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 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
2401.11416 | Shuo Sun | Shuo Sun, Changfu Shi, Jian-dong Zhang, Jianwei Mei | Bayesian analysis of gravitational wave memory effect with TianQin | null | null | null | null | gr-qc astro-ph.IM | http://creativecommons.org/licenses/by/4.0/ | The memory effect in gravitational waves is a direct prediction of general
relativity. The presence of the memory effect in gravitational wave signals not
only serves as a test for general relativity but also establishes connections
between soft theorem, and asymptotic symmetries, serving as a bridge for
exploring fundamental physics. Furthermore, with the ongoing progress in
space-based gravitational wave detection projects, the gravitational wave
memory effect generated by the merger of massive binary black hole binaries is
becoming increasingly significant and cannot be ignored. In this work, we
perform the full Bayesian analysis of the gravitational wave memory effect with
TianQin. The results indicate that the memory effect has a certain impact on
parameter estimation but does not deviate beyond the 1$\sigma$ range.
Additionally, the Bayes factor analysis suggests that when the signal-to-noise
ratio of the memory effect in TianQin is approximately 2.36, the
$\text{log}_{10}$ Bayes factor reaches 8. This result is consistent with the
findings obtained from a previous mismatch threshold.
| [
{
"created": "Sun, 21 Jan 2024 07:10:33 GMT",
"version": "v1"
}
] | 2024-01-23 | [
[
"Sun",
"Shuo",
""
],
[
"Shi",
"Changfu",
""
],
[
"Zhang",
"Jian-dong",
""
],
[
"Mei",
"Jianwei",
""
]
] | The memory effect in gravitational waves is a direct prediction of general relativity. The presence of the memory effect in gravitational wave signals not only serves as a test for general relativity but also establishes connections between soft theorem, and asymptotic symmetries, serving as a bridge for exploring fundamental physics. Furthermore, with the ongoing progress in space-based gravitational wave detection projects, the gravitational wave memory effect generated by the merger of massive binary black hole binaries is becoming increasingly significant and cannot be ignored. In this work, we perform the full Bayesian analysis of the gravitational wave memory effect with TianQin. The results indicate that the memory effect has a certain impact on parameter estimation but does not deviate beyond the 1$\sigma$ range. Additionally, the Bayes factor analysis suggests that when the signal-to-noise ratio of the memory effect in TianQin is approximately 2.36, the $\text{log}_{10}$ Bayes factor reaches 8. This result is consistent with the findings obtained from a previous mismatch threshold. |
0901.3829 | Babak Vakili | H.R. Sepangi, B. Shakerin and B. Vakili | Deformed phase space in a two dimensional minisuperspace model | 20 pages, 7 figures + 4 contourplots, to appear in CQG | Class.Quant.Grav.26:065003,2009 | 10.1088/0264-9381/26/6/065003 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the effects of noncommutativity and deformed Heisenberg algebra on
the evolution of a two dimensional minisuperspace cosmological model in
classical and quantum regimes. The phase space variables turn out to correspond
to the scale factor of a flat FRW model with a positive cosmological constant
and a dilatonic field with which the action of the model is augmented. The
exact classical and quantum solutions in commutative and noncommutative cases
are presented. We also obtain some approximate analytical solutions for the
corresponding classical and quantum cosmology in the presence of the deformed
Heisenberg relations between the phase space variables, in the limit where the
minisuperspace variables are small. These results are compared with the
standard commutative and noncommutative cases and similarities and differences
of these solutions are discussed.
| [
{
"created": "Sat, 24 Jan 2009 12:31:37 GMT",
"version": "v1"
}
] | 2009-04-08 | [
[
"Sepangi",
"H. R.",
""
],
[
"Shakerin",
"B.",
""
],
[
"Vakili",
"B.",
""
]
] | We study the effects of noncommutativity and deformed Heisenberg algebra on the evolution of a two dimensional minisuperspace cosmological model in classical and quantum regimes. The phase space variables turn out to correspond to the scale factor of a flat FRW model with a positive cosmological constant and a dilatonic field with which the action of the model is augmented. The exact classical and quantum solutions in commutative and noncommutative cases are presented. We also obtain some approximate analytical solutions for the corresponding classical and quantum cosmology in the presence of the deformed Heisenberg relations between the phase space variables, in the limit where the minisuperspace variables are small. These results are compared with the standard commutative and noncommutative cases and similarities and differences of these solutions are discussed. |
gr-qc/0304103 | Grigori Volovik | G.E. Volovik | Vacuum energy and Universe in special relativity | LaTeX file, 7 pages, no figures, to appear in JETP Letters, reference
is added | JETP Lett. 77 (2003) 639-641; Pisma Zh.Eksp.Teor.Fiz. 77 (2003)
769-771 | 10.1134/1.1604411 | null | gr-qc cond-mat hep-ph | null | The problem of cosmological constant and vacuum energy is usually thought of
as the subject of general relativity. However, the vacuum energy is important
for the Universe even in the absence of gravity, i.e. in the case when the
Newton constant G is exactly zero, G=0. We discuss the response of the vacuum
energy to the perturbations of the quantum vacuum in special relativity, and
find that as in general relativity the vacuum energy density is on the order of
the energy density of matter. In general relativity, the dependence of the
vacuum energy on the equation of state of matter does not contain G, and thus
is valid in the limit when G tends to zero. However, the result obtained for
the vacuum energy in the world without gravity, i.e. when G=0 exactly, is
different.
| [
{
"created": "Tue, 29 Apr 2003 15:18:09 GMT",
"version": "v1"
},
{
"created": "Wed, 21 May 2003 12:39:17 GMT",
"version": "v2"
},
{
"created": "Mon, 9 Jun 2003 11:41:17 GMT",
"version": "v3"
}
] | 2009-11-10 | [
[
"Volovik",
"G. E.",
""
]
] | The problem of cosmological constant and vacuum energy is usually thought of as the subject of general relativity. However, the vacuum energy is important for the Universe even in the absence of gravity, i.e. in the case when the Newton constant G is exactly zero, G=0. We discuss the response of the vacuum energy to the perturbations of the quantum vacuum in special relativity, and find that as in general relativity the vacuum energy density is on the order of the energy density of matter. In general relativity, the dependence of the vacuum energy on the equation of state of matter does not contain G, and thus is valid in the limit when G tends to zero. However, the result obtained for the vacuum energy in the world without gravity, i.e. when G=0 exactly, is different. |
2008.01426 | Naveena Kumara A | C.L. Ahmed Rizwan, A. Naveena Kumara, Kartheek Hegde, Md Sabir Ali,
Ajith K.M | Rotating Black Hole with an Anisotropic Matter Field as a Particle
Accelerator | 22 pages, 7 figures | Classical and Quantum Gravity, 2021 | 10.1088/1361-6382/abe2d9 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Recently, a generalised solution for Einstein equations of a rotating compact
body, surrounded by matter field was proposed, which is the Kerr-Newman
spacetime with an anisotropic matter. The solution possesses an additional
hair, along with the conventional mass, charge and spin, which arises from the
negative radial pressure of the anisotropic matter. In this article we show
that, this new class of black holes can act as a particle accelerator during
the collision of two generic particles in its gravitational field in the
ergo-region. The centre of mass energy of the particles shoots to arbitrary
high value in the vicinity of event horizon for the extremal black hole. The
physical conditions for the collision to take place are obtained by studying
the horizon structure and circular particle motion. The results are interesting
from astrophysical perspective.
| [
{
"created": "Tue, 4 Aug 2020 09:16:42 GMT",
"version": "v1"
}
] | 2021-03-12 | [
[
"Rizwan",
"C. L. Ahmed",
""
],
[
"Kumara",
"A. Naveena",
""
],
[
"Hegde",
"Kartheek",
""
],
[
"Ali",
"Md Sabir",
""
],
[
"M",
"Ajith K.",
""
]
] | Recently, a generalised solution for Einstein equations of a rotating compact body, surrounded by matter field was proposed, which is the Kerr-Newman spacetime with an anisotropic matter. The solution possesses an additional hair, along with the conventional mass, charge and spin, which arises from the negative radial pressure of the anisotropic matter. In this article we show that, this new class of black holes can act as a particle accelerator during the collision of two generic particles in its gravitational field in the ergo-region. The centre of mass energy of the particles shoots to arbitrary high value in the vicinity of event horizon for the extremal black hole. The physical conditions for the collision to take place are obtained by studying the horizon structure and circular particle motion. The results are interesting from astrophysical perspective. |
gr-qc/0003060 | Jong Hyuk Yoon | J.H. Yoon (Department of Physics, Konkuk University, Seoul, Korea) | (2,2)-Formalism of General Relativity: An Exact Solution | 2 figures included, IOP style file needed | Class.Quant.Grav.16:1863-1871,1999 | 10.1088/0264-9381/16/6/319 | null | gr-qc | null | I discuss the (2,2)-formalism of general relativity based on the
(2,2)-fibration of a generic 4-dimensional spacetime of the Lorentzian
signature. In this formalism general relativity is describable as a Yang-Mills
gauge theory defined on the (1+1)-dimensional base manifold, whose local gauge
symmetry is the group of the diffeomorphisms of the 2-dimensional fibre
manifold. After presenting the Einstein's field equations in this formalism, I
solve them for spherically symmetric case to obtain the Schwarzschild solution.
Then I discuss possible applications of this formalism.
| [
{
"created": "Wed, 15 Mar 2000 08:52:50 GMT",
"version": "v1"
}
] | 2010-11-19 | [
[
"Yoon",
"J. H.",
"",
"Department of Physics, Konkuk University, Seoul, Korea"
]
] | I discuss the (2,2)-formalism of general relativity based on the (2,2)-fibration of a generic 4-dimensional spacetime of the Lorentzian signature. In this formalism general relativity is describable as a Yang-Mills gauge theory defined on the (1+1)-dimensional base manifold, whose local gauge symmetry is the group of the diffeomorphisms of the 2-dimensional fibre manifold. After presenting the Einstein's field equations in this formalism, I solve them for spherically symmetric case to obtain the Schwarzschild solution. Then I discuss possible applications of this formalism. |
gr-qc/9806068 | Jonathan Wilson | J. A. Vickers, J. P. Wilson | Invariance of the distributional curvature of the cone under smooth
diffeomorphisms | 8 pages, AMS-TeX | Class.Quant.Grav. 16 (1999) 579-588 | 10.1088/0264-9381/16/2/019 | null | gr-qc | null | An explicit calculation is carried out to show that the distributional
curvature of a 2-cone, calculated by Clarke et al. (1996), using Colombeau's
new generalised functions is invariant under non-linear $C^\infty$ coordinate
transformations.
| [
{
"created": "Tue, 16 Jun 1998 09:27:07 GMT",
"version": "v1"
}
] | 2009-10-31 | [
[
"Vickers",
"J. A.",
""
],
[
"Wilson",
"J. P.",
""
]
] | An explicit calculation is carried out to show that the distributional curvature of a 2-cone, calculated by Clarke et al. (1996), using Colombeau's new generalised functions is invariant under non-linear $C^\infty$ coordinate transformations. |
gr-qc/0508039 | Alan Coley | B. J. Carr and A. A. Coley | The Similarity Hypothesis in General Relativity | to be submitted to Gen. Rel. Grav | Gen.Rel.Grav.37:2165-2188,2005 | 10.1007/s10714-005-0196-7 | null | gr-qc astro-ph | null | Self-similar models are important in general relativity and other fundamental
theories. In this paper we shall discuss the ``similarity hypothesis'', which
asserts that under a variety of physical circumstances solutions of these
theories will naturally evolve to a self-similar form. We will find there is
good evidence for this in the context of both spatially homogenous and
inhomogeneous cosmological models, although in some cases the self-similar
model is only an intermediate attractor. There are also a wide variety of
situations, including critical pheneomena, in which spherically symmetric
models tend towards self-similarity. However, this does not happen in all cases
and it is it is important to understand the prerequisites for the conjecture.
| [
{
"created": "Wed, 10 Aug 2005 14:00:34 GMT",
"version": "v1"
},
{
"created": "Sat, 3 Dec 2005 18:43:03 GMT",
"version": "v2"
}
] | 2009-11-11 | [
[
"Carr",
"B. J.",
""
],
[
"Coley",
"A. A.",
""
]
] | Self-similar models are important in general relativity and other fundamental theories. In this paper we shall discuss the ``similarity hypothesis'', which asserts that under a variety of physical circumstances solutions of these theories will naturally evolve to a self-similar form. We will find there is good evidence for this in the context of both spatially homogenous and inhomogeneous cosmological models, although in some cases the self-similar model is only an intermediate attractor. There are also a wide variety of situations, including critical pheneomena, in which spherically symmetric models tend towards self-similarity. However, this does not happen in all cases and it is it is important to understand the prerequisites for the conjecture. |
1801.07306 | Maulik K. Parikh | Maulik Parikh, Sudipta Sarkar, and Andrew Svesko | A Local First Law of Gravity | 6 pages, 1 figure, LaTeX | Phys. Rev. D 101, 104043 (2020) | 10.1103/PhysRevD.101.104043 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We find a (quasi-)local first law of thermodynamics, $\Delta E = T \Delta S -
W$, connecting gravitational entropy, $S$, with matter energy and work. For
Einstein gravity $S$ is the Bekenstein-Hawking entropy, while for general
theories of gravity $S$ is the Wald entropy, evaluated on the stretched future
light cone of any point in an arbitrary spacetime, not necessarily containing a
black hole. The equation can be written as $\rho \Delta V = T \Delta S - p
\Delta V$ by regarding the energy-momentum tensor as that of a fluid.
| [
{
"created": "Mon, 22 Jan 2018 20:24:50 GMT",
"version": "v1"
},
{
"created": "Fri, 13 Nov 2020 06:21:18 GMT",
"version": "v2"
}
] | 2020-11-16 | [
[
"Parikh",
"Maulik",
""
],
[
"Sarkar",
"Sudipta",
""
],
[
"Svesko",
"Andrew",
""
]
] | We find a (quasi-)local first law of thermodynamics, $\Delta E = T \Delta S - W$, connecting gravitational entropy, $S$, with matter energy and work. For Einstein gravity $S$ is the Bekenstein-Hawking entropy, while for general theories of gravity $S$ is the Wald entropy, evaluated on the stretched future light cone of any point in an arbitrary spacetime, not necessarily containing a black hole. The equation can be written as $\rho \Delta V = T \Delta S - p \Delta V$ by regarding the energy-momentum tensor as that of a fluid. |
2202.00010 | Kimet Jusufi | Kimet Jusufi | Black holes surrounded by Einstein clusters as models of dark matter
fluid | 11 pages, 6 figures. Accepted for publication in EPJC | Eur. Phys. J. C 83, 103 (2023) | 10.1140/epjc/s10052-023-11264-w | null | gr-qc astro-ph.GA astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We construct a novel class of spherically symmetric and asymptotically flat
black holes and naked singularities surrounded by anisotropic dark matter fluid
with the equation of state (EoS) of the form $P_t=\omega \rho$. We assume that
dark matter is made of weakly interacting particles orbiting around the
supermassive black hole in the galactic center and the dark matter halo is
formed by means of Einstein clusters having only tangential pressure. In the
large distance from the black hole, we obtain the constant flat curve with the
upper bound for the dark matter state parameter $\omega \lesssim 10^{-7}$. To
this end, we also check the energy conditions of the dark matter fluid outside
the black hole/naked singularity, the deflection of light by the galaxy, and
the shadow images of the Sgr A$^\star$ black hole using the rotating and
radiating particles. For the black hole case, we find that the effect of dark
matter fluid on the shadow radius is small, in particular the angular radius of
the black hole is shown to increase by the order $10^{-4} \mu$arcsec compared
to the vacuum solution. For the naked singularity we obtain significantly
smaller shadow radius compared to the black hole case. Finally, we study the
stability of the S2 star orbit around Sgr A$^\star$ black hole under dark
matter effects. It is argued that the motion of S2 star orbit is stable for
values $\omega \lesssim 10^{-7}$, however further increase of $\omega $ leads
to unstable orbits. Using the observational result for the shadow images of the
Sgr A$^\star$ reported by the EHT along with the tightest constraint for
$\omega$ found from the constant flat curve, we show that the black hole model
is consistent with the data while the naked singularity in our model can be
ruled out.
| [
{
"created": "Mon, 31 Jan 2022 15:48:23 GMT",
"version": "v1"
},
{
"created": "Fri, 4 Feb 2022 12:56:14 GMT",
"version": "v2"
},
{
"created": "Sun, 22 Jan 2023 13:05:55 GMT",
"version": "v3"
}
] | 2023-02-02 | [
[
"Jusufi",
"Kimet",
""
]
] | We construct a novel class of spherically symmetric and asymptotically flat black holes and naked singularities surrounded by anisotropic dark matter fluid with the equation of state (EoS) of the form $P_t=\omega \rho$. We assume that dark matter is made of weakly interacting particles orbiting around the supermassive black hole in the galactic center and the dark matter halo is formed by means of Einstein clusters having only tangential pressure. In the large distance from the black hole, we obtain the constant flat curve with the upper bound for the dark matter state parameter $\omega \lesssim 10^{-7}$. To this end, we also check the energy conditions of the dark matter fluid outside the black hole/naked singularity, the deflection of light by the galaxy, and the shadow images of the Sgr A$^\star$ black hole using the rotating and radiating particles. For the black hole case, we find that the effect of dark matter fluid on the shadow radius is small, in particular the angular radius of the black hole is shown to increase by the order $10^{-4} \mu$arcsec compared to the vacuum solution. For the naked singularity we obtain significantly smaller shadow radius compared to the black hole case. Finally, we study the stability of the S2 star orbit around Sgr A$^\star$ black hole under dark matter effects. It is argued that the motion of S2 star orbit is stable for values $\omega \lesssim 10^{-7}$, however further increase of $\omega $ leads to unstable orbits. Using the observational result for the shadow images of the Sgr A$^\star$ reported by the EHT along with the tightest constraint for $\omega$ found from the constant flat curve, we show that the black hole model is consistent with the data while the naked singularity in our model can be ruled out. |
gr-qc/0204069 | Bei-Lok Hu | B. L. Hu | A Kinetic Theory Approach to Quantum Gravity | Latex 19 pages. Invited talk given at the 6th Peyresq Meeting,
France, June, 2001. To appear in Int. J. Theor. Phys. 2002 | Int.J.Theor.Phys.41:2091-2119,2002 | 10.1023/A:1021124824987 | umdpp 02-039 | gr-qc | null | We describe a kinetic theory approach to quantum gravity -- by which we mean
a theory of the microscopic structure of spacetime, not a theory obtained by
quantizing general relativity. A figurative conception of this program is like
building a ladder with two knotted poles: quantum matter field on the right and
spacetime on the left. Each rung connecting the corresponding knots represent a
distinct level of structure. The lowest rung is hydrodynamics and general
relativity; the next rung is semiclassical gravity, with the expectation value
of quantum fields acting as source in the semiclassical Einstein equation. We
recall how ideas from the statistical mechanics of interacting quantum fields
helped us identify the existence of noise in the matter field and its effect on
metric fluctuations, leading to the establishment of the third rung: stochastic
gravity, described by the Einstein-Langevin equation. Our pathway from
stochastic to quantum gravity is via the correlation hierarchy of noise and
induced metric fluctuations. Three essential tasks beckon: 1) Deduce the
correlations of metric fluctuations from correlation noise in the matter field;
2) Reconstituting quantum coherence -- this is the reverse of decoherence --
from these correlation functions 3) Use the Boltzmann-Langevin equations to
identify distinct collective variables depicting recognizable metastable
structures in the kinetic and hydrodynamic regimes of quantum matter fields and
how they demand of their corresponding spacetime counterparts. This will give
us a hierarchy of generalized stochastic equations -- call them the
Boltzmann-Einstein hierarchy of quantum gravity -- for each level of spacetime
structure, from the macroscopic (general relativity) through the mesoscopic
(stochastic gravity) to the microscopic (quantum gravity).
| [
{
"created": "Mon, 22 Apr 2002 01:50:35 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Hu",
"B. L.",
""
]
] | We describe a kinetic theory approach to quantum gravity -- by which we mean a theory of the microscopic structure of spacetime, not a theory obtained by quantizing general relativity. A figurative conception of this program is like building a ladder with two knotted poles: quantum matter field on the right and spacetime on the left. Each rung connecting the corresponding knots represent a distinct level of structure. The lowest rung is hydrodynamics and general relativity; the next rung is semiclassical gravity, with the expectation value of quantum fields acting as source in the semiclassical Einstein equation. We recall how ideas from the statistical mechanics of interacting quantum fields helped us identify the existence of noise in the matter field and its effect on metric fluctuations, leading to the establishment of the third rung: stochastic gravity, described by the Einstein-Langevin equation. Our pathway from stochastic to quantum gravity is via the correlation hierarchy of noise and induced metric fluctuations. Three essential tasks beckon: 1) Deduce the correlations of metric fluctuations from correlation noise in the matter field; 2) Reconstituting quantum coherence -- this is the reverse of decoherence -- from these correlation functions 3) Use the Boltzmann-Langevin equations to identify distinct collective variables depicting recognizable metastable structures in the kinetic and hydrodynamic regimes of quantum matter fields and how they demand of their corresponding spacetime counterparts. This will give us a hierarchy of generalized stochastic equations -- call them the Boltzmann-Einstein hierarchy of quantum gravity -- for each level of spacetime structure, from the macroscopic (general relativity) through the mesoscopic (stochastic gravity) to the microscopic (quantum gravity). |
gr-qc/0206054 | Martin Bojowald | Martin Bojowald | Inflation from Quantum Geometry | 4 pages, 3 figures | Phys.Rev.Lett.89:261301,2002 | 10.1103/PhysRevLett.89.261301 | CGPG-02/6-2 | gr-qc astro-ph hep-th | null | Quantum geometry predicts that a universe evolves through an inflationary
phase at small volume before exiting gracefully into a standard Friedmann
phase. This does not require the introduction of additional matter fields with
ad hoc potentials; rather, it occurs because of a quantum gravity modification
of the kinetic part of ordinary matter Hamiltonians. An application of the same
mechanism can explain why the present-day cosmological acceleration is so tiny.
| [
{
"created": "Tue, 18 Jun 2002 14:30:32 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Bojowald",
"Martin",
""
]
] | Quantum geometry predicts that a universe evolves through an inflationary phase at small volume before exiting gracefully into a standard Friedmann phase. This does not require the introduction of additional matter fields with ad hoc potentials; rather, it occurs because of a quantum gravity modification of the kinetic part of ordinary matter Hamiltonians. An application of the same mechanism can explain why the present-day cosmological acceleration is so tiny. |
2212.13438 | Zheng-Wen Long | Shurui Wu, Bing-Qian Wang, Z. W. Long, Hao Chen | Validity of black hole complementarity in the context of generalized
uncertainty principle | arXiv admin note: text overlap with arXiv:1712.04444 by other authors | null | null | null | gr-qc quant-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Recently, Elias C. Vagenas et al and Yongwan Gim et al studied the validity
of the no-cloning theorem in the context of generalized uncertainty principle
(GUP), but they came to conflicting conclusions. With this in mind, we
investigate the corrections to the temperature for Schwarzschild black hole in
the context of different forms of GUP, and obtain the required energy to
duplicate information for the Schwarzschild black hole, it shows that the
required energy is greater than the mass of black hole, i.e. the no-cloning
theorem in the present of GUP is safe.
| [
{
"created": "Tue, 27 Dec 2022 10:26:35 GMT",
"version": "v1"
},
{
"created": "Fri, 28 Apr 2023 06:36:07 GMT",
"version": "v2"
}
] | 2023-05-01 | [
[
"Wu",
"Shurui",
""
],
[
"Wang",
"Bing-Qian",
""
],
[
"Long",
"Z. W.",
""
],
[
"Chen",
"Hao",
""
]
] | Recently, Elias C. Vagenas et al and Yongwan Gim et al studied the validity of the no-cloning theorem in the context of generalized uncertainty principle (GUP), but they came to conflicting conclusions. With this in mind, we investigate the corrections to the temperature for Schwarzschild black hole in the context of different forms of GUP, and obtain the required energy to duplicate information for the Schwarzschild black hole, it shows that the required energy is greater than the mass of black hole, i.e. the no-cloning theorem in the present of GUP is safe. |
1801.03840 | Florent Michel | Florent Michel, Renaud Parentani, Scott Robertson | Gravity waves on modulated flows downstream from an obstacle: The
transcritical case | 34 pages, 11 figures, version 2 close to that published in Physical
Review D | Phys. Rev. D 97, 065018 (2018) | 10.1103/PhysRevD.97.065018 | null | gr-qc physics.flu-dyn | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Periodic spatial variations of some parameter arise in analogue gravity
experiments aimed at detecting the analogue version of the Hawking effect in a
white hole flow. Having the same spatial periodicity as low-frequency
dispersive modes, they can induce resonances which significantly modify the
scattering coefficients. This has been shown numerically in a previous work [X.
Busch et al., Phys. Rev. D 90, 105005 (2014)], but the precise dependence of
the low-frequency effective temperature on the amplitude and length of the
undulation remains elusive. In this article, using the Korteweg-de Vries
equation, we explicitly compute this dependence in the small-amplitude limit
and find three regimes of "short", "intermediate" and "long" undulations
showing different scaling laws. In the latter, the effective temperature is
completely determined by the properties of the undulation, independently of the
surface gravity of the analogue white hole flow. These results are extended to
a more realistic hydrodynamical model in an appendix.
| [
{
"created": "Thu, 11 Jan 2018 16:02:54 GMT",
"version": "v1"
},
{
"created": "Fri, 20 Apr 2018 12:07:28 GMT",
"version": "v2"
}
] | 2018-04-23 | [
[
"Michel",
"Florent",
""
],
[
"Parentani",
"Renaud",
""
],
[
"Robertson",
"Scott",
""
]
] | Periodic spatial variations of some parameter arise in analogue gravity experiments aimed at detecting the analogue version of the Hawking effect in a white hole flow. Having the same spatial periodicity as low-frequency dispersive modes, they can induce resonances which significantly modify the scattering coefficients. This has been shown numerically in a previous work [X. Busch et al., Phys. Rev. D 90, 105005 (2014)], but the precise dependence of the low-frequency effective temperature on the amplitude and length of the undulation remains elusive. In this article, using the Korteweg-de Vries equation, we explicitly compute this dependence in the small-amplitude limit and find three regimes of "short", "intermediate" and "long" undulations showing different scaling laws. In the latter, the effective temperature is completely determined by the properties of the undulation, independently of the surface gravity of the analogue white hole flow. These results are extended to a more realistic hydrodynamical model in an appendix. |
2103.12037 | Giulia Capurri | Giulia Capurri, Andrea Lapi, Carlo Baccigalupi, Lumen Boco, Giulio
Scelfo, Tommaso Ronconi | Intensity and anisotropies of the stochastic Gravitational Wave
background from merging compact binaries in galaxies | 35 pages, 12 figures | null | 10.1088/1475-7516/2021/11/032 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We investigate the isotropic and anisotropic components of the Stochastic
Gravitational Wave Background (SGWB) originated from unresolved merging compact
binaries in galaxies. We base our analysis on an empirical approach to galactic
astrophysics that allows to follow the evolution of individual systems. We then
characterize the energy density of the SGWB as a tracer of the total matter
density, in order to compute the angular power spectrum of anisotropies with
the Cosmic Linear Anisotropy Solving System (CLASS) public code in full
generality. We obtain predictions for the isotropic energy density and for the
angular power spectrum of the SGWB anisotropies, and study the prospect for
their observations with advanced Laser Interferometer Gravitational-Wave and
Virgo Observatories and with the Einstein Telescope. We identify the
contributions coming from different type of sources (binary black holes, binary
neutron stars and black hole-neutron star) and from different redshifts. We
examine in detail the spectral shape of the energy density for all types of
sources, comparing the results for the two detectors. We find that the power
spectrum of the SGWB anisotropies behaves like a power law on large angular
scales and drops at small scales: we explain this behaviour in terms of the
redshift distribution of sources that contribute most to the signal, and of the
sensitivities of the two detectors. Finally, we simulate a high resolution full
sky map of the SGWB starting from the power spectra obtained with CLASS and
including Poisson statistics and clustering properties.
| [
{
"created": "Mon, 22 Mar 2021 17:38:47 GMT",
"version": "v1"
},
{
"created": "Fri, 1 Oct 2021 10:19:21 GMT",
"version": "v2"
}
] | 2021-11-16 | [
[
"Capurri",
"Giulia",
""
],
[
"Lapi",
"Andrea",
""
],
[
"Baccigalupi",
"Carlo",
""
],
[
"Boco",
"Lumen",
""
],
[
"Scelfo",
"Giulio",
""
],
[
"Ronconi",
"Tommaso",
""
]
] | We investigate the isotropic and anisotropic components of the Stochastic Gravitational Wave Background (SGWB) originated from unresolved merging compact binaries in galaxies. We base our analysis on an empirical approach to galactic astrophysics that allows to follow the evolution of individual systems. We then characterize the energy density of the SGWB as a tracer of the total matter density, in order to compute the angular power spectrum of anisotropies with the Cosmic Linear Anisotropy Solving System (CLASS) public code in full generality. We obtain predictions for the isotropic energy density and for the angular power spectrum of the SGWB anisotropies, and study the prospect for their observations with advanced Laser Interferometer Gravitational-Wave and Virgo Observatories and with the Einstein Telescope. We identify the contributions coming from different type of sources (binary black holes, binary neutron stars and black hole-neutron star) and from different redshifts. We examine in detail the spectral shape of the energy density for all types of sources, comparing the results for the two detectors. We find that the power spectrum of the SGWB anisotropies behaves like a power law on large angular scales and drops at small scales: we explain this behaviour in terms of the redshift distribution of sources that contribute most to the signal, and of the sensitivities of the two detectors. Finally, we simulate a high resolution full sky map of the SGWB starting from the power spectra obtained with CLASS and including Poisson statistics and clustering properties. |
2110.13141 | Eleonora Giovannetti | Eleonora Giovannetti, Giovanni Montani, Silvia Schiattarella | On the semiclassical and quantum picture of the Bianchi I polymer
dynamics | arXiv admin note: substantial text overlap with arXiv:2105.00360 | null | null | To appear in the Proceedings of the 16th Marcel Grossmann meeting
(5-10 July, 2021) | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We analyze the Bianchi I cosmology in the presence of a massless scalar field
and describe its dynamics via a semiclassical and quantum polymer approach. We
investigate the morphology of the emerging Big Bounce by adopting three
different sets of configurational variables: the natural Ashtekar connections,
the Universe volume plus two anisotropy coordinates and a set of anisotropic
volume-like coordinates (the latter two sets of variables would coincide in the
case of an isotropic Universe). In the semiclassical analysis we demonstrate
that the Big Bounce emerges in the dynamics for all the three sets of
variables. Moreover, when the Universe volume itself is considered as a
configurational variable, we have derived the polymer-modified Friedmann
equation and demonstrated that the Big Bounce has a universal nature, i.e. the
total critical energy density has a maximum value fixed by fundamental
constants and the Immirzi parameter only. From a pure quantum point of view, we
investigate the Bianchi I dynamics only in terms of the Ashtekar connections.
