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 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
1707.07774 | Geoffrey Lovelace | Geoffrey Lovelace, Nicholas Demos and Haroon Khan | Numerically modeling Brownian thermal noise in amorphous and crystalline
thin coatings | 23 pages, 6 figures, submitted to Classical and Quantum Gravity | null | 10.1088/1361-6382/aa9ccc | LIGO-P1700183 | gr-qc physics.ins-det | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Thermal noise is expected to be one of the noise sources limiting the
astrophysical reach of Advanced LIGO (once commissioning is complete) and
third-generation detectors. Adopting crystalline materials for thin, reflecting
mirror coatings, rather than the amorphous coatings used in current-generation
detectors, could potentially reduce thermal noise. Understanding and reducing
thermal noise requires accurate theoretical models, but modeling thermal noise
analytically is especially challenging with crystalline materials. Thermal
noise models typically rely on the fluctuation-dissipation theorem, which
relates the power spectral density of the thermal noise to an auxiliary elastic
problem. In this paper, we present results from a new, open-source tool that
numerically solves the auxiliary elastic problem to compute the Brownian
thermal noise for both amorphous and crystalline coatings. We employ
open-source frameworks to solve the auxiliary elastic problem using a
finite-element method, adaptive mesh refinement, and parallel processing that
enables us to use high resolutions capable of resolving the thin reflective
coating. We compare with approximate analytic solutions for amorphous
materials, and we verify that our solutions scale as expected. Finally, we
model the crystalline coating thermal noise in an experiment reported by Cole
and collaborators (2013), comparing our results to a simpler numerical
calculation that treats the coating as an "effectively amorphous" material. We
find that treating the coating as a cubic crystal instead of as an effectively
amorphous material increases the thermal noise by about 3%. Our results are a
step toward better understanding and reducing thermal noise to increase the
reach of future gravitational-wave detectors. (Abstract abbreviated.)
| [
{
"created": "Mon, 24 Jul 2017 23:52:43 GMT",
"version": "v1"
}
] | 2018-01-10 | [
[
"Lovelace",
"Geoffrey",
""
],
[
"Demos",
"Nicholas",
""
],
[
"Khan",
"Haroon",
""
]
] | Thermal noise is expected to be one of the noise sources limiting the astrophysical reach of Advanced LIGO (once commissioning is complete) and third-generation detectors. Adopting crystalline materials for thin, reflecting mirror coatings, rather than the amorphous coatings used in current-generation detectors, could potentially reduce thermal noise. Understanding and reducing thermal noise requires accurate theoretical models, but modeling thermal noise analytically is especially challenging with crystalline materials. Thermal noise models typically rely on the fluctuation-dissipation theorem, which relates the power spectral density of the thermal noise to an auxiliary elastic problem. In this paper, we present results from a new, open-source tool that numerically solves the auxiliary elastic problem to compute the Brownian thermal noise for both amorphous and crystalline coatings. We employ open-source frameworks to solve the auxiliary elastic problem using a finite-element method, adaptive mesh refinement, and parallel processing that enables us to use high resolutions capable of resolving the thin reflective coating. We compare with approximate analytic solutions for amorphous materials, and we verify that our solutions scale as expected. Finally, we model the crystalline coating thermal noise in an experiment reported by Cole and collaborators (2013), comparing our results to a simpler numerical calculation that treats the coating as an "effectively amorphous" material. We find that treating the coating as a cubic crystal instead of as an effectively amorphous material increases the thermal noise by about 3%. Our results are a step toward better understanding and reducing thermal noise to increase the reach of future gravitational-wave detectors. (Abstract abbreviated.) |
1301.2120 | Antonio Jes\'us L\'opez Revelles | Antonio Jes\'us L\'opez-Revelles | Growth of matter perturbations for realistic $F(R)$ models | 24 pages, 14 figures, submitted to PRD | null | 10.1103/PhysRevD.87.024021 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Two different realistic $F(R)$ modified gravity models are considered in the
framework of the Friedmann-Lemetre-Robertson-Walker universe. The parameters of
these two models are adjusted to reach coherence with the most recent and
accurate observations of the current universe. A study of the growth of matter
density perturbations is done, and several parametrizations of the growth index
are developed for both models. The ansatz for the growth index given by $\gamma
= \gamma_0 + \gamma_1 z/(1+z)$ seems to be the best parametrization for the two
models considered. Finally, the values obtained for $\gamma_0$ and $\gamma_1$
can be used in order to characterize these two models and to differentiate them
from others such as the Hu-Sawicki model.
| [
{
"created": "Thu, 10 Jan 2013 13:46:58 GMT",
"version": "v1"
}
] | 2015-06-12 | [
[
"López-Revelles",
"Antonio Jesús",
""
]
] | Two different realistic $F(R)$ modified gravity models are considered in the framework of the Friedmann-Lemetre-Robertson-Walker universe. The parameters of these two models are adjusted to reach coherence with the most recent and accurate observations of the current universe. A study of the growth of matter density perturbations is done, and several parametrizations of the growth index are developed for both models. The ansatz for the growth index given by $\gamma = \gamma_0 + \gamma_1 z/(1+z)$ seems to be the best parametrization for the two models considered. Finally, the values obtained for $\gamma_0$ and $\gamma_1$ can be used in order to characterize these two models and to differentiate them from others such as the Hu-Sawicki model. |
1210.5542 | Owen Pavel Fern\'andez Piedra | Owen Pavel Fern\'andez Piedra, J. Bernal Castillo, Y. Jim\'enez
Santana and L. Figueredo Noris | Fermion perturbations in string-theory black holes II: the higher
dimensional case | 32 pages, 8 figures | null | null | GEA-UCF 2012-2 | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper we report the results of a detailed investigation of the
complete time evolution of massless fermion fields propagating in spacetimes of
higher dimensional stringy black hole solutions, obtained from intersecting
branes in string/$M$ theory. We write the Dirac equation in $D$-dimensional
spacetime in a form suitable to perform a numerical integration of it, and
using a Prony fitting of the time domain data, we determine the quasinormal
frequencies that characterize the test field evolution at intermediary times.
