
""
]
] | Exact solutions, in terms of special functions, of all wave equations $% u_{xx} - u_{tt} = V(x) u(t,x)$, characterised by eight inequivalent time independent potentials and by variable separation, have been found. The real valueness of the solutions from computer algebra programs is not always manifest and in this work we provide ready to use solutions. We discussed especially the potential $\cosh^{-2}x (m_1 + m_2 \sinh x)$. Such potential approximates the Schwarzschild black hole potential for even parity. |
2208.10260 | Ernesto Contreras | E. Contreras, E. Fuenmayor, G. Abell\'an | Uncharged and charged anisotropic like--Durgapal stellar model with
vanishing complexity | null | Eur. Phys. J. C 82, 187 (2022) | 10.1140/epjc/s10052-022-10154-x | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work we use the vanishing complexity factor as a supplementary
condition to construct uncharged and charged like--Durgapal models. We provide
the $g_{tt}$ component of the metric of the well-known Durgapal IV and V
solutions and a particular form for the anisotropy, related to the electric
charge, to close the system of differential equations. The physical acceptance
of the models is discussed.
| [
{
"created": "Thu, 18 Aug 2022 20:34:35 GMT",
"version": "v1"
}
] | 2022-08-31 | [
[
"Contreras",
"E.",
""
],
[
"Fuenmayor",
"E.",
""
],
[
"Abellán",
"G.",
""
]
] | In this work we use the vanishing complexity factor as a supplementary condition to construct uncharged and charged like--Durgapal models. We provide the $g_{tt}$ component of the metric of the well-known Durgapal IV and V solutions and a particular form for the anisotropy, related to the electric charge, to close the system of differential equations. The physical acceptance of the models is discussed. |
2310.06876 | Telem Ibungochouba Singh | Y. Onika Laxmi, Ningthoujam Media and T. Ibungochouba Singh | P-v criticality of charged Reissner-Nordstr{\"o}m-de Sitter black hole
under the influence of Lorentz violation theory | null | null | null | null | gr-qc hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, the modified Hawking radiation and the P-v criticality of
Reissner-Nordstr{\"o}m-de Sitter (RNdS) black hole are investigated by using
Dirac equation with Lorentz violation theory in curved space time. Taking
cosmological constant as the thermodynamic pressure and its conjugate quantity
as thermodynamic volume, the analogy between the RNdS black hole in the
ensemble with fixed charge and van der Waals liquid-gas system is derived. We
also study the equation of state, critical exponents, critical point, heat
capacity, entropy correction, Gibbs free energy. It is worth mentioning that
the critical temperature, entropy, Gibbs free energy and Helmholtz free energy
are modified but the critical exponents are found to be unchanged due to the
influence of Lorentz violation theory. We observe that the number of
Hawking-Page critical point increases due to Lorentz violation theory.
| [
{
"created": "Tue, 10 Oct 2023 04:33:46 GMT",
"version": "v1"
}
] | 2023-10-12 | [
[
"Laxmi",
"Y. Onika",
""
],
[
"Media",
"Ningthoujam",
""
],
[
"Singh",
"T. Ibungochouba",
""
]
] | In this paper, the modified Hawking radiation and the P-v criticality of Reissner-Nordstr{\"o}m-de Sitter (RNdS) black hole are investigated by using Dirac equation with Lorentz violation theory in curved space time. Taking cosmological constant as the thermodynamic pressure and its conjugate quantity as thermodynamic volume, the analogy between the RNdS black hole in the ensemble with fixed charge and van der Waals liquid-gas system is derived. We also study the equation of state, critical exponents, critical point, heat capacity, entropy correction, Gibbs free energy. It is worth mentioning that the critical temperature, entropy, Gibbs free energy and Helmholtz free energy are modified but the critical exponents are found to be unchanged due to the influence of Lorentz violation theory. We observe that the number of Hawking-Page critical point increases due to Lorentz violation theory. |
gr-qc/0101021 | Marc Mars | Marc Mars | The Wahlquist-Newman solution | LaTeX, 18 pages, no figures. Accepted for publication in Phys. Rev. D | Phys.Rev. D63 (2001) 064022 | 10.1103/PhysRevD.63.064022 | null | gr-qc | null | Based on a geometrical property which holds both for the Kerr metric and for
the Wahlquist metric we argue that the Kerr metric is a vacuum subcase of the
Wahlquist perfect-fluid solution. The Kerr-Newman metric is a physically
preferred charged generalization of the Kerr metric. We discuss which geometric
property makes this metric so special and claim that a charged generalization
of the Wahlquist metric satisfying a similar property should exist. This is the
Wahlquist-Newman metric, which we present explicitly in this paper. This family
of metrics has eight essential parameters and contains the Kerr-Newman-de
Sitter and the Wahlquist metrics, as well as the whole Pleba\'nski limit of the
rotating C-metric, as particular cases. We describe the basic geometric
properties of the Wahlquist-Newman metric, including the electromagnetic field
and its sources, the static limit of the family and the extension of the
spacetime across the horizon.