In particular, we apply the Arnowitt-Deser-Misner (ADM) reduction of the
variational principle and then we quantize the system. We study the resulting
Schr\"{o}dinger dynamics, stressing that the wave packet peak behavior over
time singles out common features with the semiclassical trajectories.
| [
{
"created": "Sun, 24 Oct 2021 14:14:35 GMT",
"version": "v1"
}
] | 2022-03-10 | [
[
"Giovannetti",
"Eleonora",
""
],
[
"Montani",
"Giovanni",
""
],
[
"Schiattarella",
"Silvia",
""
]
] | We analyze the Bianchi I cosmology in the presence of a massless scalar field and describe its dynamics via a semiclassical and quantum polymer approach. We investigate the morphology of the emerging Big Bounce by adopting three different sets of configurational variables: the natural Ashtekar connections, the Universe volume plus two anisotropy coordinates and a set of anisotropic volume-like coordinates (the latter two sets of variables would coincide in the case of an isotropic Universe). In the semiclassical analysis we demonstrate that the Big Bounce emerges in the dynamics for all the three sets of variables. Moreover, when the Universe volume itself is considered as a configurational variable, we have derived the polymer-modified Friedmann equation and demonstrated that the Big Bounce has a universal nature, i.e. the total critical energy density has a maximum value fixed by fundamental constants and the Immirzi parameter only. From a pure quantum point of view, we investigate the Bianchi I dynamics only in terms of the Ashtekar connections. In particular, we apply the Arnowitt-Deser-Misner (ADM) reduction of the variational principle and then we quantize the system. We study the resulting Schr\"{o}dinger dynamics, stressing that the wave packet peak behavior over time singles out common features with the semiclassical trajectories. |
1309.1119 | Henrique de Andrade Gomes | Henrique Gomes | A first look at Weyl anomalies in shape dynamics | 13 pages. v2 Change of phrasing in the abstract to avoid semantic
ambiguity | J. Math Phys. Volume 54, Issue 11, Nov 2013, 112302 | 10.1063/1.4832396 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | One of the more popular objections towards shape dynamics is the suspicion
that anomalies in the spatial Weyl symmetry will arise upon quantization. The
purpose of this short paper is to establish the tools required for an
investigation of the sort of anomalies that can possibly arise. The first step
is to adapt to our setting Barnich and Henneaux's formulation of gauge
cohomology in the Hamiltonian setting, which serve to decompose the anomaly
into a spatial component and time component. The spatial part of the anomaly,
i.e. the anomaly in the symmetry algebra itself ($[\Omega, \Omega]\propto
\hbar$ instead of vanishing) is given by a projection of the second ghost
cohomology of the Hamiltonian BRST differential associated to $\Omega$, modulo
spatial derivatives. The temporal part, $[\Omega, H]\propto\hbar$ is given by a
different projection of the first ghost cohomology and an extra piece arising
from a solution to a functional differential equation. Assuming locality of the
gauge cohomology groups involved, this part is always local. Assuming locality
for the gauge cohomology groups, using Barnich and Henneaux's results, the
classification of Weyl cohomology for higher ghost numbers performed by
Boulanger, and following the descent equations, we find a complete
characterizations of anomalies in 3+1 dimensions. The spatial part of the
anomaly and the first component of the temporal anomaly are always local given
these assumptions even in shape dynamics. The part emerging from the solution
of the functional differential equations explicitly involves the shape dynamics
Hamiltonian, and thus might be non-local. If one restricts this extra piece of
the temporal anomaly to be also local, then overall no \emph{local} Weyl
anomalies, either temporal or spatial, emerge in the 3+1 case.
| [
{
"created": "Wed, 4 Sep 2013 17:57:16 GMT",
"version": "v1"
},
{
"created": "Thu, 5 Sep 2013 17:12:19 GMT",
"version": "v2"
}
] | 2013-11-28 | [
[
"Gomes",
"Henrique",
""
]
] | One of the more popular objections towards shape dynamics is the suspicion that anomalies in the spatial Weyl symmetry will arise upon quantization. The purpose of this short paper is to establish the tools required for an investigation of the sort of anomalies that can possibly arise. The first step is to adapt to our setting Barnich and Henneaux's formulation of gauge cohomology in the Hamiltonian setting, which serve to decompose the anomaly into a spatial component and time component. The spatial part of the anomaly, i.e. the anomaly in the symmetry algebra itself ($[\Omega, \Omega]\propto \hbar$ instead of vanishing) is given by a projection of the second ghost cohomology of the Hamiltonian BRST differential associated to $\Omega$, modulo spatial derivatives. The temporal part, $[\Omega, H]\propto\hbar$ is given by a different projection of the first ghost cohomology and an extra piece arising from a solution to a functional differential equation. Assuming locality of the gauge cohomology groups involved, this part is always local. Assuming locality for the gauge cohomology groups, using Barnich and Henneaux's results, the classification of Weyl cohomology for higher ghost numbers performed by Boulanger, and following the descent equations, we find a complete characterizations of anomalies in 3+1 dimensions. The spatial part of the anomaly and the first component of the temporal anomaly are always local given these assumptions even in shape dynamics. The part emerging from the solution of the functional differential equations explicitly involves the shape dynamics Hamiltonian, and thus might be non-local. If one restricts this extra piece of the temporal anomaly to be also local, then overall no \emph{local} Weyl anomalies, either temporal or spatial, emerge in the 3+1 case. |
1004.4298 | Tomi Koivisto | Tomi S. Koivisto | Bouncing Palatini cosmologies and their perturbations | 7 pages, 1 figure. v2: added references. | Phys.Rev.D82:044022,2010 | 10.1103/PhysRevD.82.044022 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Nonsingular cosmologies are investigated in the framework of f(R) gravity
within the first order formalism. General conditions for bounces in isotropic
and homogeneous cosmology are presented. It is shown that only a quadratic
curvature correction is needed to predict a bounce in a flat or to describe
cyclic evolution in a curved dust-filled universe. Formalism for perturbations
in these models is set up. In the simplest cases, the perturbations diverge at
the turnover. Conditions to obtain smooth evolution are derived.
| [
{
"created": "Sat, 24 Apr 2010 18:00:27 GMT",
"version": "v1"
},
{
"created": "Thu, 29 Apr 2010 13:50:43 GMT",
"version": "v2"
}
] | 2014-11-20 | [
[
"Koivisto",
"Tomi S.",
""
]
] | Nonsingular cosmologies are investigated in the framework of f(R) gravity within the first order formalism. General conditions for bounces in isotropic and homogeneous cosmology are presented. It is shown that only a quadratic curvature correction is needed to predict a bounce in a flat or to describe cyclic evolution in a curved dust-filled universe. Formalism for perturbations in these models is set up. In the simplest cases, the perturbations diverge at the turnover. Conditions to obtain smooth evolution are derived. |
2105.10951 | Mengjie Wang | Mengjie Wang, Zhou Chen, Qiyuan Pan, Jiliang Jing | Maxwell quasinormal modes on a global monopole Schwarzschild-anti-de
Sitter black hole with Robin boundary conditions | 10 pages, 5 figures, to appear in EPJC | null | 10.1140/epjc/s10052-021-09149-x | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We generalize our previous studies on the Maxwell quasinormal modes around
Schwarzschild-anti-de-Sitter black holes with Robin type vanishing energy flux
boundary conditions, by adding a global monopole on the background. We first
formulate the Maxwell equations both in the Regge-Wheeler-Zerilli and in the
Teukolsky formalisms and derive, based on the vanishing energy flux principle,
two boundary conditions in each formalism. The Maxwell equations are then
solved analytically in pure anti-de Sitter spacetimes with a global monopole,
and two different normal modes are obtained due to the existence of the
monopole parameter. In the small black hole and low frequency approximations,
the Maxwell quasinormal modes are solved perturbatively on top of normal modes
by using an asymptotic matching method, while beyond the aforementioned
approximation, the Maxwell quasinormal modes are obtained numerically. We
analyze the Maxwell quasinormal spectrum by varying the angular momentum
quantum number $\ell$, the overtone number $N$, and in particular, the monopole
parameter $8\pi\eta^2$. We show explicitly, through calculating quasinormal
frequencies with both boundary conditions, that the global monopole produces
the repulsive force.
| [
{
"created": "Sun, 23 May 2021 14:52:09 GMT",
"version": "v1"
}
] | 2021-06-16 | [
[
"Wang",
"Mengjie",
""
],
[
"Chen",
"Zhou",
""
],
[
"Pan",
"Qiyuan",
""
],
[
"Jing",
"Jiliang",
""
]
] | We generalize our previous studies on the Maxwell quasinormal modes around Schwarzschild-anti-de-Sitter black holes with Robin type vanishing energy flux boundary conditions, by adding a global monopole on the background. We first formulate the Maxwell equations both in the Regge-Wheeler-Zerilli and in the Teukolsky formalisms and derive, based on the vanishing energy flux principle, two boundary conditions in each formalism. The Maxwell equations are then solved analytically in pure anti-de Sitter spacetimes with a global monopole, and two different normal modes are obtained due to the existence of the monopole parameter. In the small black hole and low frequency approximations, the Maxwell quasinormal modes are solved perturbatively on top of normal modes by using an asymptotic matching method, while beyond the aforementioned approximation, the Maxwell quasinormal modes are obtained numerically. We analyze the Maxwell quasinormal spectrum by varying the angular momentum quantum number $\ell$, the overtone number $N$, and in particular, the monopole parameter $8\pi\eta^2$. We show explicitly, through calculating quasinormal frequencies with both boundary conditions, that the global monopole produces the repulsive force. |
2111.09483 | Avik De Dr. | Tee-How Loo, Avik De, Sanjay Mandal and P.K. Sahoo | How a projectively flat geometry regulates $F(R)$-gravity theory? | 15 pages, 8 figures | Physica Scripta, 96(12) (2021) 125034 | 10.1088/1402-4896/ac3a51 | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | In the present paper we examine a projectively flat spacetime solution of
$F(R)$-gravity theory. It is seen that once we deploy projective flatness in
the geometry of the spacetime, the matter field has constant energy density and
isotropic pressure. We then make the condition weaker and discuss the effects
of projectively harmonic spacetime geometry in $F(R)$-gravity theory and show
that the spacetime in this case reduces to a generalised Robertson-Walker
spacetime with a shear, vorticity, acceleration free perfect fluid with a
specific form of expansion scalar presented in terms of the scale factor. Role
of conharmonic curvature tensor in the spacetime geometry is also briefly
discussed. Some analysis of the obtained results are conducted in terms of
couple of $F(R)$-gravity models.
| [
{
"created": "Thu, 18 Nov 2021 02:28:32 GMT",
"version": "v1"
}
] | 2021-12-07 | [
[
"Loo",
"Tee-How",
""
],
[
"De",
"Avik",
""
],
[
"Mandal",
"Sanjay",
""
],
[
"Sahoo",
"P. K.",
""
]
] | In the present paper we examine a projectively flat spacetime solution of $F(R)$-gravity theory. It is seen that once we deploy projective flatness in the geometry of the spacetime, the matter field has constant energy density and isotropic pressure. We then make the condition weaker and discuss the effects of projectively harmonic spacetime geometry in $F(R)$-gravity theory and show that the spacetime in this case reduces to a generalised Robertson-Walker spacetime with a shear, vorticity, acceleration free perfect fluid with a specific form of expansion scalar presented in terms of the scale factor. Role of conharmonic curvature tensor in the spacetime geometry is also briefly discussed. Some analysis of the obtained results are conducted in terms of couple of $F(R)$-gravity models. |
1901.06954 | Mu-Tao Wang | Po-Ning Chen, Mu-Tao Wang, Ye-Kai Wang, and Shing-Tung Yau | Quasi-local mass on unit spheres at spatial infinity | 24 pages | null | null | null | gr-qc math-ph math.DG math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this note, we compute the limit of the Wang-Yau quasi-local mass on unit
spheres at spatial infinity of an asymptotically flat initial data set. Similar
to the small sphere limit of the Wang-Yau quasi-local mass, we prove that the
leading order term of the quasi-local mass recovers the stress-energy tensor.
For a vacuum spacetime, the quasi-local mass decays faster and the leading
order term is related to the Bel-Robinson tensor. Several new techniques of
evaluating quasilocal mass are developed in this note.
| [
{
"created": "Mon, 21 Jan 2019 15:14:07 GMT",
"version": "v1"
}
] | 2019-01-23 | [
[
"Chen",
"Po-Ning",
""
],
[
"Wang",
"Mu-Tao",
""
],
[
"Wang",
"Ye-Kai",
""
],
[
"Yau",
"Shing-Tung",
""
]
] | In this note, we compute the limit of the Wang-Yau quasi-local mass on unit spheres at spatial infinity of an asymptotically flat initial data set. Similar to the small sphere limit of the Wang-Yau quasi-local mass, we prove that the leading order term of the quasi-local mass recovers the stress-energy tensor. For a vacuum spacetime, the quasi-local mass decays faster and the leading order term is related to the Bel-Robinson tensor. Several new techniques of evaluating quasilocal mass are developed in this note. |
0906.0141 | Sergey Pavluchenko | S.A. Pavluchenko | General features of Bianchi-I cosmological models in Lovelock gravity | extended version of published Brief Report | Phys.Rev.D80:107501,2009 | 10.1103/PhysRevD.80.107501 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We derived equations of motion corresponding to Bianchi-I cosmological models
in the Lovelock gravity. Equations derived in the general case, without any
specific ansatz for any number of spatial dimensions and any order of the
Lovelock correction. We also analyzed the equations of motion solely taking
into account the highest-order correction and described the drastic difference
between the cases with odd and even numbers of spatial dimensions. For
power-law ansatz we derived conditions for Kasner and generalized Milne regimes
for the model considered. Finally, we discuss the possible influence of matter
in the form of perfect fluid on the solutions obtained.
| [
{
"created": "Mon, 1 Jun 2009 12:39:34 GMT",
"version": "v1"
},
{
"created": "Tue, 19 Jan 2010 10:04:22 GMT",
"version": "v2"
}
] | 2010-01-22 | [
[
"Pavluchenko",
"S. A.",
""
]
] | We derived equations of motion corresponding to Bianchi-I cosmological models in the Lovelock gravity. Equations derived in the general case, without any specific ansatz for any number of spatial dimensions and any order of the Lovelock correction. We also analyzed the equations of motion solely taking into account the highest-order correction and described the drastic difference between the cases with odd and even numbers of spatial dimensions. For power-law ansatz we derived conditions for Kasner and generalized Milne regimes for the model considered. Finally, we discuss the possible influence of matter in the form of perfect fluid on the solutions obtained. |
2201.05684 | Fernando Carneiro | F. L. Carneiro, S. C. Ulhoa, J. W. Maluf, J. F. da Rocha-Neto | On the total energy conservation of the Alcubierre spacetime | 25 pages, 11 figures | JCAP07(2022)030 | 10.1088/1475-7516/2022/07/030 | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | In this article, we consider the Alcubierre spacetime, such a spacetime
describes a ``bubble'' that propagates with arbitrary global velocity. This
setting allows movement at a speed greater than that of light. There are some
known problems with this metric, e.g., the source's negative energy and the
violation of the source's energy conservation when the bubble accelerates. We
address these two issues within the realm of the Teleparallel Equivalent of
General Relativity (TEGR). The energy conservation problem can be solved when
considering the energy of the gravitational field itself. The total energy of
the spacetime, gravitational plus source, is conserved even in accelerated
motion. We explicitly show the dependence of energy and gravitational energy
flux on the frame of reference, one adapted to a static observer and the other
to a free-falling one in the same coordinate system. Addressing the problem of
energy negativity of the source, we find that a static observer measures
positive energy of the source, while an Eulerian observer measures a negative
one. Thus, we surmise that negative energy may be a reference problem.
| [
{
"created": "Fri, 14 Jan 2022 21:42:17 GMT",
"version": "v1"
},
{
"created": "Thu, 18 Aug 2022 13:26:52 GMT",
"version": "v2"
}
] | 2022-08-19 | [
[
"Carneiro",
"F. L.",
""
],
[
"Ulhoa",
"S. C.",
""
],
[
"Maluf",
"J. W.",
""
],
[
"da Rocha-Neto",
"J. F.",
""
]
] | In this article, we consider the Alcubierre spacetime, such a spacetime describes a ``bubble'' that propagates with arbitrary global velocity. This setting allows movement at a speed greater than that of light. There are some known problems with this metric, e.g., the source's negative energy and the violation of the source's energy conservation when the bubble accelerates. We address these two issues within the realm of the Teleparallel Equivalent of General Relativity (TEGR). The energy conservation problem can be solved when considering the energy of the gravitational field itself. The total energy of the spacetime, gravitational plus source, is conserved even in accelerated motion. We explicitly show the dependence of energy and gravitational energy flux on the frame of reference, one adapted to a static observer and the other to a free-falling one in the same coordinate system. Addressing the problem of energy negativity of the source, we find that a static observer measures positive energy of the source, while an Eulerian observer measures a negative one. Thus, we surmise that negative energy may be a reference problem. |
gr-qc/0603109 | Prasanta Mahato | Prasanta Mahato | Torsion, Scalar Field, Mass and FRW Cosmology | null | Int.J.Theor.Phys. 44 (2005) 79-93 | null | null | gr-qc | null | In the Einstein-Cartan space $U_4$, an axial vector torsion together with a
scalar field connected to a local scale factor have been considered. By
combining two particular terms from the SO(4,1) Pontryagin density and then
modifying it in a SO(3,1) invariant way, we get a Lagrangian density with
Lagrange multipliers. Then under FRW-cosmological background, where the scalar
field is connected to the source of gravitation, the Euler-Lagrange equations
ultimately give the constancy of the gravitational constant together with only
three kinds of energy densities representing mass, radiation and cosmological
constant. The gravitational constant has been found to be linked with the
geometrical Nieh-Yan density.
| [
{
"created": "Tue, 28 Mar 2006 17:12:39 GMT",
"version": "v1"
},
{
"created": "Fri, 31 Mar 2006 16:58:45 GMT",
"version": "v2"
}
] | 2007-05-23 | [
[
"Mahato",
"Prasanta",
""
]
] | In the Einstein-Cartan space $U_4$, an axial vector torsion together with a scalar field connected to a local scale factor have been considered. By combining two particular terms from the SO(4,1) Pontryagin density and then modifying it in a SO(3,1) invariant way, we get a Lagrangian density with Lagrange multipliers. Then under FRW-cosmological background, where the scalar field is connected to the source of gravitation, the Euler-Lagrange equations ultimately give the constancy of the gravitational constant together with only three kinds of energy densities representing mass, radiation and cosmological constant. The gravitational constant has been found to be linked with the geometrical Nieh-Yan density. |
1108.5220 | Tony Downes | T. G. Downes, G. J. Milburn and C. M. Caves | Optimal Quantum Estimation for Gravitation | null | null | null | null | gr-qc math-ph math.MP quant-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Here we describe the quantum limit to measurement of the classical
gravitational field. Specifically, we write down the optimal quantum Cramer-Rao
lower bound, for any single parameter describing a metric for spacetime. The
standard time-energy and Heisenberg uncertainty relations are shown to be
special cases of the uncertainty relation for the spacetime metric. Four key
examples are given, describing quantum limited estimation for: acceleration,
black holes, gravitational waves and cosmology. We employ the locally covariant
formulation of quantum field theory in curved spacetime, which allows for a
manifestly spacetime independent derivation. The result is an uncertainty
relation applicable to all causal spacetime manifolds.
| [
{
"created": "Fri, 26 Aug 2011 01:05:25 GMT",
"version": "v1"
},
{
"created": "Mon, 5 Nov 2012 23:34:16 GMT",
"version": "v2"
}
] | 2012-11-07 | [
[
"Downes",
"T. G.",
""
],
[
"Milburn",
"G. J.",
""
],
[
"Caves",
"C. M.",
""
]
] | Here we describe the quantum limit to measurement of the classical gravitational field. Specifically, we write down the optimal quantum Cramer-Rao lower bound, for any single parameter describing a metric for spacetime. The standard time-energy and Heisenberg uncertainty relations are shown to be special cases of the uncertainty relation for the spacetime metric. Four key examples are given, describing quantum limited estimation for: acceleration, black holes, gravitational waves and cosmology. We employ the locally covariant formulation of quantum field theory in curved spacetime, which allows for a manifestly spacetime independent derivation. The result is an uncertainty relation applicable to all causal spacetime manifolds. |
2305.05438 | Killian Martineau | Maxime De Sousa, Aur\'elien Barrau, Killian Martineau | Closer look at cosmological consequences of interacting group field
theory | null | null | 10.1016/j.physletb.2023.138069 | null | gr-qc hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Group field theory has shown to be a promising framework to derive
cosmological predictions from full quantum gravity. In this brief note, we
revisit the background dynamics when interaction terms are taken into account
and conclude that, although the bounce is clearly robust, providing a
geometrical explanation for inflation seems to be very difficult. We consider
possible improvements and modifications of the original scenario and derive
several limits on the parameters of the model.
| [
{
"created": "Tue, 9 May 2023 13:29:58 GMT",
"version": "v1"
},
{
"created": "Tue, 5 Sep 2023 10:02:32 GMT",
"version": "v2"
}
] | 2023-09-06 | [
[
"De Sousa",
"Maxime",
""
],
[
"Barrau",
"Aurélien",
""
],
[
"Martineau",
"Killian",
""
]
] | Group field theory has shown to be a promising framework to derive cosmological predictions from full quantum gravity. In this brief note, we revisit the background dynamics when interaction terms are taken into account and conclude that, although the bounce is clearly robust, providing a geometrical explanation for inflation seems to be very difficult. We consider possible improvements and modifications of the original scenario and derive several limits on the parameters of the model. |
gr-qc/0206030 | Chryssomalis Chryssomalakos | C. Chryssomalakos and D. Sudarsky (ICN, UNAM) | On the Geometrical Character of Gravitation | 10 pages. Submitted to General Relativity and Gravitation. V2: a
misspelled reference corrected | Gen.Rel.Grav. 35 (2003) 605-617 | 10.1023/A:1022957916776 | null | gr-qc quant-ph | null | The issue of whether some manifestations of gravitation in the quantum
domain, are indicative or not of a non-geometrical aspect in gravitation is
discussed. We examine some examples that have been considered in this context,
providing a critical analysis of previous interpretations. The analysis of
these examples is illustrative about certain details in the interpretation of
quantum mechanics. We conclude that there are, at this time, no indications of
such departure from the geometrical character of gravitation.
| [
{
"created": "Tue, 11 Jun 2002 02:11:38 GMT",
"version": "v1"
},
{
"created": "Thu, 13 Jun 2002 23:32:34 GMT",
"version": "v2"
}
] | 2015-06-25 | [
[
"Chryssomalakos",
"C.",
"",
"ICN, UNAM"
],
[
"Sudarsky",
"D.",
"",
"ICN, UNAM"
]
] | The issue of whether some manifestations of gravitation in the quantum domain, are indicative or not of a non-geometrical aspect in gravitation is discussed. We examine some examples that have been considered in this context, providing a critical analysis of previous interpretations. The analysis of these examples is illustrative about certain details in the interpretation of quantum mechanics. We conclude that there are, at this time, no indications of such departure from the geometrical character of gravitation. |
2001.11156 | Maxime Van de Moortel | Maxime Van de Moortel | Mass inflation and the $C^2$-inextendibility of spherically symmetric
charged scalar field dynamical black holes | Versions accepted for publication in Communications in Mathematical
Physics | null | 10.1007/s00220-020-03923-w | null | gr-qc math-ph math.AP math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | It has long been suggested that the Cauchy horizon of dynamical black holes
is subject to a weak null singularity, under the mass inflation scenario. We
study in spherical symmetry the Einstein-Maxwell-Klein-Gordon equations and
\textit{while we do not directly show mass inflation}, we obtain a "mass
inflation/ridigity" dichotomy. More precisely, we prove assuming (sufficiently
slow) decay of the charged scalar field on the event horizon, that the Cauchy
horizon emanating from time-like infinity is $\mathcal{CH}_{i^+}= \mathcal{D}
\cup \mathcal{S}$ for two (possibly empty) disjoint connected sets
$\mathcal{D}$ and $\mathcal{S}$ such that:
_$\mathcal{D}$ (the dynamical set) is a past set on which the Hawking mass
blows up (mass inflation scenario).
_$\mathcal{S}$ (the static set) is a future set isometric to a
Reissner--Nordstr\"{o}m Cauchy horizon i.e.\ the radiation is zero on
$\mathcal{S}$.
As a consequence, we establish a novel classification of Cauchy horizons into
three types: dynamical ($\mathcal{S}=\emptyset$), static
($\mathcal{D}=\emptyset$) or mixed, and prove that $\mathcal{CH}_{i^+}$ is
globally $C^2$-inextendible. Our main motivation is the $C^2$ Strong Cosmic
Censorship Conjecture for a realistic model of spherical collapse in which
charged matter emulates the repulsive role of angular momentum: in our case the
Einstein-Maxwell-Klein-Gordon system on one-ended space-times. As a result, we
prove in spherical symmetry that:
- two-ended asymptotically flat space-times are $C^2$-future-inextendible
i.e. $C^2$ Strong Cosmic Censorship is true for Einstein-Maxwell-Klein-Gordon,
assuming the decay of the scalar field on the event horizon at the expected
rate.