We also present the results obtained for the quasinormal frequencies using a
sixth order WKB approximation, that are in perfect agreement with the numerical
results. The power law exponents that describe the field relaxation at very
late times are also determined, and we show that they depends upon the
dimensionality of space-time, and are identical to that associated with the
relaxation of boson fields for odd dimensions. The dependance of the
frequencies and damping factor of the spinor field with the charges of the
stringy black hole are studied.
| [
{
"created": "Fri, 19 Oct 2012 21:28:01 GMT",
"version": "v1"
},
{
"created": "Thu, 15 Nov 2012 19:20:34 GMT",
"version": "v2"
}
] | 2012-11-16 | [
[
"Piedra",
"Owen Pavel Fernández",
""
],
[
"Castillo",
"J. Bernal",
""
],
[
"Santana",
"Y. Jiménez",
""
],
[
"Noris",
"L. Figueredo",
""
]
] | In this paper we report the results of a detailed investigation of the complete time evolution of massless fermion fields propagating in spacetimes of higher dimensional stringy black hole solutions, obtained from intersecting branes in string/$M$ theory. We write the Dirac equation in $D$-dimensional spacetime in a form suitable to perform a numerical integration of it, and using a Prony fitting of the time domain data, we determine the quasinormal frequencies that characterize the test field evolution at intermediary times. We also present the results obtained for the quasinormal frequencies using a sixth order WKB approximation, that are in perfect agreement with the numerical results. The power law exponents that describe the field relaxation at very late times are also determined, and we show that they depends upon the dimensionality of space-time, and are identical to that associated with the relaxation of boson fields for odd dimensions. The dependance of the frequencies and damping factor of the spinor field with the charges of the stringy black hole are studied. |
2303.12168 | Sunil Kumar Tripathy Dr. | S. K. Tripathy, S. K. Pradhan, B. Barik, Z. Naik and B. Mishra | Evolution of Generalized Brans-Dicke parameter within a Superbounce
scenario | 10 pages, 5 figures, accepted version of the journal Symmetry | Symmetry 2023, 15(4), 790 | 10.3390/sym15040790 | null | gr-qc hep-th | http://creativecommons.org/licenses/by/4.0/ | We have studied a superbounce scenario in a set up of Brans-Dicke (BD)
theory. The BD parameter is considered to be time dependent and is assumed to
evolve with the Brans-Dicke scalar field. In the superbounce scenario, the
model bounces at an epoch corresponding to a Big Crunch provided the ekpyrotic
phase continues until that time. Within the given superbounce scenario, we
investigate the evolution of the BD parameter for different equations of state.
We chose an axially symmetric metric that has an axial symmetry along the
x-axis. The metric is assumed to incorporate an anisotropic expansion effect.
The effect of asymmetric expansion and the anisotropic parameter on the
evolving and the non-evolving part of the BD parameter is investigated.
| [
{
"created": "Mon, 20 Mar 2023 16:17:14 GMT",
"version": "v1"
}
] | 2023-03-28 | [
[
"Tripathy",
"S. K.",
""
],
[
"Pradhan",
"S. K.",
""
],
[
"Barik",
"B.",
""
],
[
"Naik",
"Z.",
""
],
[
"Mishra",
"B.",
""
]
] | We have studied a superbounce scenario in a set up of Brans-Dicke (BD) theory. The BD parameter is considered to be time dependent and is assumed to evolve with the Brans-Dicke scalar field. In the superbounce scenario, the model bounces at an epoch corresponding to a Big Crunch provided the ekpyrotic phase continues until that time. Within the given superbounce scenario, we investigate the evolution of the BD parameter for different equations of state. We chose an axially symmetric metric that has an axial symmetry along the x-axis. The metric is assumed to incorporate an anisotropic expansion effect. The effect of asymmetric expansion and the anisotropic parameter on the evolving and the non-evolving part of the BD parameter is investigated. |
1801.02490 | Gregory Horndeski | Gregory W. Horndeski | Conformally Invariant Scalar-Vector-Tensor Field Theories Consistent
with Conservation of Charge in a Four-Dimensional Space | 40 pages. arXiv admin note: substantial text overlap with
arXiv:1708.09293 In this revised edition, I have added some additional
important references, and corrected some glaring typos | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In a four-dimensional space I shall construct all of the conformally
invariant, scalar-vector-tensor field theories that are consistent with
conservation of charge, and flat space compatible. By the last assumption I
mean that the Lagrangian of the theory in question is well defined and
differentiable when evaluated for either a flat metric tensor, (and) or
constant scalar field, (and) or vanishing vector potential. The Lagrangian of
any such field theory can be chosen to be a linear combination of six
conformally invariant scalar-vector-tensor Lagrangians, with the coefficients
being scalar functions of the scalar field. Five of these generating
Lagrangians are at most of second-order, while the sixth one is of third-order.