| [
{
"created": "Fri, 5 Jan 2001 15:29:35 GMT",
"version": "v1"
}
] | 2009-11-07 | [
[
"Mars",
"Marc",
""
]
] | Based on a geometrical property which holds both for the Kerr metric and for the Wahlquist metric we argue that the Kerr metric is a vacuum subcase of the Wahlquist perfect-fluid solution. The Kerr-Newman metric is a physically preferred charged generalization of the Kerr metric. We discuss which geometric property makes this metric so special and claim that a charged generalization of the Wahlquist metric satisfying a similar property should exist. This is the Wahlquist-Newman metric, which we present explicitly in this paper. This family of metrics has eight essential parameters and contains the Kerr-Newman-de Sitter and the Wahlquist metrics, as well as the whole Pleba\'nski limit of the rotating C-metric, as particular cases. We describe the basic geometric properties of the Wahlquist-Newman metric, including the electromagnetic field and its sources, the static limit of the family and the extension of the spacetime across the horizon. |
0808.2510 | Jeffrey Kaplan | Jeffrey D. Kaplan, David A. Nichols, and Kip S. Thorne | Post-Newtonian Approximation in Maxwell-Like Form | v4: Revised for resubmission to Phys Rev D, 6 pages. v3: Reformulated
in terms of DSX papers. Submitted to Phys Rev D, 6 pages. v2: Added
references. Changed definitions & conventions | Phys.Rev.D80:124014,2009 | 10.1103/PhysRevD.80.124014 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The equations of the linearized first post-Newtonian approximation to general
relativity are often written in "gravitoelectromagnetic" Maxwell-like form,
since that facilitates physical intuition. Damour, Soffel and Xu (DSX) (as a
side issue in their complex but elegant papers on relativistic celestial
mechanics) have expressed the first post-Newtonian approximation, including all
nonlinearities, in Maxwell-like form. This paper summarizes that DSX
Maxwell-like formalism (which is not easily extracted from their celestial
mechanics papers), and then extends it to include the post-Newtonian
(Landau-Lifshitz-based) gravitational momentum density, momentum flux (i.e.
gravitational stress tensor) and law of momentum conservation in Maxwell-like
form. The authors and their colleagues have found these Maxwell-like momentum
tools useful for developing physical intuition into numerical-relativity
simulations of compact binaries with spin.
| [
{
"created": "Tue, 19 Aug 2008 00:21:27 GMT",
"version": "v1"
},
{
"created": "Wed, 17 Sep 2008 21:34:01 GMT",
"version": "v2"
},
{
"created": "Wed, 25 Feb 2009 20:55:54 GMT",
"version": "v3"
},
{
"created": "Fri, 11 Sep 2009 20:51:58 GMT",
"version": "v4"
}
] | 2012-12-13 | [
[
"Kaplan",
"Jeffrey D.",
""
],
[
"Nichols",
"David A.",
""
],
[
"Thorne",
"Kip S.",
""
]
] | The equations of the linearized first post-Newtonian approximation to general relativity are often written in "gravitoelectromagnetic" Maxwell-like form, since that facilitates physical intuition. Damour, Soffel and Xu (DSX) (as a side issue in their complex but elegant papers on relativistic celestial mechanics) have expressed the first post-Newtonian approximation, including all nonlinearities, in Maxwell-like form. This paper summarizes that DSX Maxwell-like formalism (which is not easily extracted from their celestial mechanics papers), and then extends it to include the post-Newtonian (Landau-Lifshitz-based) gravitational momentum density, momentum flux (i.e. gravitational stress tensor) and law of momentum conservation in Maxwell-like form. The authors and their colleagues have found these Maxwell-like momentum tools useful for developing physical intuition into numerical-relativity simulations of compact binaries with spin. |
2007.10116 | Alexander Zhidenko | R. A. Konoplya and A. Zhidenko | Simply rotating higher dimensional black holes in Einstein-Gauss-Bonnet
theory | 12 pages, 1 figure | Phys. Rev. D 102, 084030 (2020) | 10.1103/PhysRevD.102.084030 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Using perturbative expansion in terms of powers of the rotation parameter $a$
we construct the axisymmetric and asymptotically flat black-hole metric in the
$D$-dimensional Einstein-Gauss-Bonnet theory. In five-dimensional spacetime we
find two solutions to the field equations, describing the asymptotically flat
black holes, though only one of them is perturbative in mass, that is, goes
over into the Minkowski spacetime when the black-hole mass goes to zero. We
obtain the perturbative black-hole solution up to the order $O(\alpha a^3)$ for
any $D$, where $\alpha$ is the Gauss-Bonnet coupling, while the $D=5$ solution
which is nonperturbative in mass is found in analytic form up to the order
$O(\alpha a^7)$. In order to check the convergence of the expansion in $a$ we
analyze characteristics of photon orbits in this spacetime and compute
frequencies of the photon orbits and radius of the photon sphere.