- In the one-ended case, the Cauchy horizon emanating from time-like infinity
is $C^2$-inextendible. This result suppresses the main obstruction to $C^2$
Strong Cosmic Censorship in spherical collapse.
| [
{
"created": "Thu, 30 Jan 2020 02:43:31 GMT",
"version": "v1"
},
{
"created": "Thu, 20 Aug 2020 15:06:53 GMT",
"version": "v2"
}
] | 2021-02-03 | [
[
"Van de Moortel",
"Maxime",
""
]
] | It has long been suggested that the Cauchy horizon of dynamical black holes is subject to a weak null singularity, under the mass inflation scenario. We study in spherical symmetry the Einstein-Maxwell-Klein-Gordon equations and \textit{while we do not directly show mass inflation}, we obtain a "mass inflation/ridigity" dichotomy. More precisely, we prove assuming (sufficiently slow) decay of the charged scalar field on the event horizon, that the Cauchy horizon emanating from time-like infinity is $\mathcal{CH}_{i^+}= \mathcal{D} \cup \mathcal{S}$ for two (possibly empty) disjoint connected sets $\mathcal{D}$ and $\mathcal{S}$ such that: _$\mathcal{D}$ (the dynamical set) is a past set on which the Hawking mass blows up (mass inflation scenario). _$\mathcal{S}$ (the static set) is a future set isometric to a Reissner--Nordstr\"{o}m Cauchy horizon i.e.\ the radiation is zero on $\mathcal{S}$. As a consequence, we establish a novel classification of Cauchy horizons into three types: dynamical ($\mathcal{S}=\emptyset$), static ($\mathcal{D}=\emptyset$) or mixed, and prove that $\mathcal{CH}_{i^+}$ is globally $C^2$-inextendible. Our main motivation is the $C^2$ Strong Cosmic Censorship Conjecture for a realistic model of spherical collapse in which charged matter emulates the repulsive role of angular momentum: in our case the Einstein-Maxwell-Klein-Gordon system on one-ended space-times. As a result, we prove in spherical symmetry that: - two-ended asymptotically flat space-times are $C^2$-future-inextendible i.e. $C^2$ Strong Cosmic Censorship is true for Einstein-Maxwell-Klein-Gordon, assuming the decay of the scalar field on the event horizon at the expected rate. - In the one-ended case, the Cauchy horizon emanating from time-like infinity is $C^2$-inextendible. This result suppresses the main obstruction to $C^2$ Strong Cosmic Censorship in spherical collapse. |
gr-qc/0009028 | Arkadii A. Popov | Arkadii A. Popov, Sergey V. Sushkov | Vacuum polarization of a scalar field in wormhole spacetimes | 10 pages, RevTeX, two eps figures | Phys.Rev. D63 (2001) 044017 | 10.1103/PhysRevD.63.044017 | KGPU-00-01 | gr-qc | null | An analitical approximation of $<\phi^2>$ for a scalar field in a static
spherically symmetric wormhole spacetime is obtained. The scalar field is
assumed to be both massive and massless, with an arbitrary coupling $\xi$ to
the scalar curvature, and in a zero temperature vacuum state.
| [
{
"created": "Sun, 10 Sep 2000 07:20:36 GMT",
"version": "v1"
}
] | 2009-10-31 | [
[
"Popov",
"Arkadii A.",
""
],
[
"Sushkov",
"Sergey V.",
""
]
] | An analitical approximation of $<\phi^2>$ for a scalar field in a static spherically symmetric wormhole spacetime is obtained. The scalar field is assumed to be both massive and massless, with an arbitrary coupling $\xi$ to the scalar curvature, and in a zero temperature vacuum state. |
1812.11191 | Anzhong Wang | Bao-Fei Li, Tao Zhu, Anzhong Wang, Klaus Kirsten, Gerald Cleaver, and
Qin Sheng | Preinflationary perturbations from the closed algebra approach in loop
quantum cosmology | Corrected some typos. Phys. Rev. D99, 103536 (2019) | Phys. Rev. D 99, 103536 (2019) | 10.1103/PhysRevD.99.103536 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, the scalar and tensor perturbations in the closed algebra
approach of loop quantum cosmology are studied. Instead of the distant past in
the contracting phase, we choose the moment at which the initial conditions are
imposed to be the silent point, which circumvents the problem due to the
signature change in the super-inflationary phase and results in a well-defined
Cauchy problem. For the ultraviolet and infrared modes, different approaches
are applied in order to obtain analytical solutions with high accuracy. While
previous numerical simulations reveal an exponentially divergent power spectrum
in the ultraviolet regime, when the initial conditions are imposed in the
remote contracting phase, we find a special set of initial conditions at the
silent point, which can reproduce results that are consistent with current
observations.
| [
{
"created": "Fri, 28 Dec 2018 19:00:09 GMT",
"version": "v1"
},
{
"created": "Thu, 25 Apr 2019 20:08:45 GMT",
"version": "v2"
},
{
"created": "Fri, 17 May 2019 11:44:02 GMT",
"version": "v3"
},
{
"created": "Wed, 29 May 2019 13:42:52 GMT",
"version": "v4"
}
] | 2019-06-05 | [
[
"Li",
"Bao-Fei",
""
],
[
"Zhu",
"Tao",
""
],
[
"Wang",
"Anzhong",
""
],
[
"Kirsten",
"Klaus",
""
],
[
"Cleaver",
"Gerald",
""
],
[
"Sheng",
"Qin",
""
]
] | In this paper, the scalar and tensor perturbations in the closed algebra approach of loop quantum cosmology are studied. Instead of the distant past in the contracting phase, we choose the moment at which the initial conditions are imposed to be the silent point, which circumvents the problem due to the signature change in the super-inflationary phase and results in a well-defined Cauchy problem. For the ultraviolet and infrared modes, different approaches are applied in order to obtain analytical solutions with high accuracy. While previous numerical simulations reveal an exponentially divergent power spectrum in the ultraviolet regime, when the initial conditions are imposed in the remote contracting phase, we find a special set of initial conditions at the silent point, which can reproduce results that are consistent with current observations. |
1710.08395 | Sreeram Valluri SR | F. Chishtie, S.R. Valluri | An analytic approach for the study of pulsar spindown | null | null | 10.1088/1361-6382/aac9d6 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work we develop an analytic approach to study pulsar spindown. We use
the monopolar spindown model by Alvarez and Carrami\~{n}ana (2004), which
assumes an inverse linear law of magnetic field decay of the pulsar, to extract
an all-order formula for the spindown parameters which are expressed in terms
of modified Bessel functions. We further extend the analytic model to
incorporate the quadrupole term that accounts for the emission of gravitational
radiation, and obtain expressions for the period $P$ and frequency $f$ in terms
of transcendental equations. We derive the period of the pulsar evolution as an
approximate first order solution in the small parameter present in the full
solution. We find that the first three spindown parameters of the Crab, PSR
B1509-58, PSR B0540-69 and Vela pulsars are within their known bounds providing
a consistency check on our approach. After the four detections of gravitational
waves from binary black hole coalescence and a binary neutron merger 170814,
which was a novel joint gravitational and electromagnetic detection, a
detection of gravitational waves from pulsars will be the next landmark in the
field of multi-messenger gravitational wave astronomy.
| [
{
"created": "Mon, 23 Oct 2017 17:19:15 GMT",
"version": "v1"
}
] | 2018-07-11 | [
[
"Chishtie",
"F.",
""
],
[
"Valluri",
"S. R.",
""
]
] | In this work we develop an analytic approach to study pulsar spindown. We use the monopolar spindown model by Alvarez and Carrami\~{n}ana (2004), which assumes an inverse linear law of magnetic field decay of the pulsar, to extract an all-order formula for the spindown parameters which are expressed in terms of modified Bessel functions. We further extend the analytic model to incorporate the quadrupole term that accounts for the emission of gravitational radiation, and obtain expressions for the period $P$ and frequency $f$ in terms of transcendental equations. We derive the period of the pulsar evolution as an approximate first order solution in the small parameter present in the full solution. We find that the first three spindown parameters of the Crab, PSR B1509-58, PSR B0540-69 and Vela pulsars are within their known bounds providing a consistency check on our approach. After the four detections of gravitational waves from binary black hole coalescence and a binary neutron merger 170814, which was a novel joint gravitational and electromagnetic detection, a detection of gravitational waves from pulsars will be the next landmark in the field of multi-messenger gravitational wave astronomy. |
1304.0670 | LVK Publication | The LIGO Scientific Collaboration, the Virgo Collaboration, and the
KAGRA Collaboration: B. P. Abbott, R. Abbott, T. D. Abbott, S. Abraham, F.
Acernese, K. Ackley, C. Adams, V. B. Adya, C. Affeldt, M. Agathos, K.
Agatsuma, N. Aggarwal, O. D. Aguiar, L. Aiello, A. Ain, P. Ajith, T. Akutsu,
G. Allen, A. Allocca, M. A. Aloy, P. A. Altin, A. Amato, A. Ananyeva, S. B.
Anderson, W. G. Anderson, M. Ando, S. V. Angelova, S. Antier, S. Appert, K.
Arai, Koya Arai, Y. Arai, S. Araki, A. Araya, M. C. Araya, J. S. Areeda, M.
Ar\`ene, N. Aritomi, N. Arnaud, K. G. Arun, S. Ascenzi, G. Ashton, Y. Aso, S.
M. Aston, P. Astone, F. Aubin, P. Aufmuth, K. AultONeal, C. Austin, V.
Avendano, A. Avila-Alvarez, S. Babak, P. Bacon, F. Badaracco, M. K. M. Bader,
S. W. Bae, Y. B. Bae, L. Baiotti, R. Bajpai, 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, S. Barnum, F. Barone, B. Barr, L. Barsotti, M.
Barsuglia, D. Barta, J. Bartlett, M. A. Barton, I. Bartos, R. Bassiri, A.
Basti, M. Bawaj, J. C. Bayley, M. Bazzan, B. B\'ecsy, M. Bejger, I.
Belahcene, A. S. Bell, D. Beniwal, B. K. Berger, G. Bergmann, S. Bernuzzi, J.
J. Bero, C. P. L. Berry, D. Bersanetti, A. Bertolini, J. Betzwieser, R.
Bhandare, J. Bidler, I. A. Bilenko, S. A. Bilgili, G. Billingsley, J. Birch,
R. Birney, O. Birnholtz, S. Biscans, S. Biscoveanu, A. Bisht, M. Bitossi, M.
A. Bizouard, J. K. Blackburn, C. D. Blair, D. G. Blair, R. M. Blair, S.
Bloemen, N. Bode, M. Boer, Y. Boetzel, G. Bogaert, F. Bondu, E. Bonilla, R.
Bonnand, P. Booker, B. A. Boom, C. D. Booth, R. Bork, V. Boschi, S. Bose, K.
Bossie, V. Bossilkov, J. Bosveld, Y. Bouffanais, A. Bozzi, C. Bradaschia, P.
R. Brady, A. Bramley, M. Branchesi, J. E. Brau, T. Briant, J. H. Briggs, F.
Brighenti, A. Brillet, M. Brinkmann, V. Brisson, P. Brockill, A. F. Brooks,
D. A. Brown, D. D. Brown, S. Brunett, 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, W. A. Campbell, M. Canepa, K. Cannon, K. C. Cannon, H. Cao, J.
Cao, E. Capocasa, F. Carbognani, S. Caride, M. F. Carney, G. Carullo, J.
Casanueva Diaz, C. Casentini, S. Caudill, M. Cavagli\`a, F. Cavalier, R.
Cavalieri, G. Cella, P. Cerd\'a-Dur\'an, G. Cerretani, E. Cesarini, O.
Chaibi, K. Chakravarti, S. J. Chamberlin, M. Chan, M. L. Chan, S. Chao, P.
Charlton, E. A. Chase, E. Chassande-Mottin, D. Chatterjee, M. Chaturvedi, K.
Chatziioannou, B. D. Cheeseboro, C. S. Chen, H. Y. Chen, K. H. Chen, X. Chen,
Y. Chen, Y. R. Chen, H.-P. Cheng, C. K. Cheong, H. Y. Chia, A. Chincarini, A.
Chiummo, G. Cho, H. S. Cho, M. Cho, N. Christensen, H. Y. Chu, Q. Chu, Y. K.
Chu, S. Chua, K. W. Chung, S. Chung, G. Ciani, A. A. Ciobanu, R. Ciolfi, F.
Cipriano, A. Cirone, F. Clara, J. A. Clark, P. Clearwater, F. Cleva, C.
Cocchieri, E. Coccia, P.-F. Cohadon, D. Cohen, R. Colgan, M. Colleoni, C. G.
Collette, C. Collins, 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, R. Cotesta, 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, M. Croquette, 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, L.
E. H. Datrier, V. Dattilo, I. Dave, M. Davier, D. Davis, E. J. Daw, D. DeBra,
M. Deenadayalan, J. Degallaix, M. De Laurentis, S. Del\'eglise, W. Del Pozzo,
L. M. DeMarchi, N. Demos, T. Dent, R. De Pietri, J. Derby, R. De Rosa, C. De
Rossi, R. DeSalvo, O. de Varona, S. Dhurandhar, M. C. D\'iaz, T. Dietrich, L.
Di Fiore, M. Di Giovanni, T. Di Girolamo, A. Di Lieto, B. Ding, S. Di Pace,
I. Di Palma, F. Di Renzo, A. Dmitriev, Z. Doctor, K. Doi, F. Donovan, K. L.
Dooley, S. Doravari, I. Dorrington, T. P. Downes, M. Drago, J. C. Driggers,
Z. Du, J.-G. Ducoin, P. Dupej, S. E. Dwyer, P. J. Easter, T. B. Edo, M. C.
Edwards, A. Effler, S. Eguchi, P. Ehrens, J. Eichholz, S. S. Eikenberry, M.
Eisenmann, R. A. Eisenstein, Y. Enomoto, R. C. Essick, H. Estelles, D.
Estevez, Z. B. Etienne, T. Etzel, M. Evans, T. M. Evans, V. Fafone, H. Fair,
S. Fairhurst, X. Fan, S. Farinon, B. Farr, W. M. Farr, E. J. Fauchon-Jones,
M. Favata, M. Fays, M. Fazio, C. Fee, J. Feicht, M. M. Fejer, F. Feng, A.
Fernandez-Galiana, I. Ferrante, E. C. Ferreira, T. A. Ferreira, F. Ferrini,
F. Fidecaro, I. Fiori, D. Fiorucci, M. Fishbach, R. P. Fisher, J. M. Fishner,
M. Fitz-Axen, R. Flaminio, M. Fletcher, E. Flynn, H. Fong, J. A. Font, P. W.
F. Forsyth, J.-D. Fournier, S. Frasca, F. Frasconi, Z. Frei, A. Freise, R.
Frey, V. Frey, P. Fritschel, V. V. Frolov, Y. Fujii, M. Fukunaga, M.
Fukushima, P. Fulda, M. Fyffe, H. A. Gabbard, B. U. Gadre, S. M. Gaebel, J.
R. Gair, L. Gammaitoni, M. R. Ganija, S. G. Gaonkar, A. Garcia, C.
Garc\'ia-Quir\'os, F. Garufi, B. Gateley, S. Gaudio, G. Gaur, V. Gayathri, G.
G. Ge, G. Gemme, E. Genin, A. Gennai, D. George, J. George, L. Gergely, V.
Germain, S. Ghonge, Abhirup Ghosh, Archisman Ghosh, S. Ghosh, B. Giacomazzo,
J. A. Giaime, K. D. Giardina, A. Giazotto, K. Gill, G. Giordano, L. Glover,
P. Godwin, E. Goetz, R. Goetz, 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, P. Grassia, C. Gray, R.
Gray, G. Greco, A. C. Green, R. Green, E. M. Gretarsson, P. Groot, H. Grote,
S. Grunewald, P. Gruning, G. M. Guidi, H. K. Gulati, Y. Guo, A. Gupta, M. K.
Gupta, E. K. Gustafson, R. Gustafson, L. Haegel, A. Hagiwara, S. Haino, 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, K. Haris, J. Harms, G. M. Harry, I. W. Harry, K. Hasegawa, C.-J.
Haster, K. Haughian, H. Hayakawa, K. Hayama, F. J. Hayes, 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, Y. Himemoto, T.
Hinderer, Y. Hiranuma, N. Hirata, E. Hirose, D. Hoak, S. Hochheim, D. Hofman,
A. M. Holgado, N. A. Holland, K. Holt, D. E. Holz, Z. Hong, P. Hopkins, C.
Horst, J. Hough, E. J. Howell, C. G. Hoy, A. Hreibi, B. H. Hsieh, G. Z.
Huang, P. W. Huang, Y. J. Huang, E. A. Huerta, D. Huet, B. Hughey, M. Hulko,
S. Husa, S. H. Huttner, T. Huynh-Dinh, B. Idzkowski, A. Iess, B. Ikenoue, S.
Imam, K. Inayoshi, C. Ingram, Y. Inoue, R. Inta, G. Intini, K. Ioka, B.
Irwin, H. N. Isa, J.-M. Isac, M. Isi, Y. Itoh, B. R. Iyer, K. Izumi, T.
Jacqmin, S. J. Jadhav, K. Jani, N. N. Janthalur, P. Jaranowski, A. C.
Jenkins, J. Jiang, D. S. Johnson, A. W. Jones, D. I. Jones, R. Jones, R. J.
G. Jonker, L. Ju, K. Jung, P. Jung, J. Junker, T. Kajita, C. V. Kalaghatgi,
V. Kalogera, B. Kamai, M. Kamiizumi, N. Kanda, S. Kandhasamy, G. W. Kang, J.
B. Kanner, S. J. Kapadia, S. Karki, K. S. Karvinen, R. Kashyap, M. Kasprzack,
S. Katsanevas, E. Katsavounidis, W. Katzman, S. Kaufer, K. Kawabe, K.
Kawaguchi, N. Kawai, T. Kawasaki, N. V. Keerthana, F. K\'ef\'elian, D.
Keitel, R. Kennedy, J. S. Key, F. Y. Khalili, H. Khan, I. Khan, S. Khan, Z.
Khan, E. A. Khazanov, M. Khursheed, N. Kijbunchoo, Chunglee Kim, C. Kim, J.
C. Kim, J. Kim, K. Kim, W. Kim, W. S. Kim, Y.-M. Kim, C. Kimball, N. Kimura,
E. J. King, P. J. King, M. Kinley-Hanlon, R. Kirchhoff, J. S. Kissel, N.
Kita, H. Kitazawa, L. Kleybolte, J. H. Klika, S. Klimenko, T. D. Knowles, P.
Koch, S. M. Koehlenbeck, G. Koekoek, Y. Kojima, K. Kokeyama, S. Koley, K.
Komori, V. Kondrashov, A. K. H. Kong, A. Kontos, N. Koper, M. Korobko, W. Z.
Korth, K. Kotake, I. Kowalska, D. B. Kozak, C. Kozakai, R. Kozu, V. Kringel,
N. Krishnendu, A. Kr\'olak, G. Kuehn, A. Kumar, P. Kumar, Rahul Kumar, R.
Kumar, S. Kumar, J. Kume, C. M. Kuo, H. S. Kuo, L. Kuo, S. Kuroyanagi, K.
Kusayanagi, A. Kutynia, K. Kwak, S. Kwang, B. D. Lackey, K. H. Lai, T. L.
Lam, M. Landry, B. B. Lane, 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, Y. K. Lecoeuche, C. H. Lee, H. K. Lee, H. M. Lee, H. W. Lee, J.
Lee, K. Lee, R. K. Lee, J. Lehmann, A. Lenon, M. Leonardi, N. Leroy, N.
Letendre, Y. Levin, J. Li, K. J. L. Li, T. G. F. Li, X. Li, C. Y. Lin, F.
Lin, F. L. Lin, L. C. C. Lin, F. Linde, S. D. Linker, T. B. Littenberg, G. C.
Liu, J. Liu, X. Liu, R. K. L. Lo, N. A. Lockerbie, L. T. London, A. Longo, M.
Lorenzini, V. Loriette, M. Lormand, G. Losurdo, J. D. Lough, C. O. Lousto, G.
Lovelace, M. E. Lower, H. L\"uck, D. Lumaca, A. P. Lundgren, L. W. Luo, R.
Lynch, Y. Ma, R. Macas, S. Macfoy, M. MacInnis, D. M. Macleod, A. Macquet, F.
Maga\~na-Sandoval, L. Maga\~na Zertuche, R. M. Magee, E. Majorana, I.
Maksimovic, A. Malik, N. Man, V. Mandic, V. Mangano, G. L. Mansell, M.
Manske, M. Mantovani, F. Marchesoni, M. Marchio, F. Marion, S. M\'arka, Z.
M\'arka, C. Markakis, A. S. Markosyan, A. Markowitz, E. Maros, A. Marquina,
S. Marsat, F. Martelli, 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, J. J. McCann,
R. McCarthy, D. E. McClelland, S. McCormick, L. McCuller, S. C. McGuire, J.
McIver, D. J. McManus, T. McRae, S. T. McWilliams, D. Meacher, G. D. Meadors,
M. Mehmet, A. K. Mehta, J. Meidam, A. Melatos, G. Mendell, R. A. Mercer, L.
Mereni, E. L. Merilh, M. Merzougui, S. Meshkov, C. Messenger, C. Messick, R.
Metzdorff, P. M. Meyers, H. Miao, C. Michel, Y. Michimura, H. Middleton, E.
E. Mikhailov, L. Milano, A. L. Miller, A. Miller, M. Millhouse, J. C. Mills,
M. C. Milovich-Goff, O. Minazzoli, Y. Minenkov, N. Mio, A. Mishkin, C.
Mishra, T. Mistry, S. Mitra, V. P. Mitrofanov, G. Mitselmakher, R. Mittleman,
O. Miyakawa, A. Miyamoto, Y. Miyazaki, K. Miyo, S. Miyoki, G. Mo, D. Moffa,
K. Mogushi, S. R. P. Mohapatra, M. Montani, C. J. Moore, D. Moraru, G.
Moreno, S. Morisaki, Y. Moriwaki, B. Mours, C. M. Mow-Lowry, Arunava
Mukherjee, D. Mukherjee, S. Mukherjee, N. Mukund, A. Mullavey, J. Munch, E.
A. Mu\~niz, M. Muratore, P. G. Murray, K. Nagano, S. Nagano, A. Nagar, K.
Nakamura, H. Nakano, M. Nakano, R. Nakashima, I. Nardecchia, T. Narikawa, L.
Naticchioni, R. K. Nayak, R. Negishi, J. Neilson, G. Nelemans, T. J. N.
Nelson, M. Nery, A. Neunzert, K. Y. Ng, S. Ng, P. Nguyen, W. T. Ni, D.
Nichols, A. Nishizawa, S. Nissanke, F. Nocera, C. North, L. K. Nuttall, M.
Obergaulinger, J. Oberling, B. D. O'Brien, Y. Obuchi, G. D. O'Dea, W. Ogaki,
G. H. Ogin, J. J. Oh, S. H. Oh, M. Ohashi, N. Ohishi, M. Ohkawa, F. Ohme, H.
Ohta, M. A. Okada, K. Okutomi, M. Oliver, K. Oohara, C. P. Ooi, P. Oppermann,
Richard J. Oram, B. O'Reilly, R. G. Ormiston, L. F. Ortega, R. O'Shaughnessy,
S. Oshino, S. Ossokine, D. J. Ottaway, H. Overmier, B. J. Owen, A. E. Pace,
G. Pagano, M. A. Page, A. Pai, S. A. Pai, J. R. Palamos, O. Palashov, C.
Palomba, A. Pal-Singh, Huang-Wei Pan, K. C. Pan, B. Pang, H. F. Pang, P. T.
H. Pang, C. Pankow, F. Pannarale, B. C. Pant, F. Paoletti, A. Paoli, M. A.
Papa, A. Parida, J. Park, W. Parker, D. Pascucci, A. Pasqualetti, R.
Passaquieti, D. Passuello, M. Patil, B. Patricelli, B. L. Pearlstone, C.
Pedersen, M. Pedraza, R. Pedurand, A. Pele, F. E. Pe\~na Arellano, S. Penn,
C. J. Perez, A. Perreca, H. P. Pfeiffer, M. Phelps, K. S. Phukon, O. J.
Piccinni, M. Pichot, F. Piergiovanni, G. Pillant, L. Pinard, I. Pinto, M.
Pirello, M. Pitkin, R. Poggiani, D. Y. T. Pong, S. Ponrathnam, P. Popolizio,
E. K. Porter, J. Powell, A. K. Prajapati, J. Prasad, K. Prasai, R. Prasanna,
G. Pratten, T. Prestegard, S. Privitera, G. A. Prodi, L. G. Prokhorov, O.
Puncken, M. Punturo, P. Puppo, M. P\"urrer, H. Qi, V. Quetschke, P. J.
Quinonez, E. A. Quintero, R. Quitzow-James, F. J. Raab, H. Radkins, N.
Radulescu, P. Raffai, S. Raja, C. Rajan, B. Rajbhandari, M. Rakhmanov, K. E.
Ramirez, A. Ramos-Buades, Javed Rana, K. Rao, P. Rapagnani, V. Raymond, M.
Razzano, J. Read, T. Regimbau, L. Rei, S. Reid, D. H. Reitze, W. Ren, F.
Ricci, C. J. Richardson, J. W. Richardson, P. M. Ricker, K. Riles, M. Rizzo,
N. A. Robertson, R. Robie, F. Robinet, A. Rocchi, L. Rolland, J. G. Rollins,
V. J. Roma, M. Romanelli, R. Romano, C. L. Romel, J. H. Romie, K. Rose, D.
Rosi\'nska, S. G. Rosofsky, M. P. Ross, S. Rowan, A. R\"udiger, P. Ruggi, G.
Rutins, K. Ryan, S. Sachdev, T. Sadecki, N. Sago, S. Saito, Y. Saito, K.
Sakai, Y. Sakai, H. Sakamoto, M. Sakellariadou, Y. Sakuno, L. Salconi, M.
Saleem, A. Samajdar, L. Sammut, E. J. Sanchez, L. E. Sanchez, N.
Sanchis-Gual, V. Sandberg, J. R. Sanders, K. A. Santiago, N. Sarin, B.
Sassolas, B. S. Sathyaprakash, S. Sato, T. Sato, O. Sauter, R. L. Savage, T.
Sawada, P. Schale, M. Scheel, J. Scheuer, P. Schmidt, R. Schnabel, R. M. S.
Schofield, A. Sch\"onbeck, E. Schreiber, B. W. Schulte, B. F. Schutz, S. G.
Schwalbe, J. Scott, S. M. Scott, E. Seidel, T. Sekiguchi, Y. Sekiguchi, D.
Sellers, A. S. Sengupta, N. Sennett, D. Sentenac, V. Sequino, A. Sergeev, Y.
Setyawati, D. A. Shaddock, T. Shaffer, M. S. Shahriar, M. B. Shaner, L. Shao,
P. Sharma, P. Shawhan, H. Shen, S. Shibagaki, R. Shimizu, T. Shimoda, K.
Shimode, R. Shink, H. Shinkai, T. Shishido, A. Shoda, D. H. Shoemaker, D. M.
Shoemaker, S. ShyamSundar, K. Siellez, M. Sieniawska, D. Sigg, A. D. Silva,
L. P. Singer, N. Singh, A. Singhal, A. M. Sintes, S. Sitmukhambetov, V.
Skliris, B. J. J. Slagmolen, T. J. Slaven-Blair, J. R. Smith, R. J. E. Smith,
S. Somala, K. Somiya, E. J. Son, B. Sorazu, F. Sorrentino, H. Sotani, T.
Souradeep, E. Sowell, A. P. Spencer, A. K. Srivastava, V. Srivastava, K.
Staats, C. Stachie, M. Standke, D. A. Steer, M. Steinke, J. Steinlechner, S.
Steinlechner, D. Steinmeyer, S. P. Stevenson, D. Stocks, R. Stone, D. J.
Stops, K. A. Strain, G. Stratta, S. E. Strigin, A. Strunk, R. Sturani, A. L.
Stuver, V. Sudhir, R. Sugimoto, T. Z. Summerscales, L. Sun, S. Sunil, J.
Suresh, P. J. Sutton, Takamasa Suzuki, Toshikazu Suzuki, B. L. Swinkels, M.
J. Szczepa\'nczyk, M. Tacca, H. Tagoshi, S. C. Tait, H. Takahashi, R.
Takahashi, A. Takamori, S. Takano, H. Takeda, M. Takeda, C. Talbot, D.
Talukder, H. Tanaka, Kazuyuki Tanaka, Kenta Tanaka, Taiki Tanaka, Takahiro
Tanaka, S. Tanioka, D. B. Tanner, M. T\'apai, E. N. Tapia San Martin, A.
Taracchini, J. D. Tasson, R. Taylor, S. Telada, F. Thies, M. Thomas, P.
Thomas, S. R. Thondapu, K. A. Thorne, E. Thrane, Shubhanshu Tiwari, Srishti
Tiwari, V. Tiwari, K. Toland, T. Tomaru, Y. Tomigami, T. Tomura, M. Tonelli,
Z. Tornasi, A. Torres-Forn\'e, C. I. Torrie, D. T\"oyr\"a, F. Travasso, G.
Traylor, M. C. Tringali, A. Trovato, L. Trozzo, R. Trudeau, K. W. Tsang, T.
T. L. Tsang, M. Tse, R. Tso, K. Tsubono, S. Tsuchida, L. Tsukada, D. Tsuna,
T. Tsuzuki, D. Tuyenbayev, N. Uchikata, T. Uchiyama, A. Ueda, T. Uehara, K.
Ueno, G. Ueshima, D. Ugolini, C. S. Unnikrishnan, F. Uraguchi, A. L. Urban,
T. Ushiba, 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, M. H. P. M. van Putten, 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, D. J. Vine, J.-Y. Vinet, S. Vitale,
Francisco Hernandez Vivanco, 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. Wang, J. Z. Wang, W. H. Wang, Y. F. Wang, R. L. Ward, Z.