However, the third-order Lagrangian differs from a non-conformally invariant
second-order Lagrangian by a divergence. Consequently, all of the conformally
invariant scalar-vector-tensor field theories that are consistent with
conservation of charge, and flat space compatible, can be obtained from a
second-order Lagrangian. The vector equation of any such theory is at most of
second-order, and is an extension of Maxwell's equations, incorporating two
other first-order terms that vanish when the scalar field is constant. Hence in
regions where the scalar field is constant, the vector equation reduces to
Maxwell's.
| [
{
"created": "Fri, 5 Jan 2018 04:03:05 GMT",
"version": "v1"
},
{
"created": "Fri, 26 Jan 2018 15:29:25 GMT",
"version": "v2"
}
] | 2018-01-29 | [
[
"Horndeski",
"Gregory W.",
""
]
] | In a four-dimensional space I shall construct all of the conformally invariant, scalar-vector-tensor field theories that are consistent with conservation of charge, and flat space compatible. By the last assumption I mean that the Lagrangian of the theory in question is well defined and differentiable when evaluated for either a flat metric tensor, (and) or constant scalar field, (and) or vanishing vector potential. The Lagrangian of any such field theory can be chosen to be a linear combination of six conformally invariant scalar-vector-tensor Lagrangians, with the coefficients being scalar functions of the scalar field. Five of these generating Lagrangians are at most of second-order, while the sixth one is of third-order. However, the third-order Lagrangian differs from a non-conformally invariant second-order Lagrangian by a divergence. Consequently, all of the conformally invariant scalar-vector-tensor field theories that are consistent with conservation of charge, and flat space compatible, can be obtained from a second-order Lagrangian. The vector equation of any such theory is at most of second-order, and is an extension of Maxwell's equations, incorporating two other first-order terms that vanish when the scalar field is constant. Hence in regions where the scalar field is constant, the vector equation reduces to Maxwell's. |
gr-qc/9801110 | Kimberly C. B. New | Kimberly C. B. New (1), Keith Watt (2), Charles W. Misner (2), Joan M.
Centrella (1) ((1) Drexel University, (2) University of Maryland) | Stable 3-level leapfrog integration in numerical relativity | 14 pages and 10 postscript figures; different Hamiltonian constraint
normalization used, minor alterations to cost analysis and Conclusions
section; accepted for publication in Physical Review D | Phys.Rev. D58 (1998) 064022 | 10.1103/PhysRevD.58.064022 | null | gr-qc astro-ph | null | The 3-level leapfrog time integration algorithm is an attractive choice for
numerical relativity simulations since it is time-symmetric and avoids
non-physical damping. In Newtonian problems without velocity dependent forces,
this method enjoys the advantage of long term stability. However, for more
general differential equations, whether ordinary or partial, delayed onset
numerical instabilities can arise and destroy the solution. A known cure for
such instabilities appears to have been overlooked in many application areas.
We give an improved cure ("deloused leapfrog") that both reduces memory demands
(important for 3+1 dimensional wave equations) and allows for the use of
adaptive timesteps without a loss in accuracy. We show both that the
instability arises and that the cure we propose works in highly relativistic
problems such as tightly bound geodesics, spatially homogeneous spacetimes, and
strong gravitational waves. In the gravitational wave test case (polarized
waves in a Gowdy spacetime) the deloused leapfrog method was five to eight
times less CPU costly at various accuracies than the implicit Crank-Nicholson
method, which is not subject to this instability.
| [
{
"created": "Fri, 30 Jan 1998 21:52:19 GMT",
"version": "v1"
},
{
"created": "Fri, 26 Jun 1998 16:10:30 GMT",
"version": "v2"
}
] | 2009-10-31 | [
[
"New",
"Kimberly C. B.",
"",
"Drexel University"
],
[
"Watt",
"Keith",
"",
"University of Maryland"
],
[
"Misner",
"Charles W.",
"",
"University of Maryland"
],
[
"Centrella",
"Joan M.",
"",
"Drexel University"
]
] | The 3-level leapfrog time integration algorithm is an attractive choice for numerical relativity simulations since it is time-symmetric and avoids non-physical damping. In Newtonian problems without velocity dependent forces, this method enjoys the advantage of long term stability. However, for more general differential equations, whether ordinary or partial, delayed onset numerical instabilities can arise and destroy the solution. A known cure for such instabilities appears to have been overlooked in many application areas. We give an improved cure ("deloused leapfrog") that both reduces memory demands (important for 3+1 dimensional wave equations) and allows for the use of adaptive timesteps without a loss in accuracy. We show both that the instability arises and that the cure we propose works in highly relativistic problems such as tightly bound geodesics, spatially homogeneous spacetimes, and strong gravitational waves. In the gravitational wave test case (polarized waves in a Gowdy spacetime) the deloused leapfrog method was five to eight times less CPU costly at various accuracies than the implicit Crank-Nicholson method, which is not subject to this instability. |
1605.09506 | Chen Songbai | Mingzhi Wang, Songbai Chen, Jiliang Jing | Chaos in the motion of a test scalar particle coupling to Einstein
tensor in Schwarzschild-Melvin black hole spacetime | 18 pages, 9 figures. The title is changed, some content and
references are modified. Accepted by EPJC for publication;arXiv admin note:
text overlap with arXiv:1604.02785 | Eur. Phys. J. C (2017) 77:208 | 10.1140/epjc/s10052-017-4792-y | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present firstly the equation of motion for a test scalar particle coupling
to Einstein tensor in the Schwarzschild-Melvin black hole spacetime through the
short-wave approximation. Through analysing Poincar\'{e} sections, the power
spectrum, the fast Lyapunov exponent indicator and the bifurcation diagram, we
investigate the effects of coupling parameter on the chaotic behavior of the
particles. With the increase of the coupling strength, we find that the motion
of coupled particle for the chosen parameters becomes more regular and order
for the negative couple constant. While, for the positive one, the motion of
coupled particles first undergoes a series of transitions between chaotic
motion and regular motion and then falls into horizon or escapes to spatial
infinite. Our results show that the coupling brings about richer effects for
the motion of the particles.