| [
{
"created": "Sun, 12 Jul 2020 21:53:03 GMT",
"version": "v1"
},
{
"created": "Wed, 14 Oct 2020 17:52:58 GMT",
"version": "v2"
}
] | 2020-10-15 | [
[
"Konoplya",
"R. A.",
""
],
[
"Zhidenko",
"A.",
""
]
] | Using perturbative expansion in terms of powers of the rotation parameter $a$ we construct the axisymmetric and asymptotically flat black-hole metric in the $D$-dimensional Einstein-Gauss-Bonnet theory. In five-dimensional spacetime we find two solutions to the field equations, describing the asymptotically flat black holes, though only one of them is perturbative in mass, that is, goes over into the Minkowski spacetime when the black-hole mass goes to zero. We obtain the perturbative black-hole solution up to the order $O(\alpha a^3)$ for any $D$, where $\alpha$ is the Gauss-Bonnet coupling, while the $D=5$ solution which is nonperturbative in mass is found in analytic form up to the order $O(\alpha a^7)$. In order to check the convergence of the expansion in $a$ we analyze characteristics of photon orbits in this spacetime and compute frequencies of the photon orbits and radius of the photon sphere. |
gr-qc/9912036 | Wang Mian | Mian Wang | The Scalar-Tensor Inflationary Cosmology | 17 pages, LaTex, no figure, changed some parameters and the tables | Phys.Rev. D61 (2000) 123511 | 10.1103/PhysRevD.61.123511 | null | gr-qc astro-ph hep-ph | null | In this paper the scalar-tensor theory of gravity is assumed to describe the
evolution of the universe and the gravitational scalar $\phi$ is ascribed to
play the role of inflaton. The theory is characterized by the specified
coupling function $\omega(\phi)$ and the cosmological function $\lambda(\phi)$.
The function $\lambda(\phi)$ is nearly constant for $0<\phi<0.1$ and
$\lambda(1)=0$. The functions $\lambda(\phi)$ and $\omega(\phi)$ provide a
double-well potential for the motion of $\phi(t)$. Inflation commences and ends
naturally by the dynamics of the scalar field. The energy density of matter
increases steadily during inflation. When the constant $\Gamma$ in the action
is determined by the present matter density, the temperature at the end of
inflation is of the order of $10^{14} GeV$ in no need of reheating.
Furthermore, the gravitational scalar is just the cold dark matter that men
seek for.
| [
{
"created": "Fri, 10 Dec 1999 08:09:30 GMT",
"version": "v1"
},
{
"created": "Fri, 3 Mar 2000 14:09:08 GMT",
"version": "v2"
}
] | 2009-10-31 | [
[
"Wang",
"Mian",
""
]
] | In this paper the scalar-tensor theory of gravity is assumed to describe the evolution of the universe and the gravitational scalar $\phi$ is ascribed to play the role of inflaton. The theory is characterized by the specified coupling function $\omega(\phi)$ and the cosmological function $\lambda(\phi)$. The function $\lambda(\phi)$ is nearly constant for $0<\phi<0.1$ and $\lambda(1)=0$. The functions $\lambda(\phi)$ and $\omega(\phi)$ provide a double-well potential for the motion of $\phi(t)$. Inflation commences and ends naturally by the dynamics of the scalar field. The energy density of matter increases steadily during inflation. When the constant $\Gamma$ in the action is determined by the present matter density, the temperature at the end of inflation is of the order of $10^{14} GeV$ in no need of reheating. Furthermore, the gravitational scalar is just the cold dark matter that men seek for. |
gr-qc/0202002 | Gil de Oliveira-Neto | G. Oliveira-Neto | Naked singularities in three-dimensions | Revtex version, 11 pages and 1 eps figure | Int.J.Mod.Phys.D12:791-800,2003 | 10.1142/S0218271803003335 | null | gr-qc | null | We study an analytical solution to the Einstein's equations in
2+1-dimensions, representing the self-similar collapse of a circularly
symmetric, minimally coupled, massless, scalar field. Depending on the value of
certain parameters, this solution represents the formation of naked
singularities. Since our solution is asymptotically flat, these naked
singularities may be relevant for the weak cosmic censorship conjecture in
2+1-dimensions.
| [
{
"created": "Fri, 1 Feb 2002 17:57:19 GMT",
"version": "v1"
}
] | 2014-11-17 | [
[
"Oliveira-Neto",
"G.",
""
]
] | We study an analytical solution to the Einstein's equations in 2+1-dimensions, representing the self-similar collapse of a circularly symmetric, minimally coupled, massless, scalar field. Depending on the value of certain parameters, this solution represents the formation of naked singularities. Since our solution is asymptotically flat, these naked singularities may be relevant for the weak cosmic censorship conjecture in 2+1-dimensions. |
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