A. Warden, J. Warner, M. Was, J. Watchi, B. Weaver, L.-W. Wei, M. Weinert, A.
J. Weinstein, R. Weiss, F. Wellmann, L. Wen, E. K. Wessel, P. We{\ss}els, J.
W. Westhouse, K. Wette, J. T. Whelan, B. F. Whiting, C. Whittle, D. M.
Wilken, 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. K. Wofford, J.
Worden, J. L. Wright, C. M. Wu, D. S. Wu, H. C. Wu, S. R. Wu, D. M. Wysocki,
L. Xiao, W. R. Xu, T. Yamada, H. Yamamoto, Kazuhiro Yamamoto, Kohei Yamamoto,
T. Yamamoto, C. C. Yancey, L. Yang, M. J. Yap, M. Yazback, D. W. Yeeles, K.
Yokogawa, J. Yokoyama, T. Yokozawa, T. Yoshioka, Hang Yu, Haocun Yu, S. H. R.
Yuen, H. Yuzurihara, M. Yvert, A. K. Zadro\.zny, M. Zanolin, S. Zeidler, T.
Zelenova, J.-P. Zendri, M. Zevin, J. Zhang, L. Zhang, T. Zhang, C. Zhao, Y.
Zhao, M. Zhou, Z. Zhou, X. J. Zhu, Z. H. Zhu, A. B. Zimmerman, M. E. Zucker,
J. Zweizig | Prospects for Observing and Localizing Gravitational-Wave Transients
with Advanced LIGO, Advanced Virgo and KAGRA | 52 pages, 9 figures, 5 tables. We have updated the detector
sensitivities (including the A+ and AdV+ upgrade); added expectations for
binary black-holes, neutron-star black-holes, and intermediate-mass black
holes; and added 3D volume localization expectations. This update is to
change some numbers in Table 5 based on refinements to the simulations. Three
authors were added | Living Rev Relativ 23, 3 (2020) | 10.1007/s41114-020-00026-9 | LIGO-P1200087, VIR-0288A-12, JGW-P1808427 | gr-qc astro-ph.HE | http://creativecommons.org/licenses/by/4.0/ | We present our current best estimate of the plausible observing scenarios for
the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over
the next several years, with the intention of providing information to
facilitate planning for multi-messenger astronomy with gravitational waves. We
estimate the sensitivity of the network to transient gravitational-wave signals
for the third (O3), fourth (O4) and fifth observing (O5) runs, including the
planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study
the capability of the network to determine the sky location of the source for
gravitational-wave signals from the inspiral of binary systems of compact
objects, that is BNS, NSBH, and BBH systems. The ability to localize the
sources is given as a sky-area probability, luminosity distance, and comoving
volume. The median sky localization area (90\% credible region) is expected to
be a few hundreds of square degrees for all types of binary systems during O3
with the Advanced LIGO and Virgo (HLV) network. The median sky localization
area will improve to a few tens of square degrees during O4 with the Advanced
LIGO, Virgo, and KAGRA (HLVK) network. We evaluate sensitivity and localization
expectations for unmodeled signal searches, including the search for
intermediate mass black hole binary mergers.
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] | We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is BNS, NSBH, and BBH systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90\% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers. |
0706.3130 | Salvatore Capozziello | S. A. Ali, C. Cafaro, S. Capozziello, Ch. Corda | Abelian Magnetic Monopoles and Topologically Massive Vector Bosons in
Scalar-Tensor Gravity with Torsion Potential | 18 pages, no figures | Int. J. Mod. Phys. A23, 4315 (2008) | 10.1142/S0217751X08041438 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A Lagrangian formulation describing the electromagnetic interaction -
mediated by topologically massive vector bosons - between charged, spin-(1/2)
fermions with an abelian magnetic monopole in a curved spacetime with
non-minimal coupling and torsion potential is presented. The covariant field
equations are obtained. The issue of coexistence of massive photons and
magnetic monopoles is addressed in the present framework. It is found that
despite the topological nature of photon mass generation in curved spacetime
with isotropic dilaton field, the classical field theory describing the
nonrelativistic electromagnetic interaction between a point-like electric
charge and magnetic monopole is inconsistent.
| [
{
"created": "Thu, 21 Jun 2007 12:00:21 GMT",
"version": "v1"
},
{
"created": "Wed, 27 May 2009 16:02:32 GMT",
"version": "v2"
}
] | 2009-05-27 | [
[
"Ali",
"S. A.",
""
],
[
"Cafaro",
"C.",
""
],
[
"Capozziello",
"S.",
""
],
[
"Corda",
"Ch.",
""
]
] | A Lagrangian formulation describing the electromagnetic interaction - mediated by topologically massive vector bosons - between charged, spin-(1/2) fermions with an abelian magnetic monopole in a curved spacetime with non-minimal coupling and torsion potential is presented. The covariant field equations are obtained. The issue of coexistence of massive photons and magnetic monopoles is addressed in the present framework. It is found that despite the topological nature of photon mass generation in curved spacetime with isotropic dilaton field, the classical field theory describing the nonrelativistic electromagnetic interaction between a point-like electric charge and magnetic monopole is inconsistent. |
1807.02426 | Rodrigo Avalos | R. Avalos, I. P. Lobo, T. Sanomiya and C. Romero | On the Cauchy Problem for Weyl-Geometric Scalar-Tensor Theories of
Gravity | null | Journal of Mathematical Physics 59, 062502 (2018) | 10.1063/1.5017848 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, we analyse the well-posedness of the initial value formulation
for particular kinds of geometric scalar-tensor theories of gravity, which are
based on a Weyl integrable space-time. We will show that, within a
frame-invariant interpretation for the theory, the Cauchy problem in vacuum is
well-posed. We will analyse the global in space problem, and, furthermore, we
will show that geometric uniqueness holds for the solutions. We make contact
with Brans-Dicke theory, and by analysing the similarities with such models, we
highlight how some of our results can be translated to this well-known context,
where not all of these problems have been previously addressed.
| [
{
"created": "Fri, 6 Jul 2018 14:09:58 GMT",
"version": "v1"
}
] | 2018-07-09 | [
[
"Avalos",
"R.",
""
],
[
"Lobo",
"I. P.",
""
],
[
"Sanomiya",
"T.",
""
],
[
"Romero",
"C.",
""
]
] | In this paper, we analyse the well-posedness of the initial value formulation for particular kinds of geometric scalar-tensor theories of gravity, which are based on a Weyl integrable space-time. We will show that, within a frame-invariant interpretation for the theory, the Cauchy problem in vacuum is well-posed. We will analyse the global in space problem, and, furthermore, we will show that geometric uniqueness holds for the solutions. We make contact with Brans-Dicke theory, and by analysing the similarities with such models, we highlight how some of our results can be translated to this well-known context, where not all of these problems have been previously addressed. |
gr-qc/0105073 | Somasri Sen | Narayan Banerjee, Somasri Sen and Naresh Dadhich | On the detection of scalar hair | RevTex style, 4 pages, no figures | Mod.Phys.Lett. A16 (2001) 1223-1228 | 10.1142/S0217732301004388 | null | gr-qc | null | It is shown that the conclusion regarding the existence of a scalar hair for
a black hole in a nonminimally coupled self interacting scalar tensor theory
can be drawn from the that for a scalar field minimally coupled to gravity by
means of a conformal transformation.
| [
{
"created": "Sun, 20 May 2001 05:37:38 GMT",
"version": "v1"
}
] | 2009-11-07 | [
[
"Banerjee",
"Narayan",
""
],
[
"Sen",
"Somasri",
""
],
[
"Dadhich",
"Naresh",
""
]
] | It is shown that the conclusion regarding the existence of a scalar hair for a black hole in a nonminimally coupled self interacting scalar tensor theory can be drawn from the that for a scalar field minimally coupled to gravity by means of a conformal transformation. |
1306.2888 | Juan Luis P\'erez P\'erez | Juan L. Perez, Miguel A. Garcia-Aspeitia and L. Arturo Urena-Lopez | Cosmological solutions for a two-branes system in a vacuum bulk | null | null | 10.1063/1.4817055 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the cosmology for a two branes model in a space-time of five
dimensions where the extra coordinate is compactified on an orbifold. The
hidden brane is filled with a real scalar field endowed with a quadratic
potential that behaves as primordial dark matter field. This case is analyzed
when the radion effects are negligible in comparison with the density energy;
all possible solutions are found by means of a dynamical system approach.
| [
{
"created": "Wed, 12 Jun 2013 16:40:17 GMT",
"version": "v1"
}
] | 2015-06-16 | [
[
"Perez",
"Juan L.",
""
],
[
"Garcia-Aspeitia",
"Miguel A.",
""
],
[
"Urena-Lopez",
"L. Arturo",
""
]
] | We study the cosmology for a two branes model in a space-time of five dimensions where the extra coordinate is compactified on an orbifold. The hidden brane is filled with a real scalar field endowed with a quadratic potential that behaves as primordial dark matter field. This case is analyzed when the radion effects are negligible in comparison with the density energy; all possible solutions are found by means of a dynamical system approach. |
1003.5528 | Fabrizio De Marchi | M. Cerdonio, F. De Marchi, R. De Pietri, P. Jetzer, F. Marzari, G.
Mazzolo, A. Ortolan, M. Sereno | Modulation of LISA free-fall orbits due to the Earth-Moon system | 15 pages, 5 figures | Class.Quant.Grav.27:165007,2010 | 10.1088/0264-9381/27/16/165007 | null | gr-qc | http://creativecommons.org/licenses/by/3.0/ | We calculate the effect of the Earth-Moon (EM) system on the free-fall motion
of LISA test masses. We show that the periodic gravitational pulling of the EM
system induces a resonance with fundamental frequency 1 yr^-1 and a series of
periodic perturbations with frequencies equal to integer harmonics of the
synodic month (9.92 10^-7 Hz). We then evaluate the effects of these
perturbations (up to the 6th harmonics) on the relative motions between each
test masses couple, finding that they range between 3mm and 10pm for the 2nd
and 6th harmonic, respectively. If we take the LISA sensitivity curve, as
extrapolated down to 10^-6 Hz, we obtain that a few harmonics of the EM system
can be detected in the Doppler data collected by the LISA space mission. This
suggests that the EM system gravitational near field could provide an absolute
calibration for the LISA sensitivity at very low frequencies.
| [
{
"created": "Mon, 29 Mar 2010 12:59:26 GMT",
"version": "v1"
},
{
"created": "Wed, 9 Jun 2010 10:14:22 GMT",
"version": "v2"
}
] | 2014-11-20 | [
[
"Cerdonio",
"M.",
""
],
[
"De Marchi",
"F.",
""
],
[
"De Pietri",
"R.",
""
],
[
"Jetzer",
"P.",
""
],
[
"Marzari",
"F.",
""
],
[
"Mazzolo",
"G.",
""
],
[
"Ortolan",
"A.",
""
],
[
"Sereno",
"M.",
""
]
] | We calculate the effect of the Earth-Moon (EM) system on the free-fall motion of LISA test masses. We show that the periodic gravitational pulling of the EM system induces a resonance with fundamental frequency 1 yr^-1 and a series of periodic perturbations with frequencies equal to integer harmonics of the synodic month (9.92 10^-7 Hz). We then evaluate the effects of these perturbations (up to the 6th harmonics) on the relative motions between each test masses couple, finding that they range between 3mm and 10pm for the 2nd and 6th harmonic, respectively. If we take the LISA sensitivity curve, as extrapolated down to 10^-6 Hz, we obtain that a few harmonics of the EM system can be detected in the Doppler data collected by the LISA space mission. This suggests that the EM system gravitational near field could provide an absolute calibration for the LISA sensitivity at very low frequencies. |
1701.08719 | Yang Li | Yang Li and Daniele Oriti and Mingyi Zhang | Group field theory for quantum gravity minimally coupled to a scalar
field | 41 pages, 2 figures | null | 10.1088/1361-6382/aa85d2 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We construct a group field theory model for quantum gravity minimally coupled
to relativistic scalar fields, defining as well a corresponding discrete
gravity path integral (and, implicitly, a coupled spin foam model) in its
Feynman expansion. We also analyze a number of variations of the same model,
the corresponding discrete gravity path integrals, its generalization to the
coupling of multiple scalar fields and discuss its possible applications to the
extraction of effective cosmological dynamics from the full quantum gravity
formalism, in the context of group field theory condensate cosmology.
| [
{
"created": "Mon, 30 Jan 2017 17:35:58 GMT",
"version": "v1"
},
{
"created": "Wed, 8 Mar 2017 02:42:56 GMT",
"version": "v2"
},
{
"created": "Fri, 24 Mar 2017 09:03:27 GMT",
"version": "v3"
},
{
"created": "Sat, 1 Apr 2017 10:55:12 GMT",
"version": "v4"
}
] | 2017-09-27 | [
[
"Li",
"Yang",
""
],
[
"Oriti",
"Daniele",
""
],
[
"Zhang",
"Mingyi",
""
]
] | We construct a group field theory model for quantum gravity minimally coupled to relativistic scalar fields, defining as well a corresponding discrete gravity path integral (and, implicitly, a coupled spin foam model) in its Feynman expansion. We also analyze a number of variations of the same model, the corresponding discrete gravity path integrals, its generalization to the coupling of multiple scalar fields and discuss its possible applications to the extraction of effective cosmological dynamics from the full quantum gravity formalism, in the context of group field theory condensate cosmology. |
gr-qc/9703006 | Dr John W. Barrett | John W. Barrett | Sources of symmetric potentials | 4 pages, plain TeX, unpublished preprint from 1990, referred to in
gr-qc/9611051 | null | null | NCL-90 TP-16 | gr-qc | null | Laboratory experiments on gravitation are usually performed with objects of
constant density, so that the analysis of the forces concerns only the geometry
of their shape. In an ideal experiment, the shapes of the constituent parts
will be optimised to meet certain mathematical criteria, which ensure that the
experiment has maximal sensitivity.
Using this idea, the author suggested an experiment to determine the
departure of the gravitational force from Newton's force law [1]. The
geometrical problem which has to be solved is to find two shapes which differ
significantly, but have the same Newtonian potential. Essentially, the
experiment determines whether the two objects are distinguishable by their
gravitational force. Here, we consider the case when one of them is a round
ball. The result, Theorem 1, establishes a fact which appeared in numerical
simulations, that the second object has to have a hole in it.
| [
{
"created": "Mon, 3 Mar 1997 13:39:43 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Barrett",
"John W.",
""
]
] | Laboratory experiments on gravitation are usually performed with objects of constant density, so that the analysis of the forces concerns only the geometry of their shape. In an ideal experiment, the shapes of the constituent parts will be optimised to meet certain mathematical criteria, which ensure that the experiment has maximal sensitivity. Using this idea, the author suggested an experiment to determine the departure of the gravitational force from Newton's force law [1]. The geometrical problem which has to be solved is to find two shapes which differ significantly, but have the same Newtonian potential. Essentially, the experiment determines whether the two objects are distinguishable by their gravitational force. Here, we consider the case when one of them is a round ball. The result, Theorem 1, establishes a fact which appeared in numerical simulations, that the second object has to have a hole in it. |
2105.15188 | Zachary Nasipak | Zachary Nasipak and Charles R. Evans | Resonant self-force effects in extreme-mass-ratio binaries: A scalar
model | 32 pages, 15 figures; Updated to reflect published version | Phys. Rev. D 104, 084011 (2021) | 10.1103/PhysRevD.104.084011 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Extreme-mass ratio inspirals (EMRIs), compact binaries with small mass ratios
$\epsilon\ll 1$, will be important sources for low-frequency gravitational wave
detectors. Almost all EMRIs will evolve through important transient orbital
$r\theta$ resonances, which will enhance or diminish their gravitational wave
flux, thereby affecting the phase evolution of the waveforms at
$O(\epsilon^{1/2})$ relative to leading order. While modeling the local
gravitational self-force (GSF) during resonances is essential for generating
accurate EMRI waveforms, so far the full GSF has not been calculated for an
$r\theta$-resonant orbit owing to computational demands of the problem. As a
first step we employ a simpler model, calculating the scalar self-force (SSF)
along $r\theta$-resonant geodesics in Kerr spacetime. We demonstrate two ways
of calculating the $r\theta$-resonant SSF (and likely GSF), with one method
leaving the radial and polar motions initially independent as if the geodesic
is nonresonant. We illustrate results by calculating the SSF along geodesics
defined by three $r\theta$-resonant ratios (1:3, 1:2, 2:3). We show how the SSF
and averaged evolution of the orbital constants vary with the initial phase at
which an EMRI enters resonance. We then use our SSF data to test a previously
proposed integrability conjecture, which argues that conservative effects
vanish at adiabatic order during resonances. We find prominent contributions
from the conservative SSF to the secular evolution of the Carter constant,
$\langle \dot{\mathcal{Q}}\rangle$, but these nonvanishing contributions are on
the order of, or less than, the estimated uncertainties of our self-force
results. The uncertainties come from residual, incomplete removal of the
singular field in the regularization process. Higher order regularization
parameters, once available, will allow definitive tests of the integrability
conjecture.
| [
{
"created": "Mon, 31 May 2021 17:51:54 GMT",
"version": "v1"
},
{
"created": "Fri, 4 Jun 2021 18:52:21 GMT",
"version": "v2"
},
{
"created": "Mon, 4 Oct 2021 15:48:40 GMT",
"version": "v3"
}
] | 2021-10-05 | [
[
"Nasipak",
"Zachary",
""
],
[
"Evans",
"Charles R.",
""
]
] | Extreme-mass ratio inspirals (EMRIs), compact binaries with small mass ratios $\epsilon\ll 1$, will be important sources for low-frequency gravitational wave detectors. Almost all EMRIs will evolve through important transient orbital $r\theta$ resonances, which will enhance or diminish their gravitational wave flux, thereby affecting the phase evolution of the waveforms at $O(\epsilon^{1/2})$ relative to leading order. While modeling the local gravitational self-force (GSF) during resonances is essential for generating accurate EMRI waveforms, so far the full GSF has not been calculated for an $r\theta$-resonant orbit owing to computational demands of the problem. As a first step we employ a simpler model, calculating the scalar self-force (SSF) along $r\theta$-resonant geodesics in Kerr spacetime. We demonstrate two ways of calculating the $r\theta$-resonant SSF (and likely GSF), with one method leaving the radial and polar motions initially independent as if the geodesic is nonresonant. We illustrate results by calculating the SSF along geodesics defined by three $r\theta$-resonant ratios (1:3, 1:2, 2:3). We show how the SSF and averaged evolution of the orbital constants vary with the initial phase at which an EMRI enters resonance. We then use our SSF data to test a previously proposed integrability conjecture, which argues that conservative effects vanish at adiabatic order during resonances. We find prominent contributions from the conservative SSF to the secular evolution of the Carter constant, $\langle \dot{\mathcal{Q}}\rangle$, but these nonvanishing contributions are on the order of, or less than, the estimated uncertainties of our self-force results. The uncertainties come from residual, incomplete removal of the singular field in the regularization process. Higher order regularization parameters, once available, will allow definitive tests of the integrability conjecture. |
gr-qc/0309107 | Gaurav Khanna | Gaurav Khanna | Teukolsky evolution of particle orbits around Kerr black holes in the
time domain: elliptic and inclined orbits | 6 pages, 3 figures; submitted to PRD | Phys.Rev. D69 (2004) 024016 | 10.1103/PhysRevD.69.024016 | null | gr-qc | null | We extend the treatment of the problem of the gravitational waves produced by
a particle of negligible mass orbiting a Kerr black hole using black hole
perturbation theory in the time domain, to elliptic and inclined orbits. We
model the particle by smearing the singularities in the source term using
narrow Gaussian distributions. We compare results (energy and angular momentum
fluxes) for such orbits with those computed using the frequency domain
formalism.
| [
{
"created": "Mon, 22 Sep 2003 19:42:06 GMT",
"version": "v1"
}
] | 2009-11-10 | [
[
"Khanna",
"Gaurav",
""
]
] | We extend the treatment of the problem of the gravitational waves produced by a particle of negligible mass orbiting a Kerr black hole using black hole perturbation theory in the time domain, to elliptic and inclined orbits. We model the particle by smearing the singularities in the source term using narrow Gaussian distributions. We compare results (energy and angular momentum fluxes) for such orbits with those computed using the frequency domain formalism. |
1712.04092 | Thomas P. Kling | Thomas Kling, Kevin Roebuck, Eric Grotzke | Null Geodesics and Wave Front Singularities in the Godel Space-time | null | Gen Relativity Gravitation (2018) 50:7 | 10.1007/s10714-017-2328-2 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We explore wave fronts of null geodesics in the Godel metric emitted from
point sources both at, and away from, the origin. For constant time wave fronts
emitted by sources away from the origin, we find cusp ridges as well as blue
sky metamorphoses where spatially disconnected portions of the wave front
appear, connect to the main wave front, and then later break free and vanish.
These blue sky metamorphoses in the constant time wave fronts highlight the
non-causal features of the Godel metric. We introduce a concept of physical
distance along the null geodesics, and show that for wave fronts of constant
physical distance, the reorganization of the points making up the wave front
leads to the removal of cusp ridges.
| [
{
"created": "Tue, 12 Dec 2017 01:49:01 GMT",
"version": "v1"
}
] | 2017-12-13 | [
[
"Kling",
"Thomas",
""
],
[
"Roebuck",
"Kevin",
""
],
[
"Grotzke",
"Eric",
""
]
] | We explore wave fronts of null geodesics in the Godel metric emitted from point sources both at, and away from, the origin. For constant time wave fronts emitted by sources away from the origin, we find cusp ridges as well as blue sky metamorphoses where spatially disconnected portions of the wave front appear, connect to the main wave front, and then later break free and vanish. These blue sky metamorphoses in the constant time wave fronts highlight the non-causal features of the Godel metric. We introduce a concept of physical distance along the null geodesics, and show that for wave fronts of constant physical distance, the reorganization of the points making up the wave front leads to the removal of cusp ridges. |
1404.6210 | Victor Shchigolev Konstantinovich | V. K. Shchigolev | On Exact Cosmological Models of a Scalar Field in Lyra Geometry | 6 pages, no figures | Universal Journal of Physics and Application 1(4): 408-413, 2013 | 10.13189/ujpa.2013.010406 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Exact cosmological models for a scalar field in Lyra geometry are studied in
the presence of a time-varying effective cosmological term originated from the
specific interaction of an auxiliary $\Lambda$ - term with the displacement
vector. In this case, some exact solutions for the model equations are obtained
with the help of the so-called superpotential method (or the first-order
formalism). Some possible ways of further developing for such a model are
offered.
| [
{
"created": "Thu, 24 Apr 2014 18:08:46 GMT",
"version": "v1"
}
] | 2014-04-25 | [
[
"Shchigolev",
"V. K.",
""
]
] | Exact cosmological models for a scalar field in Lyra geometry are studied in the presence of a time-varying effective cosmological term originated from the specific interaction of an auxiliary $\Lambda$ - term with the displacement vector. In this case, some exact solutions for the model equations are obtained with the help of the so-called superpotential method (or the first-order formalism). Some possible ways of further developing for such a model are offered. |
2005.04752 | Cosimo Bambi | Bakhtiyor Narzilloev, Javlon Rayimbaev, Ahmadjon Abdujabbarov, Cosimo
Bambi | Charged particle motion around non-singular black holes in conformal
gravity in the presence of external magnetic field | 17 pages, 18 figures. v2: refereed version | Eur. Phys. J. C (2020) 80:1074 | 10.1140/epjc/s10052-020-08623-2 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We consider electromagnetic fields and charged particle dynamics around
non-singular black holes in conformal gravity immersed in an external,
asymptotically uniform magnetic field. First, we obtain analytic solutions of
the electromagnetic field equation around rotating non-singular black holes in
conformal gravity. We show that the radial components of the electric and
magnetic fields increase with the increase of the parameters $L$ and $N$ of the
black hole solution. Second, we study the dynamics of charged particles. We
show that the increase of the values of the parameters $L$ and $N$ and of
magnetic field causes a decrease in the radius of the innermost stable circular
orbits (ISCO) and the magnetic coupling parameter can mimic the effect of
conformal gravity giving the same ISCO radius up to $\omega_{\rm B}\leq 0.07$
when $N=3$.
| [
{
"created": "Sun, 10 May 2020 18:55:44 GMT",
"version": "v1"
},
{
"created": "Sat, 21 Nov 2020 23:53:07 GMT",
"version": "v2"
}
] | 2020-11-24 | [
[
"Narzilloev",
"Bakhtiyor",
""
],
[
"Rayimbaev",
"Javlon",
""
],
[
"Abdujabbarov",
"Ahmadjon",
""
],
[
"Bambi",
"Cosimo",
""
]
] | We consider electromagnetic fields and charged particle dynamics around non-singular black holes in conformal gravity immersed in an external, asymptotically uniform magnetic field. First, we obtain analytic solutions of the electromagnetic field equation around rotating non-singular black holes in conformal gravity. We show that the radial components of the electric and magnetic fields increase with the increase of the parameters $L$ and $N$ of the black hole solution. Second, we study the dynamics of charged particles. We show that the increase of the values of the parameters $L$ and $N$ and of magnetic field causes a decrease in the radius of the innermost stable circular orbits (ISCO) and the magnetic coupling parameter can mimic the effect of conformal gravity giving the same ISCO radius up to $\omega_{\rm B}\leq 0.07$ when $N=3$. |
2003.02304 | Ivan Agullo | Ivan Agullo, Javier Olmedo and V. Sreenath | Predictions for the CMB from an anisotropic quantum bounce | 5 pages, 4 figures, minor changes to match published version | Phys. Rev. Lett. 124, 251301 (2020) | 10.1103/PhysRevLett.124.251301 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We introduce an extension of the standard inflationary paradigm on which the
big bang singularity is replaced by an anisotropic bounce. Unlike in the big
bang model, cosmological perturbations find an adiabatic regime in the past. We
show that this scenario accounts for the observed quadrupolar modulation in the
temperature anisotropies of the cosmic microwave background (CMB), and we make
predictions for the remaining angular correlation functions E-E, B-B and T-E,
together with non-zero temperature-polarization correlations T-B and E-B, that
can be used to test our ideas. We base our calculations on the bounce predicted
by loop quantum cosmology, but our techniques and conclusions apply to other
bouncing models as well.
| [
{
"created": "Wed, 4 Mar 2020 19:41:09 GMT",
"version": "v1"
},
{
"created": "Thu, 9 Jul 2020 23:16:57 GMT",
"version": "v2"
}
] | 2020-07-13 | [
[
"Agullo",
"Ivan",
""
],
[
"Olmedo",
"Javier",
""
],
[
"Sreenath",
"V.",
""
]
] | We introduce an extension of the standard inflationary paradigm on which the big bang singularity is replaced by an anisotropic bounce. Unlike in the big bang model, cosmological perturbations find an adiabatic regime in the past. We show that this scenario accounts for the observed quadrupolar modulation in the temperature anisotropies of the cosmic microwave background (CMB), and we make predictions for the remaining angular correlation functions E-E, B-B and T-E, together with non-zero temperature-polarization correlations T-B and E-B, that can be used to test our ideas. We base our calculations on the bounce predicted by loop quantum cosmology, but our techniques and conclusions apply to other bouncing models as well. |
2005.13096 | A. Yu. Petrov | J. R. Nascimento, A. Yu. Petrov, P. J. Porfirio, A. R. Soares | Gravitational lensing in a black-bounce traversable wormhole spacetime | 15 pages, version accepted to PRD | Phys. Rev. D 102, 044021 (2020) | 10.1103/PhysRevD.102.044021 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work, we calculate the deflection angle of light in a spacetime that
interpolates between regular black holes and traversable wormholes, depending
on the free parameter of the metric. Afterwards, this angular deflection is
substituted into the lens equations which allows to obtain physically
measurable results, such as the position of the relativistic images and the
magnifications.
| [
{
"created": "Wed, 27 May 2020 00:23:29 GMT",
"version": "v1"
},
{
"created": "Sat, 25 Jul 2020 22:52:04 GMT",
"version": "v2"
}
] | 2020-08-11 | [
[
"Nascimento",
"J. R.",
""
],
[
"Petrov",
"A. Yu.",
""
],
[
"Porfirio",
"P. J.",
""
],
[
"Soares",
"A. R.",
""
]
] | In this work, we calculate the deflection angle of light in a spacetime that interpolates between regular black holes and traversable wormholes, depending on the free parameter of the metric. Afterwards, this angular deflection is substituted into the lens equations which allows to obtain physically measurable results, such as the position of the relativistic images and the magnifications. |
gr-qc/9804049 | Jean-Philippe Uzan du Darc | Nathalie Deruelle (DARC, Observatoire de Paris) and Jean-Philippe Uzan
(DARC, Observatoire de Paris) | Conservation Laws for Cosmological Perurbations | 7 pages, no figure, published in the Proceedings of the workshop on
Cosmology and Time Asymmetry, Peyresq, July 21-31,1996, Int. Jour. Theor.