| [
{
"created": "Tue, 31 May 2016 07:04:59 GMT",
"version": "v1"
},
{
"created": "Tue, 28 Mar 2017 15:16:39 GMT",
"version": "v2"
},
{
"created": "Sat, 8 Apr 2017 16:16:21 GMT",
"version": "v3"
}
] | 2017-04-11 | [
[
"Wang",
"Mingzhi",
""
],
[
"Chen",
"Songbai",
""
],
[
"Jing",
"Jiliang",
""
]
] | We present firstly the equation of motion for a test scalar particle coupling to Einstein tensor in the Schwarzschild-Melvin black hole spacetime through the short-wave approximation. Through analysing Poincar\'{e} sections, the power spectrum, the fast Lyapunov exponent indicator and the bifurcation diagram, we investigate the effects of coupling parameter on the chaotic behavior of the particles. With the increase of the coupling strength, we find that the motion of coupled particle for the chosen parameters becomes more regular and order for the negative couple constant. While, for the positive one, the motion of coupled particles first undergoes a series of transitions between chaotic motion and regular motion and then falls into horizon or escapes to spatial infinite. Our results show that the coupling brings about richer effects for the motion of the particles. |
1603.09683 | Chandrachur Chakraborty | Chandrachur Chakraborty, Parthapratim Pradhan | Behavior of a test gyroscope moving towards a rotating traversable
wormhole | LaTex, 18 pages including 7 figures, extensively revised version, one
new section added, accepted for publication in JCAP | JCAP03(2017)035 | 10.1088/1475-7516/2017/03/035 | null | gr-qc astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The geodesic structure of the Teo wormhole is briefly discussed and some
observables are derived that promise to be of use in detecting a rotating
traversable wormhole indirectly, if it does exist. We also deduce the exact
Lense-Thirring (LT) precession frequency of a test gyroscope moving toward a
rotating traversable Teo wormhole. The precession frequency diverges on the
ergoregion, a behavior intimately related to and governed by the geometry of
the ergoregion, analogous to the situation in a Kerr spacetime. Interestingly,
it turns out that here the LT precession is inversely proportional to the
angular momentum ($a$) of the wormhole along the pole and around it in the
strong gravity regime, a behavior contrasting with its direct variation with
$a$ in the case of other compact objects. In fact, divergence of LT precession
inside the ergoregion can also be avoided if the gyro moves with a non-zero
angular velocity in a certain range. As a result, the spin precession frequency
of the gyro can be made finite throughout its whole path, even very close to
the throat, during its travel to the wormhole. Furthermore, it is evident from
our formulation that this spin precession not only arises due to curvature or
rotation of the spacetime but also due to the non-zero angular velocity of the
spin when it does not move along a geodesic in the strong gravity regime. If in
the future, interstellar travel indeed becomes possible through a wormhole or
at least in its vicinity, our results would prove useful in determining the
behavior of a test gyroscope which is known to serve as a fundamental
navigation device.
| [
{
"created": "Thu, 31 Mar 2016 17:08:32 GMT",
"version": "v1"
},
{
"created": "Mon, 27 Feb 2017 05:14:27 GMT",
"version": "v2"
}
] | 2017-03-17 | [
[
"Chakraborty",
"Chandrachur",
""
],
[
"Pradhan",
"Parthapratim",
""
]
] | The geodesic structure of the Teo wormhole is briefly discussed and some observables are derived that promise to be of use in detecting a rotating traversable wormhole indirectly, if it does exist. We also deduce the exact Lense-Thirring (LT) precession frequency of a test gyroscope moving toward a rotating traversable Teo wormhole. The precession frequency diverges on the ergoregion, a behavior intimately related to and governed by the geometry of the ergoregion, analogous to the situation in a Kerr spacetime. Interestingly, it turns out that here the LT precession is inversely proportional to the angular momentum ($a$) of the wormhole along the pole and around it in the strong gravity regime, a behavior contrasting with its direct variation with $a$ in the case of other compact objects. In fact, divergence of LT precession inside the ergoregion can also be avoided if the gyro moves with a non-zero angular velocity in a certain range. As a result, the spin precession frequency of the gyro can be made finite throughout its whole path, even very close to the throat, during its travel to the wormhole. Furthermore, it is evident from our formulation that this spin precession not only arises due to curvature or rotation of the spacetime but also due to the non-zero angular velocity of the spin when it does not move along a geodesic in the strong gravity regime. If in the future, interstellar travel indeed becomes possible through a wormhole or at least in its vicinity, our results would prove useful in determining the behavior of a test gyroscope which is known to serve as a fundamental navigation device. |
gr-qc/0601080 | Maria J. Pareja | M. J. Pareja and J. Frauendiener | Constant scalar curvature hypersurfaces in extended Schwarzschild
space-time | 15 pages, 7 figures, uses amsart | Phys.Rev. D74 (2006) 044026 | 10.1103/PhysRevD.74.044026 | null | gr-qc | null | We present a class of spherically symmetric hypersurfaces in the
Kruskal extension of the Schwarzschild space-time. The hypersurfaces have
constant negative scalar curvature, so they are hyperboloidal in the regions of
space-time which are asymptotically flat.
| [
{
"created": "Thu, 19 Jan 2006 20:56:35 GMT",
"version": "v1"
},
{
"created": "Fri, 7 Apr 2006 16:43:22 GMT",
"version": "v2"
}
] | 2016-08-31 | [
[
"Pareja",
"M. J.",
""
],
[
"Frauendiener",
"J.",
""
]
] | We present a class of spherically symmetric hypersurfaces in the Kruskal extension of the Schwarzschild space-time. The hypersurfaces have constant negative scalar curvature, so they are hyperboloidal in the regions of space-time which are asymptotically flat. |
gr-qc/0407065 | Vladimir Trishin | Vladimir V. Kassandrov, Vladimir N. Trishin | Gauge fields and particle-like formations associated with shear-free
null congruences | 4 pages, to appear in Proceedings of the Tenth Marcel Grossmann
Meeting on General Relativity, 2003 | null | 10.1142/9789812704030_0239 | null | gr-qc | null | We consider Maxwell fields associated with any shear-free null geodesic
congruence on Minkowski or Riemannian background space-time. Bounded singular
loci of these fields are treated as particle-like formations, possess
"self-quantized" electric charge and undergo self-consistent time dynamics.