Physics, 36, 2461 (1997) | Int.J.Theor.Phys. 36 (1997) 2461 | null | null | gr-qc | null | We briefly recall the problem of defining conserved quantities such as energy
in general relativity, and the solution by introducing a symmetric background.
We apply the general formalism to perturbed Robertson-Walker spacetimes with de
Sitter geometry as background. We relate the obtained conserved quantities to
Traschen's integral constraints and mention a few applications in cosmology.
| [
{
"created": "Tue, 21 Apr 1998 14:41:54 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Deruelle",
"Nathalie",
"",
"DARC, Observatoire de Paris"
],
[
"Uzan",
"Jean-Philippe",
"",
"DARC, Observatoire de Paris"
]
] | We briefly recall the problem of defining conserved quantities such as energy in general relativity, and the solution by introducing a symmetric background. We apply the general formalism to perturbed Robertson-Walker spacetimes with de Sitter geometry as background. We relate the obtained conserved quantities to Traschen's integral constraints and mention a few applications in cosmology. |
2009.11606 | Mohammad Ali Gorji | Mohammad Ali Gorji, Hayato Motohashi, Shinji Mukohyama | Stealth dark energy in scordatura DHOST theory | 33 pages, typos corrected, published version | null | 10.1088/1475-7516/2021/03/081 | YITP-20-118, IPMU20-0099 | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A stealth de Sitter solution in scalar-tensor theories has an exact de Sitter
background metric and a nontrivial scalar field profile. Recently, in the
context of Degenerate Higher-Order Scalar-Tensor (DHOST) theories it was shown
that stealth de Sitter solutions suffer from either infinite strong coupling or
gradient instability for scalar field perturbations. The sound speed squared is
either vanishing or negative. In the first case, the strong coupling scale is
zero and thus lower than the energy scale of any physical phenomena. From the
viewpoint of effective field theory, this issue is naturally resolved by
introducing a controlled detuning of the degeneracy condition dubbed
scordatura, recovering a version of ghost condensation. In this paper we
construct a viable dark energy model in the scordatura DHOST theory based on a
stealth cosmological solution, in which the metric is the same as in the
standard $\Lambda$CDM model and the scalar field profile is linearly
time-dependent. We show that the scordatura mechanism resolves the strong
coupling and gradient instability. Further, we find that the scordatura is also
necessary to make the quasi-static limit well-defined, which implies that the
subhorizon observables are inevitably affected by the scordatura. We derive the
effective gravitational coupling and the correction to the friction term for
the subhorizon evolution of the linear dark matter energy density contrast as
well as the Weyl potential and the gravitational slip parameter. In the absence
of the scordatura, the quasi-static approximation would break down at all
scales around stealth cosmological solutions even if the issue of the infinite
strong coupling is unjustly disregarded. Therefore previous estimations of the
subhorizon evolution of matter density contrast in modified gravity in the
literature need to be revisited by taking into account the scordatura effect.
| [
{
"created": "Thu, 24 Sep 2020 11:25:33 GMT",
"version": "v1"
},
{
"created": "Thu, 25 Mar 2021 02:46:21 GMT",
"version": "v2"
}
] | 2021-03-26 | [
[
"Gorji",
"Mohammad Ali",
""
],
[
"Motohashi",
"Hayato",
""
],
[
"Mukohyama",
"Shinji",
""
]
] | A stealth de Sitter solution in scalar-tensor theories has an exact de Sitter background metric and a nontrivial scalar field profile. Recently, in the context of Degenerate Higher-Order Scalar-Tensor (DHOST) theories it was shown that stealth de Sitter solutions suffer from either infinite strong coupling or gradient instability for scalar field perturbations. The sound speed squared is either vanishing or negative. In the first case, the strong coupling scale is zero and thus lower than the energy scale of any physical phenomena. From the viewpoint of effective field theory, this issue is naturally resolved by introducing a controlled detuning of the degeneracy condition dubbed scordatura, recovering a version of ghost condensation. In this paper we construct a viable dark energy model in the scordatura DHOST theory based on a stealth cosmological solution, in which the metric is the same as in the standard $\Lambda$CDM model and the scalar field profile is linearly time-dependent. We show that the scordatura mechanism resolves the strong coupling and gradient instability. Further, we find that the scordatura is also necessary to make the quasi-static limit well-defined, which implies that the subhorizon observables are inevitably affected by the scordatura. We derive the effective gravitational coupling and the correction to the friction term for the subhorizon evolution of the linear dark matter energy density contrast as well as the Weyl potential and the gravitational slip parameter. In the absence of the scordatura, the quasi-static approximation would break down at all scales around stealth cosmological solutions even if the issue of the infinite strong coupling is unjustly disregarded. Therefore previous estimations of the subhorizon evolution of matter density contrast in modified gravity in the literature need to be revisited by taking into account the scordatura effect. |
1211.2562 | Iver Brevik | Iver Brevik | Viscosity in modified gravity | 9 pages, no figure; reference list updated and expanded | Entropy 2012, 14, 2302-2310 | 10.3390/e14112302 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A bulk viscosity is introduced in the formalism of modified gravity. It is
shown that, on the basis of a natural scaling law for the viscosity, a simple
solution can be found for quantities such as the Hubble parameter and the
energy density. These solutions may incorporate a viscosity-induced Big Rip
singularity. By introducing a phase transition in the cosmic fluid, the future
singularity can nevertheless in principle be avoided.
| [
{
"created": "Mon, 12 Nov 2012 10:58:32 GMT",
"version": "v1"
},
{
"created": "Fri, 23 Nov 2012 14:49:02 GMT",
"version": "v2"
}
] | 2012-11-26 | [
[
"Brevik",
"Iver",
""
]
] | A bulk viscosity is introduced in the formalism of modified gravity. It is shown that, on the basis of a natural scaling law for the viscosity, a simple solution can be found for quantities such as the Hubble parameter and the energy density. These solutions may incorporate a viscosity-induced Big Rip singularity. By introducing a phase transition in the cosmic fluid, the future singularity can nevertheless in principle be avoided. |
1707.06141 | Jacques Smulevici | David Fajman, J\'er\'emie Joudioux and Jacques Smulevici | The Stability of the Minkowski space for the Einstein-Vlasov system | 139 pages | Analysis & PDE 14 (2021) 425-531 | 10.2140/apde.2021.14.425 | null | gr-qc math-ph math.AP math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We prove the global stability of the Minkowski space viewed as the trivial
solution of the Einstein-Vlasov system. To estimate the Vlasov field, we use
the vector field and modified vector field techniques developed in [FJS15;
FJS17]. In particular, the initial support in the velocity variable does not
need to be compact. To control the effect of the large velocities, we identify
and exploit several structural properties of the Vlasov equation to prove that
the worst non-linear terms in the Vlasov equation either enjoy a form of the
null condition or can be controlled using the wave coordinate gauge. The basic
propagation estimates for the Vlasov field are then obtained using only weak
interior decay for the metric components. Since some of the error terms are not
time-integrable, several hierarchies in the commuted equations are exploited to
close the top order estimates. For the Einstein equations, we use wave
coordinates and the main new difficulty arises from the commutation of the
energy-momentum tensor, which needs to be rewritten using the modified vector
fields.
| [
{
"created": "Wed, 19 Jul 2017 15:10:21 GMT",
"version": "v1"
}
] | 2021-03-24 | [
[
"Fajman",
"David",
""
],
[
"Joudioux",
"Jérémie",
""
],
[
"Smulevici",
"Jacques",
""
]
] | We prove the global stability of the Minkowski space viewed as the trivial solution of the Einstein-Vlasov system. To estimate the Vlasov field, we use the vector field and modified vector field techniques developed in [FJS15; FJS17]. In particular, the initial support in the velocity variable does not need to be compact. To control the effect of the large velocities, we identify and exploit several structural properties of the Vlasov equation to prove that the worst non-linear terms in the Vlasov equation either enjoy a form of the null condition or can be controlled using the wave coordinate gauge. The basic propagation estimates for the Vlasov field are then obtained using only weak interior decay for the metric components. Since some of the error terms are not time-integrable, several hierarchies in the commuted equations are exploited to close the top order estimates. For the Einstein equations, we use wave coordinates and the main new difficulty arises from the commutation of the energy-momentum tensor, which needs to be rewritten using the modified vector fields. |
2204.09490 | Farook Rahaman | S S De, Farook Rahaman, Antara Mapdar | Geometrical Origin of Growth of Matter Perturbations | 5 pages. 1 figure | null | null | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | The density perturbation of the universe has been considered in the framework
of a Finslerian cosmological model in which the background spacetime of the
universe is taken as the spatially flat FLRW spacetime with a Finslerian
perturbation. The inhomogeneity in the matter(energy) density arises naturally
in this consideration of gravity in the $( \alpha, \beta)$ - Finsler space for
the background spacetime of the universe. The resulting inhomogeneous matter
density indicates matter perturbation departing from the uniform density, and
it is caused by the Finslerian perturbation in the Riemannian spacetime, thus
ascertaining the geometrical origin of the growth of matter perturbation.
| [
{
"created": "Tue, 19 Apr 2022 15:18:44 GMT",
"version": "v1"
}
] | 2022-04-21 | [
[
"De",
"S S",
""
],
[
"Rahaman",
"Farook",
""
],
[
"Mapdar",
"Antara",
""
]
] | The density perturbation of the universe has been considered in the framework of a Finslerian cosmological model in which the background spacetime of the universe is taken as the spatially flat FLRW spacetime with a Finslerian perturbation. The inhomogeneity in the matter(energy) density arises naturally in this consideration of gravity in the $( \alpha, \beta)$ - Finsler space for the background spacetime of the universe. The resulting inhomogeneous matter density indicates matter perturbation departing from the uniform density, and it is caused by the Finslerian perturbation in the Riemannian spacetime, thus ascertaining the geometrical origin of the growth of matter perturbation. |
1912.13432 | Plamen Fiziev | Plamen P. Fiziev | New Results for Quasi Normal Modes of Gravitational Waves | 9 pages, 4 figures | null | null | SU-2019_11 | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We briefly consider the data of collaboration LIGO/VIRGO for gravitational
waves (GW) and the recent observations of Event Horizon Telescope (EHT), and we
discuss difficulties for finding the right theory of gravity and the nature of
the observed Extremely Compact Objects (ECOs). The only undisputable way to
establish existence of event horizon of ECOs, is the extraction of Quasi Normal
Modes (QNMs) from the ringing phase of the sources of GW. We present our method
for calculation of QNMs of GW in the Schwarzschild metric with different
boundary conditions. It is based on exact solutions of the Regge-Wheeler and
Zerilli equations in terms of the confluent Heun functions. We present also new
numerical results of high precision ($ \geq 16$ digits) for QNM frequencies. We
indicate the difficulties for comparison of theoretical results for QNMs with
the observations.
| [
{
"created": "Tue, 31 Dec 2019 17:10:21 GMT",
"version": "v1"
}
] | 2020-01-01 | [
[
"Fiziev",
"Plamen P.",
""
]
] | We briefly consider the data of collaboration LIGO/VIRGO for gravitational waves (GW) and the recent observations of Event Horizon Telescope (EHT), and we discuss difficulties for finding the right theory of gravity and the nature of the observed Extremely Compact Objects (ECOs). The only undisputable way to establish existence of event horizon of ECOs, is the extraction of Quasi Normal Modes (QNMs) from the ringing phase of the sources of GW. We present our method for calculation of QNMs of GW in the Schwarzschild metric with different boundary conditions. It is based on exact solutions of the Regge-Wheeler and Zerilli equations in terms of the confluent Heun functions. We present also new numerical results of high precision ($ \geq 16$ digits) for QNM frequencies. We indicate the difficulties for comparison of theoretical results for QNMs with the observations. |
2207.04417 | Christian Ecker | Christian Ecker and Luciano Rezzolla | A general, scale-independent description of the sound speed in neutron
stars | 7 pages, 4 figures, 1 appendix, version published in ApJL | Astrophys.J.Lett. 939 (2022) 2, L35 | 10.3847/2041-8213/ac8674 | null | gr-qc astro-ph.HE nucl-th | http://creativecommons.org/licenses/by/4.0/ | Using more than a million randomly generated equations of state that satisfy
theoretical and observational constraints we construct a novel,
scale-independent description of the sound speed in neutron stars where the
latter is expressed in a unit-cube spanning the normalised radius, $r/R$, and
the mass normalized to the maximum one, $M/M_{\rm TOV}$. From this generic
representation, a number of interesting and surprising results can be deduced.
In particular, we find that light (heavy) stars have stiff (soft) cores and
soft (stiff) outer layers, respectively, or that the maximum of the sound speed
is located at the center of light stars but moves to the outer layers for stars
with $M/M_{\rm
TOV}\gtrsim0.7$, reaching a constant value of $c_s^2=1/2$ as $M\to M_{\rm
TOV}$. We also show that the sound speed decreases below the conformal limit
$c_s^2=1/3$ at the center of stars with $M=M_{\rm
TOV}$. Finally, we construct an analytic expression that accurately describes
the radial dependence of the sound speed as a function of the neutron-star
mass, thus providing an estimate of the maximum sound speed expected in a
neutron star.
| [
{
"created": "Sun, 10 Jul 2022 08:36:52 GMT",
"version": "v1"
},
{
"created": "Sat, 3 Dec 2022 13:05:57 GMT",
"version": "v2"
}
] | 2022-12-07 | [
[
"Ecker",
"Christian",
""
],
[
"Rezzolla",
"Luciano",
""
]
] | Using more than a million randomly generated equations of state that satisfy theoretical and observational constraints we construct a novel, scale-independent description of the sound speed in neutron stars where the latter is expressed in a unit-cube spanning the normalised radius, $r/R$, and the mass normalized to the maximum one, $M/M_{\rm TOV}$. From this generic representation, a number of interesting and surprising results can be deduced. In particular, we find that light (heavy) stars have stiff (soft) cores and soft (stiff) outer layers, respectively, or that the maximum of the sound speed is located at the center of light stars but moves to the outer layers for stars with $M/M_{\rm TOV}\gtrsim0.7$, reaching a constant value of $c_s^2=1/2$ as $M\to M_{\rm TOV}$. We also show that the sound speed decreases below the conformal limit $c_s^2=1/3$ at the center of stars with $M=M_{\rm TOV}$. Finally, we construct an analytic expression that accurately describes the radial dependence of the sound speed as a function of the neutron-star mass, thus providing an estimate of the maximum sound speed expected in a neutron star. |
1611.03732 | Mauro Pieroni | Mauro Pieroni | Classification of inflationary models and constraints on fundamental
physics | PhD thesis, 2016, Univ Paris Diderot | null | null | null | gr-qc astro-ph.CO hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | This work is focused on the study of early time cosmology and in particular
on the study of inflation. After an introduction on the standard Big Bang
theory, we discuss the physics of CMB and we explain how its observations can
be used to set constraints on cosmological models. We introduce inflation and
we carry out its simplest realization by presenting the observables and the
experimental constraints that can be set on inflationary models. The
possibility of observing primordial gravitational waves (GWs) produced during
inflation is discussed. We present the reasons to define a classification of
inflationary models and introduce the \beta-function formalism for inflation by
explaining why in this framework we can naturally define a set of universality
classes for inflationary models. Theoretical motivations to support the
formulation of inflation in terms of this formalism are presented. Some
generalized models of inflation are introduced and the extension of the
\beta-function formalism for inflation to these models is discussed. Finally we
focus on the study of models where the (pseudo-scalar) inflaton is coupled to
some Abelian gauge fields that can be present during inflation. The analysis of
the problem is carried out by using a characterization of inflationary models
in terms of their asymptotic behavior. A wide set of theoretical aspects and of
observational consequences is discussed.
| [
{
"created": "Fri, 11 Nov 2016 15:31:49 GMT",
"version": "v1"
}
] | 2016-11-14 | [
[
"Pieroni",
"Mauro",
""
]
] | This work is focused on the study of early time cosmology and in particular on the study of inflation. After an introduction on the standard Big Bang theory, we discuss the physics of CMB and we explain how its observations can be used to set constraints on cosmological models. We introduce inflation and we carry out its simplest realization by presenting the observables and the experimental constraints that can be set on inflationary models. The possibility of observing primordial gravitational waves (GWs) produced during inflation is discussed. We present the reasons to define a classification of inflationary models and introduce the \beta-function formalism for inflation by explaining why in this framework we can naturally define a set of universality classes for inflationary models. Theoretical motivations to support the formulation of inflation in terms of this formalism are presented. Some generalized models of inflation are introduced and the extension of the \beta-function formalism for inflation to these models is discussed. Finally we focus on the study of models where the (pseudo-scalar) inflaton is coupled to some Abelian gauge fields that can be present during inflation. The analysis of the problem is carried out by using a characterization of inflationary models in terms of their asymptotic behavior. A wide set of theoretical aspects and of observational consequences is discussed. |
gr-qc/0508098 | Andrew Moylan | A. Moylan, S.M. Scott and A.C. Searle | Developments in GRworkbench | 14 pages. To appear A. Moylan, S.M. Scott and A.C. Searle,
Developments in GRworkbench. Proceedings of the Tenth Marcel Grossmann
Meeting on General Relativity, editors M. Novello, S. Perez-Bergliaffa and R.
Ruffini. Singapore: World Scientific 2005 | null | 10.1142/9789812704030_0019 | null | gr-qc | null | The software tool GRworkbench is an ongoing project in visual, numerical
General Relativity at The Australian National University. Recently, GRworkbench
has been significantly extended to facilitate numerical experimentation in
analytically-defined space-times. The numerical differential geometric engine
has been rewritten using functional programming techniques, enabling objects
which are normally defined as functions in the formalism of differential
geometry and General Relativity to be directly represented as function
variables in the C++ code of GRworkbench. The new functional differential
geometric engine allows for more accurate and efficient visualisation of
objects in space-times and makes new, efficient computational techniques
available. Motivated by the desire to investigate a recent scientific claim
using GRworkbench, new tools for numerical experimentation have been
implemented, allowing for the simulation of complex physical situations.
| [
{
"created": "Wed, 24 Aug 2005 03:26:07 GMT",
"version": "v1"
}
] | 2016-11-09 | [
[
"Moylan",
"A.",
""
],
[
"Scott",
"S. M.",
""
],
[
"Searle",
"A. C.",
""
]
] | The software tool GRworkbench is an ongoing project in visual, numerical General Relativity at The Australian National University. Recently, GRworkbench has been significantly extended to facilitate numerical experimentation in analytically-defined space-times. The numerical differential geometric engine has been rewritten using functional programming techniques, enabling objects which are normally defined as functions in the formalism of differential geometry and General Relativity to be directly represented as function variables in the C++ code of GRworkbench. The new functional differential geometric engine allows for more accurate and efficient visualisation of objects in space-times and makes new, efficient computational techniques available. Motivated by the desire to investigate a recent scientific claim using GRworkbench, new tools for numerical experimentation have been implemented, allowing for the simulation of complex physical situations. |
gr-qc/0206010 | Gaurav Khanna | Gaurav Khanna | Collision of spinning black holes in the close limit: The parallel spin
case | 10 pages, 3 figures. Final version (to appear in PRD) | Phys.Rev. D66 (2002) 064004 | 10.1103/PhysRevD.66.064004 | null | gr-qc | null | In this paper we consider the collision of black holes with parallel spins
using first order perturbation theory of rotating black holes (Teukolsky
formalism). The black holes are assumed to be close to each other, initially
non boosted and spinning slowly. We estimate the properties of the
gravitational radiation released from such an collision. The same problem was
studied recently by Gleiser {\em et al.} in the context of the Zerilli
perturbation formalism and our results for waveforms, energy and angular
momentum radiated agree very well with the results presented in that work.
| [
{
"created": "Mon, 3 Jun 2002 23:26:37 GMT",
"version": "v1"
},
{
"created": "Fri, 23 Aug 2002 13:17:53 GMT",
"version": "v2"
}
] | 2009-11-07 | [
[
"Khanna",
"Gaurav",
""
]
] | In this paper we consider the collision of black holes with parallel spins using first order perturbation theory of rotating black holes (Teukolsky formalism). The black holes are assumed to be close to each other, initially non boosted and spinning slowly. We estimate the properties of the gravitational radiation released from such an collision. The same problem was studied recently by Gleiser {\em et al.} in the context of the Zerilli perturbation formalism and our results for waveforms, energy and angular momentum radiated agree very well with the results presented in that work. |
0712.3846 | Piotr T. Chru\'sciel | Piotr T. Chru\'sciel and Paul Tod | On Mason's rigidity theorem | minor typos corrected | Commun.Math.Phys.285:1-29,2009 | 10.1007/s00220-008-0643-x | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Following an argument proposed by Mason, we prove that there are no
algebraically special asymptotically simple vacuum space-times with a smooth,
shear-free, geodesic congruence of principal null directions extending
transversally to a cross-section of Scri. Our analysis leaves the door open for
escaping this conclusion if the congruence is not smooth, or not transverse to
Scri. One of the elements of the proof is a new rigidity theorem for the
Trautman-Bondi mass.
| [
{
"created": "Sat, 22 Dec 2007 10:43:39 GMT",
"version": "v1"
},
{
"created": "Sat, 4 Oct 2008 08:36:00 GMT",
"version": "v2"
}
] | 2008-12-18 | [
[
"Chruściel",
"Piotr T.",
""
],
[
"Tod",
"Paul",
""
]
] | Following an argument proposed by Mason, we prove that there are no algebraically special asymptotically simple vacuum space-times with a smooth, shear-free, geodesic congruence of principal null directions extending transversally to a cross-section of Scri. Our analysis leaves the door open for escaping this conclusion if the congruence is not smooth, or not transverse to Scri. One of the elements of the proof is a new rigidity theorem for the Trautman-Bondi mass. |
1601.03862 | Del Rajan | Del Rajan | Complex Spacetimes and the Newman-Janis trick | 128 pages, Victoria University of Wellington | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this thesis, we explore the subject of complex spacetimes, in which the
mathematical theory of complex manifolds gets modified for application to
General Relativity. We will also explore the mysterious Newman-Janis trick,
which is an elementary and quite short method to obtain the Kerr black hole
from the Schwarzschild black hole through the use of complex variables. This
exposition will cover variations of the Newman-Janis trick, partial
explanations, as well as original contributions
| [
{
"created": "Fri, 15 Jan 2016 10:16:43 GMT",
"version": "v1"
},
{
"created": "Sat, 25 Mar 2017 23:21:03 GMT",
"version": "v2"
}
] | 2017-03-28 | [
[
"Rajan",
"Del",
""
]
] | In this thesis, we explore the subject of complex spacetimes, in which the mathematical theory of complex manifolds gets modified for application to General Relativity. We will also explore the mysterious Newman-Janis trick, which is an elementary and quite short method to obtain the Kerr black hole from the Schwarzschild black hole through the use of complex variables. This exposition will cover variations of the Newman-Janis trick, partial explanations, as well as original contributions |
2401.02898 | Fech Scen Khoo | Fech Scen Khoo, Bahareh Azad, Jose Luis Bl\'azquez-Salcedo, Luis
Manuel Gonz\'alez-Romero, Burkhard Kleihaus, Jutta Kunz, Francisco
Navarro-L\'erida | Quasinormal modes of rapidly rotating Ellis-Bronnikov wormholes | 19 pages, 4 figures, 3 tables; v2: equations added, results
unchanged, matches published version | Phys. Rev. D 109, 084013 (2024) | 10.1103/PhysRevD.109.084013 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present for the first time a study of the quasinormal modes of rapidly
rotating Ellis-Bronnikov wormholes in General Relativity. We compute the
spectrum of the wormholes using a spectral decomposition of the metric
perturbations on a numerical background. We focus on the $M_z=2,3$ sector of
the perturbations, and show that the triple isospectrality of the symmetric and
static Ellis-Bronnikov wormhole is broken due to rotation, giving rise to a
much richer spectrum than the spectrum of Kerr black holes. We do not find any
instabilities for $M_z=2,3$ perturbations.
| [
{
"created": "Fri, 5 Jan 2024 17:00:05 GMT",
"version": "v1"
},
{
"created": "Mon, 8 Apr 2024 15:34:22 GMT",
"version": "v2"
}
] | 2024-04-09 | [
[
"Khoo",
"Fech Scen",
""
],
[
"Azad",
"Bahareh",
""
],
[
"Blázquez-Salcedo",
"Jose Luis",
""
],
[
"González-Romero",
"Luis Manuel",
""
],
[
"Kleihaus",
"Burkhard",
""
],
[
"Kunz",
"Jutta",
""
],
[
"Navarro-Lérida",
"Francisco",
""
]
] | We present for the first time a study of the quasinormal modes of rapidly rotating Ellis-Bronnikov wormholes in General Relativity. We compute the spectrum of the wormholes using a spectral decomposition of the metric perturbations on a numerical background. We focus on the $M_z=2,3$ sector of the perturbations, and show that the triple isospectrality of the symmetric and static Ellis-Bronnikov wormhole is broken due to rotation, giving rise to a much richer spectrum than the spectrum of Kerr black holes. We do not find any instabilities for $M_z=2,3$ perturbations. |
gr-qc/0606045 | Frank B. Estabrook | Frank B. Estabrook | Classic field theories of gravitation embedded in ten dimensions | 6 pages | null | null | null | gr-qc | null | Two classic field theories of metric gravitation are given as
constant-coefficient Exterior Differential Systems (EDS) on the flat
orthonormal frame bundle over ten dimensional space. They are derivable by
variation of Cartan 4-forms, and shown to be well-posed by calculation of their
Cartan characteristic integers. Their solutions are embedded Riemannian
4-spaces. The first theory is generated by torsion 2-forms and Ricci-flat
3-forms and is a constant-coefficient EDS for vacuum tetrad gravity; its Cartan
character table is the same as found for an EDS recently given in terms of
tetrad frame and connection variables [1] [2]. The second constant-coefficient
EDS is generated solely by 2-forms, and has a Cartan form of quadratic
Yang-Mills type. Its solutions lie in torsion free 6-spaces and are fibered
over 3-spaces. We conjecture that these solutions may be classically related to
10-dimensional quantum field theoretic constructions of cosmological vacua [3].
| [
{
"created": "Fri, 9 Jun 2006 21:02:26 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Estabrook",
"Frank B.",
""
]
] | Two classic field theories of metric gravitation are given as constant-coefficient Exterior Differential Systems (EDS) on the flat orthonormal frame bundle over ten dimensional space. They are derivable by variation of Cartan 4-forms, and shown to be well-posed by calculation of their Cartan characteristic integers. Their solutions are embedded Riemannian 4-spaces. The first theory is generated by torsion 2-forms and Ricci-flat 3-forms and is a constant-coefficient EDS for vacuum tetrad gravity; its Cartan character table is the same as found for an EDS recently given in terms of tetrad frame and connection variables [1] [2]. The second constant-coefficient EDS is generated solely by 2-forms, and has a Cartan form of quadratic Yang-Mills type. Its solutions lie in torsion free 6-spaces and are fibered over 3-spaces. We conjecture that these solutions may be classically related to 10-dimensional quantum field theoretic constructions of cosmological vacua [3]. |
gr-qc/0001086 | Manuel H. Tiglio | Manuel H. Tiglio | How much energy do closed timelike curves in 2+1 spacetimes need? | 3 pages, with no figures. Accepted in PRD as Rapid Communication | Phys.Rev.D61:081503,2000 | 10.1103/PhysRevD.61.081503 | null | gr-qc | null | By noticing that, in open 2+1 gravity, polarized surfaces cannot converge in
the presence of timelike total energy momentum (except for a rotation of 2 pi),
we give a simple argument which shows that, quite generally, closed timelike
curves cannot exist in the presence of such energy condition.
| [
{
"created": "Thu, 27 Jan 2000 00:32:15 GMT",
"version": "v1"
}
] | 2009-12-30 | [
[
"Tiglio",
"Manuel H.",
""
]
] | By noticing that, in open 2+1 gravity, polarized surfaces cannot converge in the presence of timelike total energy momentum (except for a rotation of 2 pi), we give a simple argument which shows that, quite generally, closed timelike curves cannot exist in the presence of such energy condition. |
0901.3207 | Ion I. Cot{\ba}escu | Ion I. Cotaescu | Polarized vector bosons on the de Sitter expanding universe | 17 pages no figures | Gen.Rel.Grav.42:861-876,2010 | 10.1007/s10714-009-0886-7 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The quantum theory of the vector field minimally coupled to the gravity of
the de Sitter spacetime is built in a canonical manner starting with a new
complete set of quantum modes of given momentum and helicity derived in the
moving chart of conformal time. It is shown that the canonical quantization
leads to new vector propagators which satisfy similar equations as the
propagators derived by Tsamis and Woodard [{\em J.Math.Phys.} {\bf 48} (2007)
052306] but having a different structure. The one-particle operators are also
written down pointing out that their properties are similar with those found
already in the quantum theory of the scalar, Dirac and Maxwell free fields.
| [
{
"created": "Wed, 21 Jan 2009 09:06:18 GMT",
"version": "v1"
},
{
"created": "Sun, 15 Mar 2009 06:47:38 GMT",
"version": "v2"
},
{
"created": "Fri, 11 Sep 2009 06:27:02 GMT",
"version": "v3"
}
] | 2010-04-14 | [
[
"Cotaescu",
"Ion I.",
""
]
] | The quantum theory of the vector field minimally coupled to the gravity of the de Sitter spacetime is built in a canonical manner starting with a new complete set of quantum modes of given momentum and helicity derived in the moving chart of conformal time. It is shown that the canonical quantization leads to new vector propagators which satisfy similar equations as the propagators derived by Tsamis and Woodard [{\em J.Math.Phys.} {\bf 48} (2007) 052306] but having a different structure. The one-particle operators are also written down pointing out that their properties are similar with those found already in the quantum theory of the scalar, Dirac and Maxwell free fields. |
0908.0337 | Thomas W. Baumgarte | Jason D. Immerman and Thomas W. Baumgarte | Trumpet-puncture initial data for black holes | 6 pages, 5 figures, published version | Phys.Rev.D80:061501,2009 | 10.1103/PhysRevD.80.061501 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We propose a new approach, based on the puncture method, to construct black
hole initial data in the so-called trumpet geometry, i.e. on slices that
asymptote to a limiting surface of non-zero areal radius. Our approach is easy
to implement numerically and, at least for non-spinning black holes, does not
require any internal boundary conditions. We present numerical results,
obtained with a uniform-grid finite-difference code, for boosted black holes
and binary black holes. We also comment on generalizations of this method for
spinning black holes.
| [
{
"created": "Mon, 3 Aug 2009 20:11:46 GMT",
"version": "v1"
},
{
"created": "Thu, 1 Oct 2009 21:33:47 GMT",
"version": "v2"
}
] | 2009-10-20 | [
[
"Immerman",
"Jason D.",
""
],
[
"Baumgarte",
"Thomas W.",
""
]
] | We propose a new approach, based on the puncture method, to construct black hole initial data in the so-called trumpet geometry, i.e. on slices that asymptote to a limiting surface of non-zero areal radius. Our approach is easy to implement numerically and, at least for non-spinning black holes, does not require any internal boundary conditions. We present numerical results, obtained with a uniform-grid finite-difference code, for boosted black holes and binary black holes. We also comment on generalizations of this method for spinning black holes. |
1512.06977 | Atsushi Naruko | Atsushi Naruko, Daisuke Yoshida and Shinji Mukohyama | Gravitational scalar-tensor theory | 6 pages | null | 10.1088/0264-9381/33/9/09LT01 | YITP-15-117, IPMU 15-0211 | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We consider a new form of theories of gravity in which the action is written
in terms of the Ricci scalar and its first and second derivatives. Despite the
higher derivative nature of the action, the theory is free from ghost under an
appropriate choice of the functional form of the Lagrangian. This model
possesses $2+2$ physical degrees of freedom, namely $2$ scalar degrees and $2$
tensor degrees. We exhaust all such theories with the Lagrangian of the form
$f(R, (\nabla R)^2, \Box R)$, where $R$ is the Ricci scalar, and then show some
examples beyond this ansatz. In course of analysis, we prove the equivalence
between these examples and generalized bi-Galileon theories.
| [
{
"created": "Tue, 22 Dec 2015 07:48:11 GMT",
"version": "v1"
},
{
"created": "Tue, 23 Apr 2019 02:07:24 GMT",
"version": "v2"
}
] | 2019-04-24 | [
[
"Naruko",
"Atsushi",
""
],
[
"Yoshida",
"Daisuke",
""
],
[
"Mukohyama",
"Shinji",
""
]
] | We consider a new form of theories of gravity in which the action is written in terms of the Ricci scalar and its first and second derivatives. Despite the higher derivative nature of the action, the theory is free from ghost under an appropriate choice of the functional form of the Lagrangian. This model possesses $2+2$ physical degrees of freedom, namely $2$ scalar degrees and $2$ tensor degrees. We exhaust all such theories with the Lagrangian of the form $f(R, (\nabla R)^2, \Box R)$, where $R$ is the Ricci scalar, and then show some examples beyond this ansatz. In course of analysis, we prove the equivalence between these examples and generalized bi-Galileon theories. |
gr-qc/0302069 | Grigori Volovik | G.E. Volovik | Evolution of cosmological constant in effective gravity | LaTeX file, 5 pages, no figures, version submitted to JETP Letters | Pisma Zh.Eksp.Teor.Fiz. 77 (2003) 407-411; JETP Lett. 77 (2003)
339-343 | 10.1134/1.1581956 | null | gr-qc cond-mat hep-ph | null | In contrast to the phenomenon of nullification of the cosmological constant
in the equilibrium vacuum, which is the general property of any quantum vacuum,
there are many options in modifying the Einstein equation to allow the
cosmological constant to evolve in a non-equilibrium vacuum. An attempt is made
to extend the Einstein equation in the direction suggested by the
condensed-matter analogy of the quantum vacuum. Different scenarios are found
depending on the behavior of and the relation between the relaxation parameters
involved, some of these scenarios having been discussed in the literature. One
of them reproduces the scenario in which the effective cosmological constant
emerges as a constant of integration. The second one describes the situation,
when after the cosmological phase transition the cosmological constant drops
from zero to the negative value; this scenario describes the relaxation from
this big negative value back to zero and then to a small positive value. In the
third example the relaxation time is not a constant but depends on matter; this
scenario demonstrates that the vacuum energy (or its fraction) can play the
role of the cold dark matter.
| [
{
"created": "Mon, 17 Feb 2003 15:57:49 GMT",
"version": "v1"
},
{
"created": "Wed, 5 Mar 2003 12:40:32 GMT",
"version": "v2"
}
] | 2009-11-10 | [
[
"Volovik",
"G. E.",
""
]
] | In contrast to the phenomenon of nullification of the cosmological constant in the equilibrium vacuum, which is the general property of any quantum vacuum, there are many options in modifying the Einstein equation to allow the cosmological constant to evolve in a non-equilibrium vacuum. An attempt is made to extend the Einstein equation in the direction suggested by the condensed-matter analogy of the quantum vacuum. Different scenarios are found depending on the behavior of and the relation between the relaxation parameters involved, some of these scenarios having been discussed in the literature. One of them reproduces the scenario in which the effective cosmological constant emerges as a constant of integration. The second one describes the situation, when after the cosmological phase transition the cosmological constant drops from zero to the negative value; this scenario describes the relaxation from this big negative value back to zero and then to a small positive value. In the third example the relaxation time is not a constant but depends on matter; this scenario demonstrates that the vacuum energy (or its fraction) can play the role of the cold dark matter. |
gr-qc/9510027 | Shigemot | M. Kenmoku, K. Otsuki, K. Shigemoto and K. Uehara | Classical and Quantum Solutions and the Problem of Time in $R^2$
Cosmology | 17 pages, latex, no figure, one reference is corrected | Class.Quant.Grav. 13 (1996) 1751-1760 | 10.1088/0264-9381/13/7/008 | NWU-11/95 | gr-qc | null | We have studied various classical solutions in $R^2$ cosmology. Especially we
have obtained general classical solutions in pure $R^2$\ cosmology. Even in the
quantum theory, we can solve the Wheeler-DeWitt equation in pure $R^2$\
cosmology exactly. Comparing these classical and quantum solutions in $R^2$\
cosmology, we have studied the problem of time in general relativity.
| [
{
"created": "Mon, 16 Oct 1995 07:21:31 GMT",
"version": "v1"
},
{
"created": "Wed, 18 Oct 1995 08:25:12 GMT",
"version": "v2"
}
] | 2009-10-28 | [
[
"Kenmoku",
"M.",
""
],
[
"Otsuki",
"K.",
""
],
[
"Shigemoto",
"K.",
""
],
[
"Uehara",
"K.",
""
]
] | We have studied various classical solutions in $R^2$ cosmology. Especially we have obtained general classical solutions in pure $R^2$\ cosmology. Even in the quantum theory, we can solve the Wheeler-DeWitt equation in pure $R^2$\ cosmology exactly. Comparing these classical and quantum solutions in $R^2$\ cosmology, we have studied the problem of time in general relativity. |
1502.07672 | Antonio Enea Romano | Antonio Enea Romano, Sergio Andres Vallejo | Low red-shift effects of local structure on the Hubble parameter in
presence of a cosmological constant | 14 pages, 4 figures | null | 10.1140/epjc/s10052-016-4033-9 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In order to estimate the effects of local structure on the Hubble parameter
we calculate the low-redshift expansion for $H(z)$ and $\frac{\delta H}{H}$ for
an observer at the center of a spherically symmetric matter distribution in
presence of a cosmological constant. We then test the accuracy of the formulae
comparing them with fully relativistic non perturbative numerical calculations
for different cases for the density profile. The low red-shift expansion we
obtain gives results more precise than perturbation theory since is based on
the use of an exact solution of Einstein's field equations. For larger density
contrasts the low red-shift formulae accuracy improves respect to the
perturbation theory accuracy because the latter is based on the assumption of a
small density contrast, while the former does not rely on such assumption.
The formulae can be used to take into account the effects on the Hubble
expansion parameter due to the monopole component of the local structure. If
the $H(z)$ observations will show deviations from the $\Lambda CDM$ prediction
compatible with the formulae we have derived, this could be considered an
independent evidence of the existence of a local inhomogeneity, and the
formulae could be used to determine the characteristics of this local
structure.
| [
{
"created": "Wed, 25 Feb 2015 01:24:52 GMT",
"version": "v1"
},
{
"created": "Tue, 3 Mar 2015 04:06:42 GMT",
"version": "v2"
},
{
"created": "Fri, 24 Jul 2015 07:50:48 GMT",
"version": "v3"
},
{
"created": "Tue, 26 Apr 2016 06:21:33 GMT",
"version": "v4"
}
] | 2016-07-29 | [
[
"Romano",
"Antonio Enea",
""
],
[
"Vallejo",
"Sergio Andres",
""
]
] | In order to estimate the effects of local structure on the Hubble parameter we calculate the low-redshift expansion for $H(z)$ and $\frac{\delta H}{H}$ for an observer at the center of a spherically symmetric matter distribution in presence of a cosmological constant. We then test the accuracy of the formulae comparing them with fully relativistic non perturbative numerical calculations for different cases for the density profile. The low red-shift expansion we obtain gives results more precise than perturbation theory since is based on the use of an exact solution of Einstein's field equations. For larger density contrasts the low red-shift formulae accuracy improves respect to the perturbation theory accuracy because the latter is based on the assumption of a small density contrast, while the former does not rely on such assumption. The formulae can be used to take into account the effects on the Hubble expansion parameter due to the monopole component of the local structure. If the $H(z)$ observations will show deviations from the $\Lambda CDM$ prediction compatible with the formulae we have derived, this could be considered an independent evidence of the existence of a local inhomogeneity, and the formulae could be used to determine the characteristics of this local structure. |
1610.04094 | Andrea Addazi AndAdd | Andrea Addazi | (Anti)evaporation of Dyonic Black Holes in string-inspired dilaton
$f(R)$-gravity | null | null | 10.1142/S0217751X17501020 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We discuss dyonic black hole solutions in the case of $f(R)$-gravity coupled
with a dilaton and two gauge bosons. The study of such a model is highly
motivated from string theory. Our Black Hole solutions are extensions of the
one firstly studied by Kallosh, Linde, Ort\'in, Peet and Van Proyen (KLOPV) in
[arXiv:hep-th/9205027]. We will show that extreme solutions are unstable. In
particular, these solutions have Bousso-Hawking-Nojiri-Odintsov
(anti)evaporation instabilities.
| [
{
"created": "Thu, 13 Oct 2016 14:22:29 GMT",
"version": "v1"
}
] | 2017-07-05 | [
[
"Addazi",
"Andrea",
""
]
] | We discuss dyonic black hole solutions in the case of $f(R)$-gravity coupled with a dilaton and two gauge bosons. The study of such a model is highly motivated from string theory. Our Black Hole solutions are extensions of the one firstly studied by Kallosh, Linde, Ort\'in, Peet and Van Proyen (KLOPV) in [arXiv:hep-th/9205027]. We will show that extreme solutions are unstable. In particular, these solutions have Bousso-Hawking-Nojiri-Odintsov (anti)evaporation instabilities. |
2209.00770 | Eduardo Bittencourt | \'Erico Goulart, Eduardo Bittencourt, Elliton O. S. Brand\~ao | Light propagation in (2+1)-dimensional electrodynamics: the case of
linear constitutive laws | 12 pages, matching the published version | Phys. Rev. A 106 063521 (2022) | 10.1103/PhysRevA.106.063521 | null | gr-qc math-ph math.MP physics.optics | http://creativecommons.org/licenses/by/4.0/ | In this paper, we turn our attention to light propagation in
three-dimensional electrodynamics. More specifically, we investigate the
behavior of light rays in a continuous bi-dimensional hypothetical medium
living in a three-dimensional ambient spacetime. Relying on a fully covariant
approach, we assume that the medium is endowed with a local and linear response
tensor which maps field strengths into excitations. In the geometric optics
limit, we then obtain the corresponding Fresnel equation and, using well-known
results from algebraic geometry, we derive the effective optical metric.
| [
{
"created": "Fri, 2 Sep 2022 01:04:19 GMT",
"version": "v1"
},
{
"created": "Sat, 31 Dec 2022 18:02:54 GMT",
"version": "v2"
}
] | 2023-01-03 | [
[
"Goulart",
"Érico",
""
],
[
"Bittencourt",
"Eduardo",
""
],
[
"Brandão",
"Elliton O. S.",
""
]
] | In this paper, we turn our attention to light propagation in three-dimensional electrodynamics. More specifically, we investigate the behavior of light rays in a continuous bi-dimensional hypothetical medium living in a three-dimensional ambient spacetime. Relying on a fully covariant approach, we assume that the medium is endowed with a local and linear response tensor which maps field strengths into excitations. In the geometric optics limit, we then obtain the corresponding Fresnel equation and, using well-known results from algebraic geometry, we derive the effective optical metric. |
1607.08537 | Fan Zhang | Fan Zhang | Accumulative coupling between magnetized tenuous plasma and
gravitational waves | 10 pages, 1 figure | Phys. Rev. D 94, 024048 (2016) | 10.1103/PhysRevD.94.024048 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We explicitly compute the plasma wave (PW) induced by a plane gravitational
wave (GW) travelling through a region of strongly magnetized plasma, governed
by force-free electrodynamics. The PW co-moves with the GW and absorbs its
energy to grow over time, creating an essentially force-free counterpart to the
inverse-Gertsenshtein effect. The time-averaged Poynting flux of the induced PW
is comparable to the vacuum case, but the associated current may offer a more
sensitive alternative to photodetection when designing experiments for
detecting/constraining high frequency gravitational waves. Aside from the exact
solutions, we also offer an analysis of the general properties of the GW to PW
conversion process, which should find use when evaluating electromagnetic
counterparts to astrophysical gravitational waves, that are generated directly
by the latter as a second order phenomenon.
| [
{
"created": "Thu, 28 Jul 2016 17:05:30 GMT",
"version": "v1"
}
] | 2016-07-29 | [
[
"Zhang",
"Fan",
""
]
] | We explicitly compute the plasma wave (PW) induced by a plane gravitational wave (GW) travelling through a region of strongly magnetized plasma, governed by force-free electrodynamics. The PW co-moves with the GW and absorbs its energy to grow over time, creating an essentially force-free counterpart to the inverse-Gertsenshtein effect. The time-averaged Poynting flux of the induced PW is comparable to the vacuum case, but the associated current may offer a more sensitive alternative to photodetection when designing experiments for detecting/constraining high frequency gravitational waves. Aside from the exact solutions, we also offer an analysis of the general properties of the GW to PW conversion process, which should find use when evaluating electromagnetic counterparts to astrophysical gravitational waves, that are generated directly by the latter as a second order phenomenon. |
2405.19006 | Guglielmo Faggioli | Guglielmo Faggioli, Maarten van de Meent, Alessandra Buonanno, Aldo
Gamboa, Mohammed Khalil, Gaurav Khanna | Testing eccentric corrections to the radiation-reaction force in the
test-mass limit of effective-one-body models | null | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work, we test an effective-one-body radiation-reaction force for
eccentric planar orbits of a test mass in a Kerr background, which contains
third-order post-Newtonian (PN) non-spinning and second-order PN spin
contributions. We compare the analytical fluxes connected to two different
resummations of this force, truncated at different PN orders in the eccentric
sector, with the numerical fluxes computed through the use of frequency- and
time-domain Teukolsky-equation codes. We find that the different PN truncations
of the radiation-reaction force show the expected scaling in the weak
gravitational-field regime, and we observe a fractional difference with the
numerical fluxes that is $<5 \%$, for orbits characterized by eccentricity $0
\le e \le 0.7$, central black-hole spin $-0.99 M \le a \le 0.99 M$ and fixed
orbital-averaged quantity $x=\langle M\Omega \rangle^{2/3} = 0.06$,
corresponding to the mildly strong-field regime with semilatera recta $9 M<p<17
M$. Our analysis provides useful information for the development of
spin-aligned eccentric models in the comparable-mass case.
| [
{
"created": "Wed, 29 May 2024 11:45:09 GMT",
"version": "v1"
}
] | 2024-05-30 | [
[
"Faggioli",
"Guglielmo",
""
],
[
"van de Meent",
"Maarten",
""
],
[
"Buonanno",
"Alessandra",
""
],
[
"Gamboa",
"Aldo",
""
],
[
"Khalil",
"Mohammed",
""
],
[
"Khanna",
"Gaurav",
""
]
] | In this work, we test an effective-one-body radiation-reaction force for eccentric planar orbits of a test mass in a Kerr background, which contains third-order post-Newtonian (PN) non-spinning and second-order PN spin contributions. We compare the analytical fluxes connected to two different resummations of this force, truncated at different PN orders in the eccentric sector, with the numerical fluxes computed through the use of frequency- and time-domain Teukolsky-equation codes. We find that the different PN truncations of the radiation-reaction force show the expected scaling in the weak gravitational-field regime, and we observe a fractional difference with the numerical fluxes that is $<5 \%$, for orbits characterized by eccentricity $0 \le e \le 0.7$, central black-hole spin $-0.99 M \le a \le 0.99 M$ and fixed orbital-averaged quantity $x=\langle M\Omega \rangle^{2/3} = 0.06$, corresponding to the mildly strong-field regime with semilatera recta $9 M<p<17 M$. Our analysis provides useful information for the development of spin-aligned eccentric models in the comparable-mass case. |
2311.01495 | Kiana Salehi | Kiana Salehi, Avery Broderick and Boris Georgiev | Photon Rings and Shadow Size for General Integrable Spacetimes | null | null | null | null | gr-qc astro-ph.HE | http://creativecommons.org/licenses/by/4.0/ | There are now multiple direct probes of the region near black hole horizons,
including direct imaging with the Event Horizon Telescope (EHT). As a result,
it is now of considerable interest to identify what aspects of the underlying
spacetime are constrained by these observations. For this purpose, we present a
new formulation of an existing broad class of integrable, axisymmetric,
stationary spinning black hole spacetimes, specified by four free radial
functions, that makes manifest which functions are responsible for setting the
location and morphology of the event horizon and ergosphere. We explore the
size of the black hole shadow and high-order photon rings for polar observers,
approximately appropriate for the EHT observations of M87*, finding analogous
expressions to those for general spherical spacetimes. Of particular interest,
we find that these are independent of the properties of the ergosphere, but
does directly probe on the free function that defines the event horizon. Based
on these, we extend the nonperturbative, nonparametric characterization of the
gravitational implications of various near-horizon measurements to spinning
spacetimes. Finally, we demonstrate this characterization for a handful of
explicit alternative spacetimes.
| [
{
"created": "Thu, 2 Nov 2023 18:00:00 GMT",
"version": "v1"
}
] | 2023-11-06 | [
[
"Salehi",
"Kiana",
""
],
[
"Broderick",
"Avery",
""
],
[
"Georgiev",
"Boris",
""
]
] | There are now multiple direct probes of the region near black hole horizons, including direct imaging with the Event Horizon Telescope (EHT). As a result, it is now of considerable interest to identify what aspects of the underlying spacetime are constrained by these observations. For this purpose, we present a new formulation of an existing broad class of integrable, axisymmetric, stationary spinning black hole spacetimes, specified by four free radial functions, that makes manifest which functions are responsible for setting the location and morphology of the event horizon and ergosphere. We explore the size of the black hole shadow and high-order photon rings for polar observers, approximately appropriate for the EHT observations of M87*, finding analogous expressions to those for general spherical spacetimes. Of particular interest, we find that these are independent of the properties of the ergosphere, but does directly probe on the free function that defines the event horizon. Based on these, we extend the nonperturbative, nonparametric characterization of the gravitational implications of various near-horizon measurements to spinning spacetimes. Finally, we demonstrate this characterization for a handful of explicit alternative spacetimes. |
gr-qc/9911025 | Alexander N. Petrov | A. N. Petrov (1) and J. Katz (2) ((1) Sternberg Astronomical
Institute, Moscow (2) Racah Institute of Physics, Jerusalem) | Relativistic Conservation Laws on Curved Backgrounds and the Theory of
Cosmological Perturbations | 38 pages, plain TEX | Proc.Roy.Soc.Lond.458:319-337,2002 | 10.1098/rspa.2001.0865 | null | gr-qc | null | We first consider the Lagrangian formulation of general relativity for
perturbations with respect to a background spacetime. We show that by combining
Noether's method with Belinfante's "symmetrization'' procedure we obtain
conserved vectors that are independent of any divergence added to the perturbed
Hilbert Lagrangian. We also show that the corresponding perturbed energy-
momentum tensor is symmetrical and divergenceless but only on backgrounds that
are "Einstein spaces" in the sense of A.Z. Petrov. de Sitter or anti-de Sitter
and Einstein "spacetimes" are Einstein spaces but in general
Friedmann-Robertson -Walker spacetimes are not. Each conserved vector is a
divergence of an anti- symmetric tensor, a "superpotential". We find
superpotentials which are a generalization of Papapetrou's superpotential and
are rigorously linear, even for large perturbations, in terms of the inverse
metric density components and their first order derivatives. The
superpotentials give correct globally conserved quantities at spatial infinity.
They resemble Abbott and Deser's superpotential, but give correctly the
Bondi-Sachs total four-momentum at null infinity. Next we calculate conserved
vectors and superpotentials for perturbations of a Friedmann-Robertson-Walker
background associated with its 15 conformal Killing vectors given in a
convenient form. The integral of each conserved vector in a finite volume V at
a given conformal time is equal to a surface integral on the boundary of V of
the superpotential. For given boundary conditions each such integral is part of
a flux whose total through a closed hypersurface is equal to zero. For given
boundary conditions on V, the integral can be considered as an "integral
constraint" on data in the volume...
| [
{
"created": "Mon, 8 Nov 1999 13:47:09 GMT",
"version": "v1"
},
{
"created": "Fri, 12 Nov 1999 16:13:02 GMT",
"version": "v2"
},
{
"created": "Sun, 24 Jun 2001 11:38:15 GMT",
"version": "v3"
}
] | 2015-06-25 | [
[
"Petrov",
"A. N.",
""
],
[
"Katz",
"J.",
""
]
] | We first consider the Lagrangian formulation of general relativity for perturbations with respect to a background spacetime. We show that by combining Noether's method with Belinfante's "symmetrization'' procedure we obtain conserved vectors that are independent of any divergence added to the perturbed Hilbert Lagrangian. We also show that the corresponding perturbed energy- momentum tensor is symmetrical and divergenceless but only on backgrounds that are "Einstein spaces" in the sense of A.Z. Petrov. de Sitter or anti-de Sitter and Einstein "spacetimes" are Einstein spaces but in general Friedmann-Robertson -Walker spacetimes are not. Each conserved vector is a divergence of an anti- symmetric tensor, a "superpotential". We find superpotentials which are a generalization of Papapetrou's superpotential and are rigorously linear, even for large perturbations, in terms of the inverse metric density components and their first order derivatives. The superpotentials give correct globally conserved quantities at spatial infinity. They resemble Abbott and Deser's superpotential, but give correctly the Bondi-Sachs total four-momentum at null infinity. Next we calculate conserved vectors and superpotentials for perturbations of a Friedmann-Robertson-Walker background associated with its 15 conformal Killing vectors given in a convenient form. The integral of each conserved vector in a finite volume V at a given conformal time is equal to a surface integral on the boundary of V of the superpotential. For given boundary conditions each such integral is part of a flux whose total through a closed hypersurface is equal to zero. For given boundary conditions on V, the integral can be considered as an "integral constraint" on data in the volume... |
1706.04920 | Martin Kr\v{s}\v{s}\'ak | Sebastian Bahamonde, Christian G. Boehmer, Martin Krssak | New classes of modified teleparallel gravity models | v2: 10 pages, accepted for publication in PLB; for a detailed
derivation of the field equations see Appendix A in v1 | Phys.Lett. B775 (2017) 37-43 | 10.1016/j.physletb.2017.10.026 | null | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | New classes of modified teleparallel theories of gravity are introduced. The
action of this theory is constructed to be a function of the irreducible parts
of torsion $f(T_{\rm ax},T_{\rm ten},T_{\rm vec})$, where $T_{\rm ax},T_{\rm
ten}$ and $T_{\rm vec}$ are squares of the axial, tensor and vector components
of torsion, respectively. This is the most general (well-motivated) second
order teleparallel theory of gravity that can be constructed from the torsion
tensor. Different particular second order theories can be recovered from this
theory such as new general relativity, conformal teleparallel gravity or $f(T)$
gravity. Additionally, the boundary term $B$ which connects the Ricci scalar
with the torsion scalar via $R=-T+B$ can also be incorporated into the action.
By performing a conformal transformation, it is shown that the two unique
theories which have an Einstein frame are either the teleparallel equivalent of
general relativity or $f(-T+B)=f(R)$ gravity, as expected.
| [
{
"created": "Thu, 15 Jun 2017 15:19:42 GMT",
"version": "v1"
},
{
"created": "Sun, 22 Oct 2017 01:54:34 GMT",
"version": "v2"
}
] | 2017-10-31 | [
[
"Bahamonde",
"Sebastian",
""
],
[
"Boehmer",
"Christian G.",
""
],
[
"Krssak",
"Martin",
""
]
] | New classes of modified teleparallel theories of gravity are introduced. The action of this theory is constructed to be a function of the irreducible parts of torsion $f(T_{\rm ax},T_{\rm ten},T_{\rm vec})$, where $T_{\rm ax},T_{\rm ten}$ and $T_{\rm vec}$ are squares of the axial, tensor and vector components of torsion, respectively. This is the most general (well-motivated) second order teleparallel theory of gravity that can be constructed from the torsion tensor. Different particular second order theories can be recovered from this theory such as new general relativity, conformal teleparallel gravity or $f(T)$ gravity. Additionally, the boundary term $B$ which connects the Ricci scalar with the torsion scalar via $R=-T+B$ can also be incorporated into the action. By performing a conformal transformation, it is shown that the two unique theories which have an Einstein frame are either the teleparallel equivalent of general relativity or $f(-T+B)=f(R)$ gravity, as expected. |
2303.11104 | Shahram Jalalzadeh | Shahram Jalalzadeh | Intrinsic quantum dynamics of particles in brane gravity | 17 pages, 4 figures, to appear in Annal of Physics | Ann. Phys. (2023) 452, 169291 | 10.1016/j.aop.2023.169291 | null | gr-qc hep-th quant-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Newtonian dynamics of particles in brane gravity is investigated. Due to
the coupling of the particles' energy-momentum tensor to the tension of the
brane, the particle is semi-confined and oscillates along the extra dimension.
We demonstrate that the frequency of these oscillations is proportional to the
kinetic energy of the particle in the brane. We show that the classical
stability of particle trajectories on the brane gives us the Bohr--Sommerfeld
quantization condition. The particle's motion along the extra dimension allows
us to formulate a geometrical version of the uncertainty principle.