Complicated singular solutions of Maxwell (as well as related complex
Yang-Mills) equations can be obtained in a purely algebraic way using the Kerr
theorem.
| [
{
"created": "Fri, 16 Jul 2004 16:50:42 GMT",
"version": "v1"
}
] | 2016-11-09 | [
[
"Kassandrov",
"Vladimir V.",
""
],
[
"Trishin",
"Vladimir N.",
""
]
] | We consider Maxwell fields associated with any shear-free null geodesic congruence on Minkowski or Riemannian background space-time. Bounded singular loci of these fields are treated as particle-like formations, possess "self-quantized" electric charge and undergo self-consistent time dynamics. Complicated singular solutions of Maxwell (as well as related complex Yang-Mills) equations can be obtained in a purely algebraic way using the Kerr theorem. |
2006.13757 | Peng Zhao | David Hilditch, Juan A. Valiente Kroon, Peng Zhao | Improved existence for the characteristic initial value problem with the
conformal Einstein field equations | 44 pages, 3 figures. arXiv admin note: text overlap with
arXiv:1911.00047 | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We adapt Luk's analysis of the characteristic initial value problem in
General Relativity to the asymptotic characteristic problem for the conformal
Einstein field equations to demonstrate the local existence of solutions in a
neighbourhood of the set on which the data are given. In particular, we obtain
existence of solutions along a narrow rectangle along null infinity which, in
turn, corresponds to an infinite domain in the asymptotic region of the
physical spacetime. This result generalises work by K\'ann\'ar on the local
existence of solutions to the characteristic initial value problem by means of
Rendall's reduction strategy. In analysing the conformal Einstein equations we
make use of the Newman-Penrose formalism and a gauge due to J. Stewart.
| [
{
"created": "Tue, 23 Jun 2020 14:37:08 GMT",
"version": "v1"
}
] | 2020-06-25 | [
[
"Hilditch",
"David",
""
],
[
"Kroon",
"Juan A. Valiente",
""
],
[
"Zhao",
"Peng",
""
]
] | We adapt Luk's analysis of the characteristic initial value problem in General Relativity to the asymptotic characteristic problem for the conformal Einstein field equations to demonstrate the local existence of solutions in a neighbourhood of the set on which the data are given. In particular, we obtain existence of solutions along a narrow rectangle along null infinity which, in turn, corresponds to an infinite domain in the asymptotic region of the physical spacetime. This result generalises work by K\'ann\'ar on the local existence of solutions to the characteristic initial value problem by means of Rendall's reduction strategy. In analysing the conformal Einstein equations we make use of the Newman-Penrose formalism and a gauge due to J. Stewart. |
gr-qc/0701149 | Deborah A. Konkowski | T. M. Helliwell and D. A. Konkowski | Quantum healing of classical singularities in power-law spacetimes | 14 pages, 1 figure; extensive revisions | Class.Quant.Grav.24:3377-3390,2007 | 10.1088/0264-9381/24/13/014 | null | gr-qc | null | We study a broad class of spacetimes whose metric coefficients reduce to
powers of a radius r in the limit of small r. Among these four-parameter
"power-law" metrics we identify those parameters for which the spacetimes have
classical singularities as r approaches 0. We show that a large set of such
classically singular spacetimes is nevertheless nonsingular quantum
mechanically, in that the Hamiltonian operator is essentially self-adjoint, so
that the evolution of quantum wave packets lacks the ambiguity associated with
scattering off singularities. Using these metrics, the broadest class yet
studied to compare classical with quantum singularities, we explore the
physical reasons why some that are singular classically are "healed" quantum
mechanically, while others are not. We show that most (but not all) of the
remaining quantum-mechanically singular spacetimes can be excluded if either
the weak energy condition or the dominant energy condition is invoked, and we
briefly discuss the effect of this work on the strong cosmic censorship
hypothesis.
| [
{
"created": "Sat, 27 Jan 2007 18:35:24 GMT",
"version": "v1"
},
{
"created": "Wed, 9 May 2007 19:29:29 GMT",
"version": "v2"
},
{
"created": "Wed, 9 May 2007 22:29:28 GMT",
"version": "v3"
}
] | 2008-11-26 | [
[
"Helliwell",
"T. M.",
""
],
[
"Konkowski",
"D. A.",
""
]
] | We study a broad class of spacetimes whose metric coefficients reduce to powers of a radius r in the limit of small r. Among these four-parameter "power-law" metrics we identify those parameters for which the spacetimes have classical singularities as r approaches 0. We show that a large set of such classically singular spacetimes is nevertheless nonsingular quantum mechanically, in that the Hamiltonian operator is essentially self-adjoint, so that the evolution of quantum wave packets lacks the ambiguity associated with scattering off singularities. Using these metrics, the broadest class yet studied to compare classical with quantum singularities, we explore the physical reasons why some that are singular classically are "healed" quantum mechanically, while others are not. We show that most (but not all) of the remaining quantum-mechanically singular spacetimes can be excluded if either the weak energy condition or the dominant energy condition is invoked, and we briefly discuss the effect of this work on the strong cosmic censorship hypothesis. |
0904.3976 | Leonardo Fernandez-Jambrina | L. Fern\'andez-Jambrina, L.M. Gonz\'alez-Romero | On non-singular inhomogeneous cosmological models | 6 pp. Proceedings of ERE'04; Published in Beyond General Relativity.
Proceedings of the 2004 Spanish Relativity Meeting (ERE2004). Eds: N.
Alonso-Alberca, E. Alvarez, T. Ortin, (ed.), M.A. Vazquez-Mozo. Universidad
Autonoma de Madrid, Madrid, 2007 | Published in Beyond General Relativity. Proceedings of the 2004
Spanish Relativity Meeting (ERE2004). Eds: N. Alonso-Alberca, E. Alvarez, T.
Ortin, (ed.), M.A. Vazquez-Mozo. Universidad Autonoma de Madrid, Madrid,
129-134, 2007 | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this talk we would like to review recent results on non-singular
cosmological models. It has been recently shown that among stiff perfect fluid
inhomogeneous spacetimes the absence of singularities is more common than it
was expected in the literature. We would like to generalize these results and
apply them to other matter sources.
| [
{
"created": "Sat, 25 Apr 2009 10:55:00 GMT",
"version": "v1"
}
] | 2009-04-29 | [
[
"Fernández-Jambrina",
"L.",
""
],
[
"González-Romero",
"L. M.",
""
]
] | In this talk we would like to review recent results on non-singular cosmological models. It has been recently shown that among stiff perfect fluid inhomogeneous spacetimes the absence of singularities is more common than it was expected in the literature. We would like to generalize these results and apply them to other matter sources. |
0710.5167 | Pablo Laguna | Ian Hinder, Birjoo Vaishnav, Frank Herrmann, Deirdre Shoemaker, Pablo
Laguna | Circularization and Final Spin in Eccentric Binary Black Hole Inspirals | 4 pages, 4 figures, 2 tables. Final version in PRD | Phys.Rev.D77:081502,2008 | 10.1103/PhysRevD.77.081502 | null | gr-qc astro-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present results from numerical relativity simulations of equal mass,
non-spinning binary black hole inspirals and mergers with initial
eccentricities e <= 0.8 and coordinate separations D >= 12 M of up to 9 orbits
(18 gravitational wave cycles). We extract the mass M_f and spin a_f of the
final black hole and find, for eccentricities e < 0.4, that a_f/M_f = 0.69 and
M_f/M_adm = 0.96 are independent of the initial eccentricity, suggesting that
the binary has circularized by the merger time. For e > 0.5, the black holes
plunge rather than orbit, and we obtain a maximum spin parameter a_f/M_f = 0.72
around e = 0.5.
| [
{
"created": "Fri, 26 Oct 2007 19:42:29 GMT",
"version": "v1"
},
{
"created": "Wed, 2 Jul 2008 18:46:39 GMT",
"version": "v2"
}
] | 2008-11-26 | [
[
"Hinder",
"Ian",
""
],
[
"Vaishnav",
"Birjoo",
""
],
[
"Herrmann",
"Frank",
""
],
[
"Shoemaker",
"Deirdre",
""
],
[
"Laguna",
"Pablo",
""
]
] | We present results from numerical relativity simulations of equal mass, non-spinning binary black hole inspirals and mergers with initial eccentricities e <= 0.8 and coordinate separations D >= 12 M of up to 9 orbits (18 gravitational wave cycles). We extract the mass M_f and spin a_f of the final black hole and find, for eccentricities e < 0.4, that a_f/M_f = 0.69 and M_f/M_adm = 0.96 are independent of the initial eccentricity, suggesting that the binary has circularized by the merger time. For e > 0.5, the black holes plunge rather than orbit, and we obtain a maximum spin parameter a_f/M_f = 0.72 around e = 0.5. |
0711.2754 | Carlos Augusto Romero Filho | F. Dahia, G. A. T. Gomez, C. Romero | On the embedding of spacetime in five-dimensional Weyl spaces | 16 pages, new title and references added | null | 10.1063/1.3000049 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We revisit Weyl geometry in the context of recent higher-dimensional theories
of spacetime. After introducing the Weyl theory in a modern geometrical
language we present some results that represent extensions of Riemannian
theorems. We consider the theory of local embeddings and submanifolds in the
context of Weyl geometries and show how a Riemannian spacetime may be locally
and isometrically embedded in a Weyl bulk. We discuss the problem of classical
confinement and the stability of motion of particles and photons in the
neighbourhood of branes for the case when the Weyl bulk has the geometry of a
warped product space. We show how the confinement and stability properties of
geodesics near the brane may be affected by the Weyl field. We construct a
classical analogue of quantum confinement inspired in theoretical-field models
by considering a Weyl scalar field which depends only on the extra coordinate.
| [
{
"created": "Sat, 17 Nov 2007 17:22:39 GMT",
"version": "v1"
},
{
"created": "Tue, 23 Sep 2008 13:30:03 GMT",
"version": "v2"
}
] | 2009-11-13 | [
[
"Dahia",
"F.",
""
],
[
"Gomez",
"G. A. T.",
""
],
[
"Romero",
"C.",
""
]
] | We revisit Weyl geometry in the context of recent higher-dimensional theories of spacetime. After introducing the Weyl theory in a modern geometrical language we present some results that represent extensions of Riemannian theorems. We consider the theory of local embeddings and submanifolds in the context of Weyl geometries and show how a Riemannian spacetime may be locally and isometrically embedded in a Weyl bulk. We discuss the problem of classical confinement and the stability of motion of particles and photons in the neighbourhood of branes for the case when the Weyl bulk has the geometry of a warped product space. We show how the confinement and stability properties of geodesics near the brane may be affected by the Weyl field. We construct a classical analogue of quantum confinement inspired in theoretical-field models by considering a Weyl scalar field which depends only on the extra coordinate. |
1704.05471 | Robert Penna | Robert F. Penna, Scott A. Hughes, Stephen O'Sullivan | Strong-field tidal distortions of rotating black holes: III. Embeddings
in hyperbolic 3-space | 10 pages, 6 figures | null | 10.1103/PhysRevD.96.064030 | null | gr-qc astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In previous work, we developed tools for quantifying the tidal distortion of
a black hole's event horizon due to an orbiting companion. These tools use
techniques which require large mass ratios (companion mass $\mu$ much smaller
than black hole mass $M$), but can be used for arbitrary bound orbits, and for
any black hole spin. We also showed how to visualize these distorted black
holes by embedding their horizons in a global Euclidean 3-space,
${\mathbb{E}}^3$. Such visualizations illustrate interesting and important
information about horizon dynamics. Unfortunately, we could not visualize black
holes with spin parameter $a_* > \sqrt{3}/2 \approx 0.866$: such holes cannot
be globally embedded into ${\mathbb{E}}^3$. In this paper, we overcome this
difficulty by showing how to embed the horizons of tidally distorted Kerr black
holes in a hyperbolic 3-space, ${\mathbb{H}}^3$. We use black hole perturbation
theory to compute the Gaussian curvatures of tidally distorted event horizons,
from which we build a two-dimensional metric of their distorted horizons. We
develop a numerical method for embedding the tidally distorted horizons in
${\mathbb{H}}^3$. As an application, we give a sequence of embeddings into
${\mathbb{H}}^3$ of a tidally interacting black hole with spin $a_*=0.9999$. A
small amplitude, high frequency oscillation seen in previous work shows up
particularly clearly in these embeddings.