Furthermore, we exhibited that the particle's motion along the extra dimension
is identical to the time-independent Schr\"odinger equation. The dynamics of a
free particle, particles in a box, a harmonic oscillator, a bouncing particle,
and tunneling are re-examined. We show that the particle's motion along the
extra dimension yields a quantized energy spectrum for bound states.
| [
{
"created": "Mon, 20 Mar 2023 13:41:07 GMT",
"version": "v1"
}
] | 2023-04-04 | [
[
"Jalalzadeh",
"Shahram",
""
]
] | The Newtonian dynamics of particles in brane gravity is investigated. Due to the coupling of the particles' energy-momentum tensor to the tension of the brane, the particle is semi-confined and oscillates along the extra dimension. We demonstrate that the frequency of these oscillations is proportional to the kinetic energy of the particle in the brane. We show that the classical stability of particle trajectories on the brane gives us the Bohr--Sommerfeld quantization condition. The particle's motion along the extra dimension allows us to formulate a geometrical version of the uncertainty principle. Furthermore, we exhibited that the particle's motion along the extra dimension is identical to the time-independent Schr\"odinger equation. The dynamics of a free particle, particles in a box, a harmonic oscillator, a bouncing particle, and tunneling are re-examined. We show that the particle's motion along the extra dimension yields a quantized energy spectrum for bound states. |
1001.2616 | Ngangbam Ibohal | Ng. Ibohal and L. Kapil | Charged black holes in Vaidya backgrounds: Hawking's Radiation | 30 pages, latex file, no figures | Int.J.Mod.Phys.D19:437-464,2010 | 10.1142/S0218271810016518 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper we propose a class of embedded solutions of Einstein's field
equations describing non-rotating Reissner-Nordstrom-Vaidya and rotating
Kerr-Newman-Vaidya black holes.
| [
{
"created": "Fri, 15 Jan 2010 06:19:41 GMT",
"version": "v1"
}
] | 2014-11-20 | [
[
"Ibohal",
"Ng.",
""
],
[
"Kapil",
"L.",
""
]
] | In this paper we propose a class of embedded solutions of Einstein's field equations describing non-rotating Reissner-Nordstrom-Vaidya and rotating Kerr-Newman-Vaidya black holes. |
1904.10248 | James Edholm | James Edholm | Infinite Derivative Gravity: A finite number of predictions | Doctoral thesis | null | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Ghost-free Infinite Derivative Gravity (IDG) is a modified gravity theory
which can avoid the singularities predicted by General Relativity. This thesis
examines the effect of IDG on four areas of importance for theoretical
cosmologists and experimentalists. First, the gravitational potential produced
by a point source is derived and compared to experimental evidence, around both
Minkowski and (Anti) de Sitter backgrounds. Second, the conditions necessary
for avoidance of singularities for perturbations around Minkowski and (Anti) de
Sitter spacetimes are found, as well as for background
Friedmann-Robertson-Walker spacetimes. Third, the modification to perturbations
during primordial inflation is derived and shown to give a constraint on the
mass scale of IDG, and to allow further tests of the theory. Finally, the
effect of IDG on the production and propagation of gravitational waves is
derived and it is shown that IDG gives almost precisely the same predictions as
General Relativity for the power emitted by a binary system.
| [
{
"created": "Tue, 23 Apr 2019 11:18:59 GMT",
"version": "v1"
},
{
"created": "Sat, 2 Nov 2019 16:29:39 GMT",
"version": "v2"
}
] | 2019-11-05 | [
[
"Edholm",
"James",
""
]
] | Ghost-free Infinite Derivative Gravity (IDG) is a modified gravity theory which can avoid the singularities predicted by General Relativity. This thesis examines the effect of IDG on four areas of importance for theoretical cosmologists and experimentalists. First, the gravitational potential produced by a point source is derived and compared to experimental evidence, around both Minkowski and (Anti) de Sitter backgrounds. Second, the conditions necessary for avoidance of singularities for perturbations around Minkowski and (Anti) de Sitter spacetimes are found, as well as for background Friedmann-Robertson-Walker spacetimes. Third, the modification to perturbations during primordial inflation is derived and shown to give a constraint on the mass scale of IDG, and to allow further tests of the theory. Finally, the effect of IDG on the production and propagation of gravitational waves is derived and it is shown that IDG gives almost precisely the same predictions as General Relativity for the power emitted by a binary system. |
1909.13393 | Yan Peng | Yan Peng | Stationary scalar hairy configurations supported by Neumann compact
stars | 10 pages, 1 figure | Nuclear Physics B 950(2020)114879 | 10.1016/j.nuclphysb.2019.114879 | null | gr-qc hep-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study stationary scalar field hairy configurations supported by
asymptotically flat horizonless compact stars. At the star surface, we impose
Neumann boundary conditions for the scalar field. With analytical methods, we
obtain bounds on the frequency of scalar fields. For certain discrete frequency
satisfying the bounds, we numerically get solutions of scalar hairy stars. We
also disclose effects of model parameters on the discrete frequency of scalar
fields.
| [
{
"created": "Sun, 29 Sep 2019 22:51:35 GMT",
"version": "v1"
},
{
"created": "Sat, 7 Dec 2019 03:47:30 GMT",
"version": "v2"
}
] | 2019-12-10 | [
[
"Peng",
"Yan",
""
]
] | We study stationary scalar field hairy configurations supported by asymptotically flat horizonless compact stars. At the star surface, we impose Neumann boundary conditions for the scalar field. With analytical methods, we obtain bounds on the frequency of scalar fields. For certain discrete frequency satisfying the bounds, we numerically get solutions of scalar hairy stars. We also disclose effects of model parameters on the discrete frequency of scalar fields. |
gr-qc/9801037 | Mike Grebeniuk | V.N. Melnikov | Multidimensional Gravity and Cosmology: Exact Solutions | 17 pages, Latex. To appear in Proceedings of MG8 Meeting, Jerusalem,
1997 (World Scientific, Singapore) | null | null | null | gr-qc | null | A short review of recent results on exact solutions in multidimensional
cosmology and overview of reports at workshop in MG8 (held by the author) are
presented.
| [
{
"created": "Mon, 12 Jan 1998 16:29:57 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Melnikov",
"V. N.",
""
]
] | A short review of recent results on exact solutions in multidimensional cosmology and overview of reports at workshop in MG8 (held by the author) are presented. |
gr-qc/9906092 | Piotr Jaranowski | Piotr Jaranowski and Gerhard Sch\"afer | The binary black-hole problem at the third post-Newtonian approximation
in the orbital motion: Static part | LaTeX, 9 pages, to be submitted to Physical Review D | Phys.Rev.D60:124003,1999 | 10.1103/PhysRevD.60.124003 | null | gr-qc | null | Post-Newtonian expansions of the Brill-Lindquist and Misner-Lindquist
solutions of the time-symmetric two-black-hole initial value problem are
derived. The static Hamiltonians related to the expanded solutions, after
identifying the bare masses in both solutions, are found to differ from each
other at the third post-Newtonian approximation. By shifting the position
variables of the black holes the post-Newtonian expansions of the three metrics
can be made to coincide up to the fifth post-Newtonian order resulting in
identical static Hamiltonians up the third post-Newtonian approximation. The
calculations shed light on previously performed binary point-mass calculations
at the third post-Newtonian approximation.
| [
{
"created": "Wed, 23 Jun 1999 09:30:58 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Jaranowski",
"Piotr",
""
],
[
"Schäfer",
"Gerhard",
""
]
] | Post-Newtonian expansions of the Brill-Lindquist and Misner-Lindquist solutions of the time-symmetric two-black-hole initial value problem are derived. The static Hamiltonians related to the expanded solutions, after identifying the bare masses in both solutions, are found to differ from each other at the third post-Newtonian approximation. By shifting the position variables of the black holes the post-Newtonian expansions of the three metrics can be made to coincide up to the fifth post-Newtonian order resulting in identical static Hamiltonians up the third post-Newtonian approximation. The calculations shed light on previously performed binary point-mass calculations at the third post-Newtonian approximation. |
2008.05331 | Juan M. Z\'arate Pretel | Juan M. Z. Pretel | Equilibrium, radial stability and non-adiabatic gravitational collapse
of anisotropic neutron stars | 17 pages, 7 figures | Eur. Phys. J. C 80 (2020) 726 | 10.1140/epjc/s10052-020-8301-3 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work we construct families of anisotropic neutron stars for an
equation of state compatible with the constraints of the gravitational-wave
event GW170817 and for four anisotropy ansatze. Such stars are subjected to a
radial perturbation in order to study their stability against radial
oscillations and we develop a dynamical model to describe the non-adiabatic
gravitational collapse of the unstable anisotropic configurations whose
ultimate fate is the formation of a black hole. We find that the standard
criterion for radial stability $dM/d\rho_c >0$ is not always compatible with
the calculation of the oscillation frequencies for some anisotropy ansatze, and
each anisotropy parameter is constrained taking into account the recent
restriction of maximum mass of neutron stars. We further generalize the TOV
equations within a non-adiabatic context and we investigate the dynamical
behaviour of the equation of state, heat flux, anisotropy factor and mass
function as an unstable anisotropic star collapses. After obtaining the
evolution equations we recover, as a static limit, the background equations.
| [
{
"created": "Wed, 12 Aug 2020 14:12:05 GMT",
"version": "v1"
}
] | 2020-08-13 | [
[
"Pretel",
"Juan M. Z.",
""
]
] | In this work we construct families of anisotropic neutron stars for an equation of state compatible with the constraints of the gravitational-wave event GW170817 and for four anisotropy ansatze. Such stars are subjected to a radial perturbation in order to study their stability against radial oscillations and we develop a dynamical model to describe the non-adiabatic gravitational collapse of the unstable anisotropic configurations whose ultimate fate is the formation of a black hole. We find that the standard criterion for radial stability $dM/d\rho_c >0$ is not always compatible with the calculation of the oscillation frequencies for some anisotropy ansatze, and each anisotropy parameter is constrained taking into account the recent restriction of maximum mass of neutron stars. We further generalize the TOV equations within a non-adiabatic context and we investigate the dynamical behaviour of the equation of state, heat flux, anisotropy factor and mass function as an unstable anisotropic star collapses. After obtaining the evolution equations we recover, as a static limit, the background equations. |
1404.4195 | Ola Malaeb | O. Malaeb | Hamiltonian Formulation of Mimetic Gravity | null | Phys. Rev. D 91, 103526 (2015) | 10.1103/PhysRevD.91.103526 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Hamiltonian formulation of Mimetic Gravity is formulated. Although there
are two more equations than those of general relativity, these are proved to be
the constraint equation and the conservation of energy-momentum tensor. The
Poisson brackets are then computed and closure is proved. At the end,
Wheeler-DeWitt equation was solved for a homogeneous and isotropic universe.
This was done first for a vanishing potential where agreement with the dust
case was shown, and then for a constant potential.
| [
{
"created": "Wed, 16 Apr 2014 10:38:08 GMT",
"version": "v1"
},
{
"created": "Thu, 30 Apr 2015 13:15:38 GMT",
"version": "v2"
}
] | 2015-05-27 | [
[
"Malaeb",
"O.",
""
]
] | The Hamiltonian formulation of Mimetic Gravity is formulated. Although there are two more equations than those of general relativity, these are proved to be the constraint equation and the conservation of energy-momentum tensor. The Poisson brackets are then computed and closure is proved. At the end, Wheeler-DeWitt equation was solved for a homogeneous and isotropic universe. This was done first for a vanishing potential where agreement with the dust case was shown, and then for a constant potential. |
1607.01442 | Douglas A. Singleton | Douglas Singleton and Steve Wilburn | Global versus Local -- Mach's Principle versus the Equivalence Principle | 9 pages revtex, no figures. Awarded an "honorable mention" in the
Gravity Research Foundation 2016 Essays on Gravitation contest. To be
published in special edition of IJMPD | null | 10.1142/S0218271816440090 | null | gr-qc hep-th quant-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The equivalence principle is the conceptual basis for general relativity. In
contrast Mach's principle, although said to have been influential on Einstein
in his formulation of general relativity, has not been shown to be central to
the structure of general relativity. In this essay we suggest that the quantum
effects of Hawking and Unruh radiation are a manifestation of a {\it thermal}
Mach's principle, where the local thermodynamic properties of the system are
determined by the non-local structure of the quantum fields which determine the
vacuum of a given spacetime. By comparing Hawking and Unruh temperatures for
the same local acceleration we find a violation of the Einstein elevator
version of the equivalence principle, which vanishes in the limit that the
horizon is approached.
| [
{
"created": "Wed, 6 Jul 2016 00:06:03 GMT",
"version": "v1"
}
] | 2016-11-15 | [
[
"Singleton",
"Douglas",
""
],
[
"Wilburn",
"Steve",
""
]
] | The equivalence principle is the conceptual basis for general relativity. In contrast Mach's principle, although said to have been influential on Einstein in his formulation of general relativity, has not been shown to be central to the structure of general relativity. In this essay we suggest that the quantum effects of Hawking and Unruh radiation are a manifestation of a {\it thermal} Mach's principle, where the local thermodynamic properties of the system are determined by the non-local structure of the quantum fields which determine the vacuum of a given spacetime. By comparing Hawking and Unruh temperatures for the same local acceleration we find a violation of the Einstein elevator version of the equivalence principle, which vanishes in the limit that the horizon is approached. |
gr-qc/0304064 | Hideo Kodama | Hideo Kodama and Wataru Hikida (YITP, Kyoto University) | Global structure of the Zipoy-Voorhees-Weyl spacetime and the delta=2
Tomimatsu-Sato spacetime | 20 pages, 11 figures. The title was slightly changed, and references
were added. The published version | Class.Quant.Grav. 20:5121-5140,2003 | 10.1088/0264-9381/20/23/011 | null | gr-qc astro-ph | null | We investigate the structure of the ZVW (Zipoy-Voorhees-Weyl) spacetime,
which is a Weyl solution described by the Zipoy-Voorhees metric, and the
delta=2 Tomimatsu-Sato spacetime. We show that the singularity of the ZVW
spacetime, which is represented by a segment rho=0, -sigma<z<sigma in the Weyl
coordinates, is geometrically point-like for delta<0, string-like for 0<delta<1
and ring-like for delta>1. These singularities are always naked and have
positive Komar masses for delta>0. Thus, they provide a non-trivial example of
naked singularities with positive mass. We further show that the ZVW spacetime
has a degenerate Killing horizon with a ring singularity at the equatorial
plane for delta=2,3 and delta>=4. We also show that the delta=2 Tomimatsu-Sato
spacetime has a degenerate horizon with two components, in contrast to the
general belief that the Tomimatsu-Sato solutions with even delta do not have
horizons.
| [
{
"created": "Thu, 17 Apr 2003 10:28:43 GMT",
"version": "v1"
},
{
"created": "Fri, 31 Oct 2003 17:26:17 GMT",
"version": "v2"
}
] | 2011-01-27 | [
[
"Kodama",
"Hideo",
"",
"YITP, Kyoto University"
],
[
"Hikida",
"Wataru",
"",
"YITP, Kyoto University"
]
] | We investigate the structure of the ZVW (Zipoy-Voorhees-Weyl) spacetime, which is a Weyl solution described by the Zipoy-Voorhees metric, and the delta=2 Tomimatsu-Sato spacetime. We show that the singularity of the ZVW spacetime, which is represented by a segment rho=0, -sigma<z<sigma in the Weyl coordinates, is geometrically point-like for delta<0, string-like for 0<delta<1 and ring-like for delta>1. These singularities are always naked and have positive Komar masses for delta>0. Thus, they provide a non-trivial example of naked singularities with positive mass. We further show that the ZVW spacetime has a degenerate Killing horizon with a ring singularity at the equatorial plane for delta=2,3 and delta>=4. We also show that the delta=2 Tomimatsu-Sato spacetime has a degenerate horizon with two components, in contrast to the general belief that the Tomimatsu-Sato solutions with even delta do not have horizons. |
1108.3512 | Andrew J. S. Hamilton | Andrew J. S. Hamilton | Towards a general description of the interior structure of rotating
black holes | 15 pages | null | null | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The purpose of this paper is to present a number of proposals about the
interior structure of a rotating black hole that is accreting slowly, but in an
arbitrary time- and space-dependent fashion. The proposals could potentially be
tested with numerical simulations. Outgoing and ingoing particles free-falling
in the parent Kerr geometry become highly focused along the principal outgoing
and ingoing null directions as they approach the inner horizon, triggering the
mass inflation instability. The original arguments of Barrabes, Israel &
Poisson (1990) regarding inflation in rotating black holes are reviewed, and
shown to be based on Raychauduri's equation applied along the outgoing and
ingoing null directions. It is argued that gravitational waves should behave in
the geometric optics limit, and consequently that the spacetime should be
almost shear-free. A full set of shear-free equations is derived. A specific
line-element is proposed, which is argued should provide a satisfactory
approximation during early inflation. Finally, it is argued that
super-Planckian collisions between outgoing and ingoing particles will lead to
entropy production, bringing inflation to an end, and precipitating collapse.
| [
{
"created": "Wed, 17 Aug 2011 15:57:53 GMT",
"version": "v1"
}
] | 2011-08-22 | [
[
"Hamilton",
"Andrew J. S.",
""
]
] | The purpose of this paper is to present a number of proposals about the interior structure of a rotating black hole that is accreting slowly, but in an arbitrary time- and space-dependent fashion. The proposals could potentially be tested with numerical simulations. Outgoing and ingoing particles free-falling in the parent Kerr geometry become highly focused along the principal outgoing and ingoing null directions as they approach the inner horizon, triggering the mass inflation instability. The original arguments of Barrabes, Israel & Poisson (1990) regarding inflation in rotating black holes are reviewed, and shown to be based on Raychauduri's equation applied along the outgoing and ingoing null directions. It is argued that gravitational waves should behave in the geometric optics limit, and consequently that the spacetime should be almost shear-free. A full set of shear-free equations is derived. A specific line-element is proposed, which is argued should provide a satisfactory approximation during early inflation. Finally, it is argued that super-Planckian collisions between outgoing and ingoing particles will lead to entropy production, bringing inflation to an end, and precipitating collapse. |
1410.8643 | Jiro Soda | Jiro Soda | Anisotropic Power-law Inflation: A counter example to the cosmic no-hair
conjecture | 6 pages, 1 figure, Conference proceedings for the Spanish Relativity
Meeting (ERE 2014), Valencia, Spain, 1-5 Sept. 2014 | null | 10.1088/1742-6596/600/1/012026 | KOBE-TH-14-10 | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | It is widely believed that anisotropy in the expansion of the universe will
decay exponentially fast during inflation. This is often referred to as the
cosmic no-hair conjecture. However, we find a counter example to the cosmic
no-hair conjecture in the context of supergravity. As a demonstration, we
present an exact anisotropic power-law inflationary solution which is an
attractor in the phase space. We emphasize that anisotropic inflation is quite
generic in the presence of anisotropic sources which couple with an inflaton.
| [
{
"created": "Fri, 31 Oct 2014 05:13:37 GMT",
"version": "v1"
}
] | 2015-05-20 | [
[
"Soda",
"Jiro",
""
]
] | It is widely believed that anisotropy in the expansion of the universe will decay exponentially fast during inflation. This is often referred to as the cosmic no-hair conjecture. However, we find a counter example to the cosmic no-hair conjecture in the context of supergravity. As a demonstration, we present an exact anisotropic power-law inflationary solution which is an attractor in the phase space. We emphasize that anisotropic inflation is quite generic in the presence of anisotropic sources which couple with an inflaton. |
2103.06724 | Georgios Lukes-Gerakopoulos | Georgios Lukes-Gerakopoulos and Vojt\v{e}ch Witzany | Non-linear effects in EMRI dynamics and their imprints on gravitational
waves | 44 pages, 9 figures, 1 table. Invited chapter for "Handbook of
Gravitational Wave Astronomy" (Eds. C. Bambi, S. Katsanevas, and K. Kokkotas;
Springer, Singapore, 2021) | null | 10.1007/978-981-15-4702-7_42-1 | null | gr-qc astro-ph.HE nlin.CD | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The largest part of any gravitational-wave inspiral of a compact binary can
be understood as a slow, adiabatic drift between the trajectories of a certain
referential conservative system. In many contexts, the phase space of this
conservative system is smooth and there are no "topological transitions" in the
phase space, meaning that there are no sudden qualitative changes in the
character of the orbital motion during the inspiral. However, in this chapter
we discuss the cases where this assumption fails and non-linear and/or
non-smooth transitions come into play. In integrable conservative systems under
perturbation, topological transitions suddenly appear at resonances, and we
sketch how to implement the passage through such regions in an inspiral model.
Even though many of the developments of this chapter apply to general
inspirals, we focus on a particular scenario known as the Extreme mass ratio
inspiral (EMRI). An EMRI consists of a compact stellar-mass object inspiralling
into a supermassive black hole. At leading order, the referential conservative
system is simply geodesic motion in the field of the supermassive black hole
and the rate of the drift is given by radiation reaction. In Einstein gravity
the supermassive black hole field is the Kerr space-time in which the geodesic
motion is integrable. However, the equations of motion can be perturbed in
various ways so that prolonged resonances and chaos appear in phase space as
well as the inspiral, which we demonstrate in simple physically motivated
examples.
| [
{
"created": "Thu, 11 Mar 2021 15:17:15 GMT",
"version": "v1"
}
] | 2021-11-23 | [
[
"Lukes-Gerakopoulos",
"Georgios",
""
],
[
"Witzany",
"Vojtěch",
""
]
] | The largest part of any gravitational-wave inspiral of a compact binary can be understood as a slow, adiabatic drift between the trajectories of a certain referential conservative system. In many contexts, the phase space of this conservative system is smooth and there are no "topological transitions" in the phase space, meaning that there are no sudden qualitative changes in the character of the orbital motion during the inspiral. However, in this chapter we discuss the cases where this assumption fails and non-linear and/or non-smooth transitions come into play. In integrable conservative systems under perturbation, topological transitions suddenly appear at resonances, and we sketch how to implement the passage through such regions in an inspiral model. Even though many of the developments of this chapter apply to general inspirals, we focus on a particular scenario known as the Extreme mass ratio inspiral (EMRI). An EMRI consists of a compact stellar-mass object inspiralling into a supermassive black hole. At leading order, the referential conservative system is simply geodesic motion in the field of the supermassive black hole and the rate of the drift is given by radiation reaction. In Einstein gravity the supermassive black hole field is the Kerr space-time in which the geodesic motion is integrable. However, the equations of motion can be perturbed in various ways so that prolonged resonances and chaos appear in phase space as well as the inspiral, which we demonstrate in simple physically motivated examples. |
0806.3293 | Samuel E. Gralla | Samuel E. Gralla and Robert M. Wald | A Rigorous Derivation of Gravitational Self-force | typos fixed; errors in equations corrected; notes added to text | Class.Quant.Grav.25:205009,2008; Erratum-ibid.28:159501,2011 | 10.1088/0264-9381/25/20/205009 10.1088/0264-9381/28/15/159501 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | There is general agreement that the MiSaTaQuWa equations should describe the
motion of a "small body" in general relativity, taking into account the leading
order self-force effects. However, previous derivations of these equations have
made a number of ad hoc assumptions and/or contain a number of unsatisfactory
features. For example, all previous derivations have invoked, without proper
justification, the step of "Lorenz gauge relaxation", wherein the linearized
Einstein equation is written down in the form appropriate to the Lorenz gauge,
but the Lorenz gauge condition is then not imposed--thereby making the
resulting equations for the metric perturbation inequivalent to the linearized
Einstein equations. In this paper, we analyze the issue of "particle motion" in
general relativity in a systematic and rigorous way by considering a
one-parameter family of metrics, $g_{ab} (\lambda)$, corresponding to having a
body (or black hole) that is "scaled down" to zero size and mass in an
appropriate manner. We prove that the limiting worldline of such a
one-parameter family must be a geodesic of the background metric, $g_{ab}
(\lambda=0)$. Gravitational self-force--as well as the force due to coupling of
the spin of the body to curvature--then arises as a first-order perturbative
correction in $\lambda$ to this worldline. No assumptions are made in our
analysis apart from the smoothness and limit properties of the one-parameter
family of metrics. Our approach should provide a framework for systematically
calculating higher order corrections to gravitational self-force, including
higher multipole effects, although we do not attempt to go beyond first order
calculations here. The status of the MiSaTaQuWa equations is explained.
| [
{
"created": "Thu, 19 Jun 2008 22:03:30 GMT",
"version": "v1"
},
{
"created": "Mon, 21 Jul 2008 14:50:18 GMT",
"version": "v2"
},
{
"created": "Mon, 18 Aug 2008 22:23:07 GMT",
"version": "v3"
},
{
"created": "Thu, 11 Sep 2008 21:05:54 GMT",
"version": "v4"
},
{
"created": "Fri, 29 Apr 2011 14:18:21 GMT",
"version": "v5"
}
] | 2011-06-30 | [
[
"Gralla",
"Samuel E.",
""
],
[
"Wald",
"Robert M.",
""
]
] | There is general agreement that the MiSaTaQuWa equations should describe the motion of a "small body" in general relativity, taking into account the leading order self-force effects. However, previous derivations of these equations have made a number of ad hoc assumptions and/or contain a number of unsatisfactory features. For example, all previous derivations have invoked, without proper justification, the step of "Lorenz gauge relaxation", wherein the linearized Einstein equation is written down in the form appropriate to the Lorenz gauge, but the Lorenz gauge condition is then not imposed--thereby making the resulting equations for the metric perturbation inequivalent to the linearized Einstein equations. In this paper, we analyze the issue of "particle motion" in general relativity in a systematic and rigorous way by considering a one-parameter family of metrics, $g_{ab} (\lambda)$, corresponding to having a body (or black hole) that is "scaled down" to zero size and mass in an appropriate manner. We prove that the limiting worldline of such a one-parameter family must be a geodesic of the background metric, $g_{ab} (\lambda=0)$. Gravitational self-force--as well as the force due to coupling of the spin of the body to curvature--then arises as a first-order perturbative correction in $\lambda$ to this worldline. No assumptions are made in our analysis apart from the smoothness and limit properties of the one-parameter family of metrics. Our approach should provide a framework for systematically calculating higher order corrections to gravitational self-force, including higher multipole effects, although we do not attempt to go beyond first order calculations here. The status of the MiSaTaQuWa equations is explained. |
gr-qc/0504104 | Sunil Maharaj | S. Hansraj, S. D. Maharaj, A. M. Msomi and K. S. Govinder | Lie symmetries for equations in conformal geometries | 19 pages, To appear in J. Phys. A | J.Phys. A38 (2005) 4419-4432 | 10.1088/0305-4470/38/20/009 | null | gr-qc | null | We seek exact solutions to the Einstein field equations which arise when two
spacetime geometries are conformally related. Whilst this is a simple method to
generate new solutions to the field equations, very few such examples have been
found in practice. We use the method of Lie analysis of differential equations
to obtain new group invariant solutions to conformally related Petrov type D
spacetimes. Four cases arise depending on the nature of the Lie symmetry
generator. In three cases we are in a position to solve the master field
equation in terms of elementary functions. In the fourth case special solutions
in terms of Bessel functions are obtained. These solutions contain known models
as special cases.
| [
{
"created": "Thu, 21 Apr 2005 13:36:44 GMT",
"version": "v1"
}
] | 2009-11-11 | [
[
"Hansraj",
"S.",
""
],
[
"Maharaj",
"S. D.",
""
],
[
"Msomi",
"A. M.",
""
],
[
"Govinder",
"K. S.",
""
]
] | We seek exact solutions to the Einstein field equations which arise when two spacetime geometries are conformally related. Whilst this is a simple method to generate new solutions to the field equations, very few such examples have been found in practice. We use the method of Lie analysis of differential equations to obtain new group invariant solutions to conformally related Petrov type D spacetimes. Four cases arise depending on the nature of the Lie symmetry generator. In three cases we are in a position to solve the master field equation in terms of elementary functions. In the fourth case special solutions in terms of Bessel functions are obtained. These solutions contain known models as special cases. |
gr-qc/9903089 | Petr Hajicek | Petr Hajicek (University of Berne, Switzerland) | Choice of Gauge in Quantum Gravity | Latex, 8 pages, no figures, Europian size (to get American size,
delete the preambel) | null | null | BUTP-99/05 | gr-qc | null | This paper is an extended version of the talk given at 19th Texas Symposium
of Relativistic Astrophysics and Cosmology, Paris, 1998. It reviews of some
recent work; mathematical details are skipped. It is well-known that a choice
of gauge in generally covariant models has a twofold pupose: not only to render
the dynamics unique, but also to define the spacetime points. A geometric way
of choosing gauge that is not based on coordinate conditions---the so-called
covariant gauge fixing---is described. After a covariant gauge fixing, the
dynamics is unique and the background manifold points are well-defined, but the
description remains invariant with respect to all diffeomorphisms of the
background manifold. Transformations between different covariant gauge fixings
form the well-known Bergmann-Komar group. Each covariant gauge fixing
determines a so-called Kucha\v{r} decomposition. The construction of the
quantum theory is based on the Kucha\v{r} form of the action and the Dirac
method of operator constraints. It is demonstrated that the Bergmann-Komar
group is too large to be implementable by unitary maps in the quantum domain.