| [
{
"created": "Tue, 18 Apr 2017 18:00:18 GMT",
"version": "v1"
},
{
"created": "Thu, 20 Apr 2017 15:10:33 GMT",
"version": "v2"
}
] | 2017-10-11 | [
[
"Penna",
"Robert F.",
""
],
[
"Hughes",
"Scott A.",
""
],
[
"O'Sullivan",
"Stephen",
""
]
] | In previous work, we developed tools for quantifying the tidal distortion of a black hole's event horizon due to an orbiting companion. These tools use techniques which require large mass ratios (companion mass $\mu$ much smaller than black hole mass $M$), but can be used for arbitrary bound orbits, and for any black hole spin. We also showed how to visualize these distorted black holes by embedding their horizons in a global Euclidean 3-space, ${\mathbb{E}}^3$. Such visualizations illustrate interesting and important information about horizon dynamics. Unfortunately, we could not visualize black holes with spin parameter $a_* > \sqrt{3}/2 \approx 0.866$: such holes cannot be globally embedded into ${\mathbb{E}}^3$. In this paper, we overcome this difficulty by showing how to embed the horizons of tidally distorted Kerr black holes in a hyperbolic 3-space, ${\mathbb{H}}^3$. We use black hole perturbation theory to compute the Gaussian curvatures of tidally distorted event horizons, from which we build a two-dimensional metric of their distorted horizons. We develop a numerical method for embedding the tidally distorted horizons in ${\mathbb{H}}^3$. As an application, we give a sequence of embeddings into ${\mathbb{H}}^3$ of a tidally interacting black hole with spin $a_*=0.9999$. A small amplitude, high frequency oscillation seen in previous work shows up particularly clearly in these embeddings. |
2402.07205 | Rong-Jia Yang | Rong-Jia Yang, Yong-Ben Shi | Baryogenesis in quantum fluctuation modified gravity | 11 pages, 6 figures | null | null | null | gr-qc hep-th | http://creativecommons.org/licenses/by-nc-sa/4.0/ | We consider baryogenesis in quantum fluctuation modified gravity. We explore
three forms (two are newly proposed here) of baryogenesis interaction and
discuss the effect of these interaction terms on the baryon-to-entropy ratio
during the radiation era of the expanding universe. We constrain the model
parameters with the current observational data, implying that this modified
gravity is capable to address the issue of baryon asymmetry in a successful
manner.
| [
{
"created": "Sun, 11 Feb 2024 13:34:34 GMT",
"version": "v1"
},
{
"created": "Wed, 17 Apr 2024 12:46:20 GMT",
"version": "v2"
}
] | 2024-04-18 | [
[
"Yang",
"Rong-Jia",
""
],
[
"Shi",
"Yong-Ben",
""
]
] | We consider baryogenesis in quantum fluctuation modified gravity. We explore three forms (two are newly proposed here) of baryogenesis interaction and discuss the effect of these interaction terms on the baryon-to-entropy ratio during the radiation era of the expanding universe. We constrain the model parameters with the current observational data, implying that this modified gravity is capable to address the issue of baryon asymmetry in a successful manner. |
1506.04432 | Jerzy Matyjasek | Jerzy Matyjasek and Pawel Sadurski | Inside the Schwarzschild-Tangherlini black holes | null | Phys. Rev. D 92, 044023 (2015) | 10.1103/PhysRevD.92.044023 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The first-order semiclassical Einstein field equations are solved in the
interior of the Schwarzschild-Tangherlini black holes. The source term is taken
to be the stress-energy tensor of the quantized massive scalar field with
arbitrary curvature coupling calculated within the framework of the
Schwinger-DeWitt approximation. It is shown that for the minimal coupling the
quantum effects tend to isotropize the interior of the black hole (which can be
interpreted as an anisotropic collapsing universe) for D=4 and 5, whereas for
D=6 and 7 the spacetime becomes more anisotropic. Similar behavior is observed
for the conformal coupling with the reservation that for D=5 isotropization of
the spacetime occurs during (approximately) the first 1/3 of the lifetime of
the interior universe. On the other hand, we find that regardless of the
dimension, the quantum perturbations initially strengthen the grow of curvature
and its later behavior depends on the dimension and the coupling. It is shown
that the Karlhede's scalar can still be used as a useful device for locating
the horizon of the quantum-corrected black hole, as expected.
| [
{
"created": "Sun, 14 Jun 2015 19:34:56 GMT",
"version": "v1"
}
] | 2015-08-19 | [
[
"Matyjasek",
"Jerzy",
""
],
[
"Sadurski",
"Pawel",
""
]
] | The first-order semiclassical Einstein field equations are solved in the interior of the Schwarzschild-Tangherlini black holes. The source term is taken to be the stress-energy tensor of the quantized massive scalar field with arbitrary curvature coupling calculated within the framework of the Schwinger-DeWitt approximation. It is shown that for the minimal coupling the quantum effects tend to isotropize the interior of the black hole (which can be interpreted as an anisotropic collapsing universe) for D=4 and 5, whereas for D=6 and 7 the spacetime becomes more anisotropic. Similar behavior is observed for the conformal coupling with the reservation that for D=5 isotropization of the spacetime occurs during (approximately) the first 1/3 of the lifetime of the interior universe. On the other hand, we find that regardless of the dimension, the quantum perturbations initially strengthen the grow of curvature and its later behavior depends on the dimension and the coupling. It is shown that the Karlhede's scalar can still be used as a useful device for locating the horizon of the quantum-corrected black hole, as expected. |
1608.00631 | Carlos A. R. Herdeiro | Jorge F. M. Delgado, Carlos A. R. Herdeiro, Eugen Radu and Helgi
Runarsson | Kerr-Newman black holes with scalar hair | 11 pages, 4 figures; v2. Change in title and other minor changes, to
match published version | Phys.Lett. B761 (2016) 234-241 | 10.1016/j.physletb.2016.08.032 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We construct electrically charged Kerr black holes (BHs) with scalar hair.