| [
{
"created": "Wed, 24 Mar 1999 09:54:59 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Hajicek",
"Petr",
"",
"University of Berne, Switzerland"
]
] | This paper is an extended version of the talk given at 19th Texas Symposium of Relativistic Astrophysics and Cosmology, Paris, 1998. It reviews of some recent work; mathematical details are skipped. It is well-known that a choice of gauge in generally covariant models has a twofold pupose: not only to render the dynamics unique, but also to define the spacetime points. A geometric way of choosing gauge that is not based on coordinate conditions---the so-called covariant gauge fixing---is described. After a covariant gauge fixing, the dynamics is unique and the background manifold points are well-defined, but the description remains invariant with respect to all diffeomorphisms of the background manifold. Transformations between different covariant gauge fixings form the well-known Bergmann-Komar group. Each covariant gauge fixing determines a so-called Kucha\v{r} decomposition. The construction of the quantum theory is based on the Kucha\v{r} form of the action and the Dirac method of operator constraints. It is demonstrated that the Bergmann-Komar group is too large to be implementable by unitary maps in the quantum domain. |
gr-qc/0103062 | Zeferino Andrade | Zeferino Andrade | Trapped and excited w modes of stars with a phase transition and R>=5M | To appear in Physical Review D | Phys.Rev. D63 (2001) 124002 | 10.1103/PhysRevD.63.124002 | null | gr-qc astro-ph | null | The trapped $w$-modes of stars with a first order phase transition (a density
discontinuity) are computed and the excitation of some of the modes of these
stars by a perturbing shell is investigated. Attention is restricted to odd
parity (``axial'') $w$-modes. With $R$ the radius of the star, $M$ its mass,
$R_{i}$ the radius of the inner core and $M_{i}$ the mass of such core, it is
shown that stars with $R/M\geq 5$ can have several trapped $w$-modes, as long
as $R_{i}/M_{i}<2.6$. Excitation of the least damped $w$-mode is confirmed for
a few models. All of these stars can only exist however, for values of the
ratio between the densities of the two phases, greater than $\sim 46$. We also
show that stars with a phase transition and a given value of $R/M$ can have far
more trapped modes than a homogeneous single density star with the same value
of $R/M$, provided both $R/M$ and $R_{i}/M_{i}$ are smaller than 3. If the
phase transition is very fast, most of the stars with trapped modes are
unstable to radial oscillations. We compute the time of instability, and find
it to be comparable to the damping of the $w$-mode excited in most cases where
$w$-mode excitation is likely. If on the other hand the phase transition is
slow, all the stars are stable to radial oscillations.
| [
{
"created": "Fri, 16 Mar 2001 13:42:29 GMT",
"version": "v1"
}
] | 2009-11-07 | [
[
"Andrade",
"Zeferino",
""
]
] | The trapped $w$-modes of stars with a first order phase transition (a density discontinuity) are computed and the excitation of some of the modes of these stars by a perturbing shell is investigated. Attention is restricted to odd parity (``axial'') $w$-modes. With $R$ the radius of the star, $M$ its mass, $R_{i}$ the radius of the inner core and $M_{i}$ the mass of such core, it is shown that stars with $R/M\geq 5$ can have several trapped $w$-modes, as long as $R_{i}/M_{i}<2.6$. Excitation of the least damped $w$-mode is confirmed for a few models. All of these stars can only exist however, for values of the ratio between the densities of the two phases, greater than $\sim 46$. We also show that stars with a phase transition and a given value of $R/M$ can have far more trapped modes than a homogeneous single density star with the same value of $R/M$, provided both $R/M$ and $R_{i}/M_{i}$ are smaller than 3. If the phase transition is very fast, most of the stars with trapped modes are unstable to radial oscillations. We compute the time of instability, and find it to be comparable to the damping of the $w$-mode excited in most cases where $w$-mode excitation is likely. If on the other hand the phase transition is slow, all the stars are stable to radial oscillations. |
2010.03299 | Jaros{\l}aw Kopi\'nski | Jaros{\l}aw Kopi\'nski and Juan A. Valiente Kroon | New spinorial approach to mass inequalities for black holes in general
relativity | v3: minor corrections | Phys. Rev. D 103, 024057 (2021) | 10.1103/PhysRevD.103.024057 | null | gr-qc math-ph math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A new spinorial strategy for the construction of geometric inequalities
involving the Arnowitt-Deser-Misner (ADM) mass of black hole systems in general
relativity is presented. This approach is based on a second order elliptic
equation (the approximate twistor equation) for a valence 1 Weyl spinor. This
has the advantage over other spinorial approaches to the construction of
geometric inequalities based on the Sen-Witten-Dirac equation that it allows to
specify boundary conditions for the two components of the spinor. This greater
control on the boundary data has the potential of giving rise to new geometric
inequalities involving the mass. In particular, it is shown that the mass is
bounded from below by an integral functional over a marginally outer trapped
surface (MOTS) which depends on a freely specifiable valence 1 spinor. From
this main inequality, by choosing the free data in an appropriate way, one
obtains a new nontrivial bounds of the mass in terms of the inner expansion of
the MOTS. The analysis makes use of a new formalism for the $1+1+2$
decomposition of spinorial equations.
| [
{
"created": "Wed, 7 Oct 2020 09:25:36 GMT",
"version": "v1"
},
{
"created": "Sun, 24 Jan 2021 11:18:49 GMT",
"version": "v2"
},
{
"created": "Tue, 30 May 2023 08:51:54 GMT",
"version": "v3"
}
] | 2023-05-31 | [
[
"Kopiński",
"Jarosław",
""
],
[
"Kroon",
"Juan A. Valiente",
""
]
] | A new spinorial strategy for the construction of geometric inequalities involving the Arnowitt-Deser-Misner (ADM) mass of black hole systems in general relativity is presented. This approach is based on a second order elliptic equation (the approximate twistor equation) for a valence 1 Weyl spinor. This has the advantage over other spinorial approaches to the construction of geometric inequalities based on the Sen-Witten-Dirac equation that it allows to specify boundary conditions for the two components of the spinor. This greater control on the boundary data has the potential of giving rise to new geometric inequalities involving the mass. In particular, it is shown that the mass is bounded from below by an integral functional over a marginally outer trapped surface (MOTS) which depends on a freely specifiable valence 1 spinor. From this main inequality, by choosing the free data in an appropriate way, one obtains a new nontrivial bounds of the mass in terms of the inner expansion of the MOTS. The analysis makes use of a new formalism for the $1+1+2$ decomposition of spinorial equations. |
gr-qc/0509067 | David Lonie | G.S. Hall and D.P. Lonie | On the compatibility of Lorentz-metrics with linear connections on
4-dimensional manifolds | LaTex2e, 19 pages, uses iop style files | J.Phys. A39 (2006) 2995-3010 | 10.1088/0305-4470/39/12/009 | null | gr-qc | null | This paper considers 4-dimensional manifolds upon which there is a Lorentz
metric, h, and a symmetric connection and which are originally assumed
unrelated. It then derives sufficient conditions on the metric and connection
(expressed through the curvature tensor) for the connection to be the
Levi-Civita connection of some (local) Lorentz metric, g, and calculates the
relationship between g and h. Some examples are provided which help to assess
the strength of the sufficient conditions derived.
| [
{
"created": "Fri, 16 Sep 2005 11:49:20 GMT",
"version": "v1"
}
] | 2009-11-11 | [
[
"Hall",
"G. S.",
""
],
[
"Lonie",
"D. P.",
""
]
] | This paper considers 4-dimensional manifolds upon which there is a Lorentz metric, h, and a symmetric connection and which are originally assumed unrelated. It then derives sufficient conditions on the metric and connection (expressed through the curvature tensor) for the connection to be the Levi-Civita connection of some (local) Lorentz metric, g, and calculates the relationship between g and h. Some examples are provided which help to assess the strength of the sufficient conditions derived. |
gr-qc/0403054 | Valeri Frolov | Valeri P. Frolov, Dmitri V. Fursaev, and Dejan Stojkovic | Interaction of higher-dimensional rotating black holes with branes | Version published in Class. Quant. Grav | Class.Quant.Grav. 21 (2004) 3483-3498 | 10.1088/0264-9381/21/14/011 | Alberta-Thy-05-04, MCTP-04-20 | gr-qc hep-ph hep-th | null | We study interaction of rotating higher dimensional black holes with a brane
in space-times with large extra dimensions. We demonstrate that in a general
case a rotating black hole attached to a brane can loose bulk components of its
angular momenta. A stationary black hole can have only those components of the
angular momenta which are connected with Killing vectors generating
transformations preserving a position of the brane. In a final stationary state
the null Killing vector generating the black hole horizon is tangent to the
brane. We discuss first the interaction of a cosmic string and a domain wall
with the 4D Kerr black hole. We then prove the general result for slowly
rotating higher dimensional black holes interacting with branes. The
characteristic time when a rotating black hole with the gravitational radius
$r_0$ reaches this final stationary state is $T\sim r_0^{p-1}/(G\sigma)$, where
$G$ is the higher dimensional gravitational coupling constant, $\sigma$ is the
brane tension, and $p$ is the number of extra dimensions.
| [
{
"created": "Sat, 13 Mar 2004 00:08:58 GMT",
"version": "v1"
},
{
"created": "Tue, 15 Jun 2004 23:28:06 GMT",
"version": "v2"
},
{
"created": "Wed, 28 Jul 2004 17:10:55 GMT",
"version": "v3"
}
] | 2009-11-10 | [
[
"Frolov",
"Valeri P.",
""
],
[
"Fursaev",
"Dmitri V.",
""
],
[
"Stojkovic",
"Dejan",
""
]
] | We study interaction of rotating higher dimensional black holes with a brane in space-times with large extra dimensions. We demonstrate that in a general case a rotating black hole attached to a brane can loose bulk components of its angular momenta. A stationary black hole can have only those components of the angular momenta which are connected with Killing vectors generating transformations preserving a position of the brane. In a final stationary state the null Killing vector generating the black hole horizon is tangent to the brane. We discuss first the interaction of a cosmic string and a domain wall with the 4D Kerr black hole. We then prove the general result for slowly rotating higher dimensional black holes interacting with branes. The characteristic time when a rotating black hole with the gravitational radius $r_0$ reaches this final stationary state is $T\sim r_0^{p-1}/(G\sigma)$, where $G$ is the higher dimensional gravitational coupling constant, $\sigma$ is the brane tension, and $p$ is the number of extra dimensions. |
gr-qc/0109048 | Valter Moretti | Valter Moretti (Math.Dept.-Trento Univ.) | Comments on the Stress-Energy Tensor Operator in Curved Spacetime | 35 pages, no figure, LaTeX2e. Final form accepted for publication in
Commun.Math.Phys | Commun.Math.Phys. 232 (2003) 189-221 | 10.1007/s00220-002-0702-7 | UTM 601 | gr-qc hep-th math-ph math.MP | null | Hollands and Wald's technique based on *-algebras of Wick products of field
operators is strightforwardly generalized to define the stress-energy tensor
operator in curved globally hyperbolic spacetimes. In particular, the locality
and covariance requirement is generalized to Wick products of differentiated
quantum fields. The proposed stress-energy tensor operator is conserved and
reduces to the classical form if field operators are replaced by classical
fields satisfying the equation of motion. The definition is based on the
existence of convenient counterterms given by certain local Wick products of
differentiated fields. They are independent from the arbitrary length scale
(and any quantum state) and they classically vanish on solutions of field
equation. The averaged stress-energy tensor with respect to Hadamard quantum
states can be obtained by an improved point-splitting renormalization procedure
which makes use of the nonambiguous part of the Hadamard parametrix only that
is completely determined by the local geometry and the parameters which appear
in the Klein-Gordon operator. The averaged stress-energy tensor also coincides
with that found by employing the local $\zeta$-function approach.
| [
{
"created": "Thu, 13 Sep 2001 14:37:34 GMT",
"version": "v1"
},
{
"created": "Tue, 14 May 2002 15:30:38 GMT",
"version": "v2"
}
] | 2009-11-07 | [
[
"Moretti",
"Valter",
"",
"Math.Dept.-Trento Univ."
]
] | Hollands and Wald's technique based on *-algebras of Wick products of field operators is strightforwardly generalized to define the stress-energy tensor operator in curved globally hyperbolic spacetimes. In particular, the locality and covariance requirement is generalized to Wick products of differentiated quantum fields. The proposed stress-energy tensor operator is conserved and reduces to the classical form if field operators are replaced by classical fields satisfying the equation of motion. The definition is based on the existence of convenient counterterms given by certain local Wick products of differentiated fields. They are independent from the arbitrary length scale (and any quantum state) and they classically vanish on solutions of field equation. The averaged stress-energy tensor with respect to Hadamard quantum states can be obtained by an improved point-splitting renormalization procedure which makes use of the nonambiguous part of the Hadamard parametrix only that is completely determined by the local geometry and the parameters which appear in the Klein-Gordon operator. The averaged stress-energy tensor also coincides with that found by employing the local $\zeta$-function approach. |
1104.3719 | Subenoy Chakraborty | Ritabrata biswas, Subenoy Chakraborty | Black Hole Thermodynamics in Horava Lifshitz Gravity and the Related
Geometry | 8 figures | Astrophys.Space Sci.332:193,2011 | 10.1007/s10509-010-0504-x | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Recently, Ho$\breve{r}$ava proposed a non-relativistic renormalizable theory
of gravity which is essentially a field theoretic model for a UV complete
theory of gravity and reduces to Einstein gravity with a non-vanishing
cosmological constant in IR. Also the theory admits a Lifshitz scale-invariance
in time and space with broken Lorentz symmetry at short scale. On the other
hand, at large distances higher derivative terms do not contribute and the
theory coincides with general relativity. Subsequently, Cai and his
collaborators and then Catiuo et al have obtained black hole solutions in this
gravity theory and studied the thermodynamic properties of the black hole
solution. In the present paper, we have investigated the black hole
thermodynamic for two choices of the entropy function - a classical and a
topological in nature. Finally, it is examined whether a phase transition is
possible or not.
| [
{
"created": "Tue, 19 Apr 2011 12:02:11 GMT",
"version": "v1"
}
] | 2015-03-19 | [
[
"biswas",
"Ritabrata",
""
],
[
"Chakraborty",
"Subenoy",
""
]
] | Recently, Ho$\breve{r}$ava proposed a non-relativistic renormalizable theory of gravity which is essentially a field theoretic model for a UV complete theory of gravity and reduces to Einstein gravity with a non-vanishing cosmological constant in IR. Also the theory admits a Lifshitz scale-invariance in time and space with broken Lorentz symmetry at short scale. On the other hand, at large distances higher derivative terms do not contribute and the theory coincides with general relativity. Subsequently, Cai and his collaborators and then Catiuo et al have obtained black hole solutions in this gravity theory and studied the thermodynamic properties of the black hole solution. In the present paper, we have investigated the black hole thermodynamic for two choices of the entropy function - a classical and a topological in nature. Finally, it is examined whether a phase transition is possible or not. |
gr-qc/0003019 | Lorenzo Fatibene | L. Fatibene, M. Ferraris, M. Francaviglia, M. Raiteri | Noether Charges, Brown-York Quasilocal Energy and Related Topics | 43 pages, 3 figures, PlainTeX file | J.Math.Phys.42:1173-1195,2001 | 10.1063/1.1336514 | null | gr-qc | null | The Lagrangian proposed by York et al. and the covariant first order
Lagrangian for General Relativity are introduced to deal with the (vacuum)
gravitational field on a reference background. The two Lagrangians are compared
and we show that the first one can be obtained from the latter under suitable
hypotheses. The induced variational principles are also compared and discussed.
A conditioned correspondence among Noether conserved quantities, quasilocal
energy and the standard Hamiltonian obtained by 3+1 decomposition is also
established. As a result, it turns out that the covariant first order
Lagrangian is better suited whenever a reference background field has to be
taken into account, as it is commonly accepted when dealing with conserved
quantities in non-asymptotically flat spacetimes. As a further advantage of the
use of a covariant first order Lagrangian, we show that all the quantities
computed are manifestly covariant, as it is appropriate in General Relativity.
| [
{
"created": "Tue, 7 Mar 2000 13:27:05 GMT",
"version": "v1"
}
] | 2014-11-17 | [
[
"Fatibene",
"L.",
""
],
[
"Ferraris",
"M.",
""
],
[
"Francaviglia",
"M.",
""
],
[
"Raiteri",
"M.",
""
]
] | The Lagrangian proposed by York et al. and the covariant first order Lagrangian for General Relativity are introduced to deal with the (vacuum) gravitational field on a reference background. The two Lagrangians are compared and we show that the first one can be obtained from the latter under suitable hypotheses. The induced variational principles are also compared and discussed. A conditioned correspondence among Noether conserved quantities, quasilocal energy and the standard Hamiltonian obtained by 3+1 decomposition is also established. As a result, it turns out that the covariant first order Lagrangian is better suited whenever a reference background field has to be taken into account, as it is commonly accepted when dealing with conserved quantities in non-asymptotically flat spacetimes. As a further advantage of the use of a covariant first order Lagrangian, we show that all the quantities computed are manifestly covariant, as it is appropriate in General Relativity. |
2206.03338 | Masroor C. Pookkillath | Antonio De Felice, Shinji Mukohyama, Masroor C. Pookkillath | Extended minimal theories of massive gravity | 20 pages+appendices, 1 figure | null | 10.1103/PhysRevD.106.084050 | YITP-22-59, IPMU22-0035 | gr-qc astro-ph.CO hep-th | http://creativecommons.org/licenses/by/4.0/ | In this work, we introduce a class of extended Minimal Theories of Massive
Gravity (eMTMG), without requiring a priori that the theory should admit the
same homogeneous and isotropic cosmological solutions as the de
Rham-Gabadadze-Tolley massive gravity. The theory is constructed as to have
only two degrees of freedom in the gravity sector. In order to perform this
step we first introduce a precursor theory endowed with a general graviton mass
term, to which, at the level of the Hamiltonian, we add two extra constraints
as to remove the unwanted degrees of freedom, which otherwise would typically
lead to ghosts and/or instabilities. On analyzing the number of independent
constraints and the properties of tensor mode perturbations, we see that the
gravitational waves are the only propagating gravitational degrees of freedom
which do acquire a non-trivial mass, as expected. In order to understand how
the effective gravitational force works for this theory we then investigate
cosmological scalar perturbations in the presence of a pressureless fluid. We
then restrict the whole class of models by imposing the following conditions at
all times: 1) it is possible to define an effective gravitational constant,
$G_{{\rm eff}}$; 2) the value $G_{\text{eff}}/G_{N}$ is always finite but not
always equal to unity (as to allow some non-trivial modifications of gravity,
besides the massive tensorial modes); and 3) the square of mass of the graviton
is always positive. These constraints automatically make also the ISW-effect
contributions finite at all times. Finally we focus on a simple subclass of
such theories, and show they already can give a rich and interesting
phenomenology.
| [
{
"created": "Tue, 7 Jun 2022 14:21:50 GMT",
"version": "v1"
}
] | 2022-11-09 | [
[
"De Felice",
"Antonio",
""
],
[
"Mukohyama",
"Shinji",
""
],
[
"Pookkillath",
"Masroor C.",
""
]
] | In this work, we introduce a class of extended Minimal Theories of Massive Gravity (eMTMG), without requiring a priori that the theory should admit the same homogeneous and isotropic cosmological solutions as the de Rham-Gabadadze-Tolley massive gravity. The theory is constructed as to have only two degrees of freedom in the gravity sector. In order to perform this step we first introduce a precursor theory endowed with a general graviton mass term, to which, at the level of the Hamiltonian, we add two extra constraints as to remove the unwanted degrees of freedom, which otherwise would typically lead to ghosts and/or instabilities. On analyzing the number of independent constraints and the properties of tensor mode perturbations, we see that the gravitational waves are the only propagating gravitational degrees of freedom which do acquire a non-trivial mass, as expected. In order to understand how the effective gravitational force works for this theory we then investigate cosmological scalar perturbations in the presence of a pressureless fluid. We then restrict the whole class of models by imposing the following conditions at all times: 1) it is possible to define an effective gravitational constant, $G_{{\rm eff}}$; 2) the value $G_{\text{eff}}/G_{N}$ is always finite but not always equal to unity (as to allow some non-trivial modifications of gravity, besides the massive tensorial modes); and 3) the square of mass of the graviton is always positive. These constraints automatically make also the ISW-effect contributions finite at all times. Finally we focus on a simple subclass of such theories, and show they already can give a rich and interesting phenomenology. |
2403.13028 | Sujay Kr. Biswas | Goutam Mandal and Sujay Kr. Biswas | Dynamical systems analysis of a cosmological model with interacting
Umami Chaplygin fluid in adiabatic particle creation mechanism: Some bouncing
features | 29 pages, 12 captioned figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The present work aims to investigate an interacting Umami Chaplygin gas in
the background dynamics of a spatially flat Friedmann-Lemaitre-Robertson-Walker
(FLRW) universe when adiabatic particle creation is allowed. Here, the universe
is taken to be an open thermodynamical model where the particle is created
irreversibly and consequently, the creation pressure comes into the
energy-momentum tensor of the material content. The rate at which the particle
created is assumed to have a linear relation with the Hubble parameter and the
created particle is dark matter (pressureless). The Umami Chaplygin gas is
considered dark energy, pressureless dust is taken as dark matter and a
phenomenological interaction term is taken for mathematical simplicity.
Dynamical analysis is performed to obtain an overall evolution of the model we
consider. The autonomous system is obtained by considering dimensionless
variables in terms of cosmological variables. The local stability of the
critical points and the classical stability of the model are also performed at
each critical point. This study explores some cosmologically viable scenarios
when we constrain the model parameters. Some critical points exhibit the
accelerated de Sitter expansion of the universe at both the early phase as well
as the late phase of evolution which is characterized by completely Umami
Chaplygin fluid equation of state. Scaling solutions are also described by some
other critical points showing late-time accelerated attractors in phase space
satisfying present observational data, and solving the coincidence problem. A
unified cosmic evolution is also achieved within this model describing the
evolution of the universe starting from inflation to late time acceleration
connecting through a matter-dominated intermediate phase. Finally, the
non-singular bouncing behavior of the universe is also investigated for this
model numerically.
| [
{
"created": "Tue, 19 Mar 2024 03:27:55 GMT",
"version": "v1"
}
] | 2024-03-21 | [
[
"Mandal",
"Goutam",
""
],
[
"Biswas",
"Sujay Kr.",
""
]
] | The present work aims to investigate an interacting Umami Chaplygin gas in the background dynamics of a spatially flat Friedmann-Lemaitre-Robertson-Walker (FLRW) universe when adiabatic particle creation is allowed. Here, the universe is taken to be an open thermodynamical model where the particle is created irreversibly and consequently, the creation pressure comes into the energy-momentum tensor of the material content. The rate at which the particle created is assumed to have a linear relation with the Hubble parameter and the created particle is dark matter (pressureless). The Umami Chaplygin gas is considered dark energy, pressureless dust is taken as dark matter and a phenomenological interaction term is taken for mathematical simplicity. Dynamical analysis is performed to obtain an overall evolution of the model we consider. The autonomous system is obtained by considering dimensionless variables in terms of cosmological variables. The local stability of the critical points and the classical stability of the model are also performed at each critical point. This study explores some cosmologically viable scenarios when we constrain the model parameters. Some critical points exhibit the accelerated de Sitter expansion of the universe at both the early phase as well as the late phase of evolution which is characterized by completely Umami Chaplygin fluid equation of state. Scaling solutions are also described by some other critical points showing late-time accelerated attractors in phase space satisfying present observational data, and solving the coincidence problem. A unified cosmic evolution is also achieved within this model describing the evolution of the universe starting from inflation to late time acceleration connecting through a matter-dominated intermediate phase. Finally, the non-singular bouncing behavior of the universe is also investigated for this model numerically. |
2007.05464 | Marcello Ortaggio | Sigbj{\o}rn Hervik, Marcello Ortaggio | Universal $p$-form black holes in generalized theories of gravity | 15 pages. v2: typos fixed, minor improvements to the text, refs.
added | Eur. Phys. J. C 80, 1020 (2020) | 10.1140/epjc/s10052-020-08571-x | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We explore how far one can go in constructing $d$-dimensional static black
holes coupled to $p$-form and scalar fields before actually specifying the
gravity and electrodynamics theory one wants to solve. At the same time, we
study to what extent one can enlarge the space of black hole solutions by
allowing for horizon geometries more general than spaces of constant curvature.
We prove that a generalized Schwarzschild-like ansatz with an arbitrary
isotropy-irreducible homogeneous base space (IHS) provides an answer to both
questions, up to naturally adapting the gauge fields to the spacetime geometry.
In particular, an IHS-K\"ahler base space enables one to construct magnetic and
dyonic 2-form solutions in a large class of theories, including non-minimally
couplings. We exemplify our results by constructing simple solutions to
particular theories such as $R^2$, Gauss-Bonnet and (a sector of)
Einstein-Horndeski gravity coupled to certain $p$-form and conformally
invariant electrodynamics.
| [
{
"created": "Fri, 10 Jul 2020 16:06:42 GMT",
"version": "v1"
},
{
"created": "Wed, 11 Nov 2020 11:58:18 GMT",
"version": "v2"
}
] | 2020-11-12 | [
[
"Hervik",
"Sigbjørn",
""
],
[
"Ortaggio",
"Marcello",
""
]
] | We explore how far one can go in constructing $d$-dimensional static black holes coupled to $p$-form and scalar fields before actually specifying the gravity and electrodynamics theory one wants to solve. At the same time, we study to what extent one can enlarge the space of black hole solutions by allowing for horizon geometries more general than spaces of constant curvature. We prove that a generalized Schwarzschild-like ansatz with an arbitrary isotropy-irreducible homogeneous base space (IHS) provides an answer to both questions, up to naturally adapting the gauge fields to the spacetime geometry. In particular, an IHS-K\"ahler base space enables one to construct magnetic and dyonic 2-form solutions in a large class of theories, including non-minimally couplings. We exemplify our results by constructing simple solutions to particular theories such as $R^2$, Gauss-Bonnet and (a sector of) Einstein-Horndeski gravity coupled to certain $p$-form and conformally invariant electrodynamics. |
0808.3828 | Hideyoshi Arakida | Hideyoshi Arakida | Time Delay in Robertson-McVittie Spacetime and its Application to
Increase of Astronomical Unit | 15 pages, 1 figure, accepted for publication in New Astronomy | New Astronomy, Volume 14, Issue 3, p. 264-268 (2009( | 10.1016/j.newast.2008.08.010 | null | gr-qc astro-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We investigated the light propagation by means of the Robertson-McVittie
solution which is considered to be the spacetime around the gravitating body
embedded in the FLRW (Friedmann-Lema{\^i}tre-Robertson-Walker) background
metric. We concentrated on the time delay and derived the correction terms with
respect to the Shapiro's formula. To relate with the actual observation and its
reduction process, we also took account of the time transformations; coordinate
time to proper one, and conversely, proper time to coordinate one. We applied
these results to the problem of increase of astronomical unit reported by
Krasinsky and Brumberg (2004). However, we found the influence of the
cosmological expansion on the light propagation does not give an explanation of
observed value, $d{\rm AU}/dt = 15 \pm 4$ [m/century] in the framework of
Robertson-McVittie metric.
| [
{
"created": "Thu, 28 Aug 2008 06:02:54 GMT",
"version": "v1"
}
] | 2012-02-07 | [
[
"Arakida",
"Hideyoshi",
""
]
] | We investigated the light propagation by means of the Robertson-McVittie solution which is considered to be the spacetime around the gravitating body embedded in the FLRW (Friedmann-Lema{\^i}tre-Robertson-Walker) background metric. We concentrated on the time delay and derived the correction terms with respect to the Shapiro's formula. To relate with the actual observation and its reduction process, we also took account of the time transformations; coordinate time to proper one, and conversely, proper time to coordinate one. We applied these results to the problem of increase of astronomical unit reported by Krasinsky and Brumberg (2004). However, we found the influence of the cosmological expansion on the light propagation does not give an explanation of observed value, $d{\rm AU}/dt = 15 \pm 4$ [m/century] in the framework of Robertson-McVittie metric. |
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