Firstly, we take an uncharged scalar field, interacting with the
electromagnetic field only indirectly, via the background metric. The
corresponding family of solutions, dubbed Kerr-Newman BHs with ungauged scalar
hair, reduces to (a sub-family of) Kerr-Newman BHs in the limit of vanishing
scalar hair and to uncharged rotating boson stars in the limit of vanishing
horizon. It adds one extra parameter to the uncharged solutions: the total
electric charge. This leading electromagnetic multipole moment is unaffected by
the scalar hair and can be computed by using Gauss's law on any closed
2-surface surrounding (a spatial section of) the event horizon. By contrast,
the first sub-leading electromagnetic multipole -- the magnetic dipole moment
--, gets suppressed by the scalar hair, such that the gyromagnetic ratio is
always smaller than the Kerr-Newman value ($g=2$). Secondly, we consider a
gauged scalar field and obtain a family of Kerr-Newman BHs with gauged scalar
hair. The electrically charged scalar field now stores a part of the total
electric charge, which can only be computed by applying Gauss' law at spatial
infinity and introduces a new solitonic limit -- electrically charged rotating
boson stars. In both cases, we analyse some physical properties of the
solutions.
| [
{
"created": "Mon, 1 Aug 2016 22:23:28 GMT",
"version": "v1"
},
{
"created": "Tue, 13 Sep 2016 10:00:58 GMT",
"version": "v2"
}
] | 2016-09-14 | [
[
"Delgado",
"Jorge F. M.",
""
],
[
"Herdeiro",
"Carlos A. R.",
""
],
[
"Radu",
"Eugen",
""
],
[
"Runarsson",
"Helgi",
""
]
] | We construct electrically charged Kerr black holes (BHs) with scalar hair. Firstly, we take an uncharged scalar field, interacting with the electromagnetic field only indirectly, via the background metric. The corresponding family of solutions, dubbed Kerr-Newman BHs with ungauged scalar hair, reduces to (a sub-family of) Kerr-Newman BHs in the limit of vanishing scalar hair and to uncharged rotating boson stars in the limit of vanishing horizon. It adds one extra parameter to the uncharged solutions: the total electric charge. This leading electromagnetic multipole moment is unaffected by the scalar hair and can be computed by using Gauss's law on any closed 2-surface surrounding (a spatial section of) the event horizon. By contrast, the first sub-leading electromagnetic multipole -- the magnetic dipole moment --, gets suppressed by the scalar hair, such that the gyromagnetic ratio is always smaller than the Kerr-Newman value ($g=2$). Secondly, we consider a gauged scalar field and obtain a family of Kerr-Newman BHs with gauged scalar hair. The electrically charged scalar field now stores a part of the total electric charge, which can only be computed by applying Gauss' law at spatial infinity and introduces a new solitonic limit -- electrically charged rotating boson stars. In both cases, we analyse some physical properties of the solutions. |
gr-qc/0405073 | Ewa Czuchry | E. Czuchry, J. Jezierski and J. Kijowski | Local approach to thermodynamics of black holes | 10 pages, to appear in Proceedings of the Seventh Hungarian
Relativity Workshop | in Relativity Today (Proc. 7th Hungarian Relativity Workshop,
2003) Ed. I. Racz, (Akad\'emiai Kiad\'o, Budapest, 2004) | null | null | gr-qc | null | Hamiltonian description of gravitational field contained in a spacetime
region with boundary $S$ being a null-like hypersurface (a wave front) is
discussed. Complete generating formula for the Hamiltonian dynamics (with no
surface integrals neglected) is presented. A quasi-local proof of the 1-st law
of black holes thermodynamics is obtained as a consequence, in case when $S$ is
a non-expanding horizon. The 0-th law and Penrose inequalities are discussed
from this point of view.
| [
{
"created": "Fri, 14 May 2004 07:41:15 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Czuchry",
"E.",
""
],
[
"Jezierski",
"J.",
""
],
[
"Kijowski",
"J.",
""
]
] | Hamiltonian description of gravitational field contained in a spacetime region with boundary $S$ being a null-like hypersurface (a wave front) is discussed. Complete generating formula for the Hamiltonian dynamics (with no surface integrals neglected) is presented. A quasi-local proof of the 1-st law of black holes thermodynamics is obtained as a consequence, in case when $S$ is a non-expanding horizon. The 0-th law and Penrose inequalities are discussed from this point of view. |
1010.1933 | Babak Vakili | Babak Vakili and Nima Khosravi | Bianchi type I cyclic cosmology from Lie-algebraically deformed phase
space | 13 pages, to appear in PRD, typos corrected, Refs. added | Phys. Rev. D 82 (2010) 103509 | 10.1103/PhysRevD.82.103509 | null | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the effects of noncommutativity, in the form of a Lie-algebraically
deformed Poisson commutation relations, on the evolution of a Bianchi type I
cosmological model with a positive cosmological constant. The phase space
variables turn out to correspond to the scale factors of this model in $x$, $y$
and $z$ directions. According to the conditions that the structure constants
(deformation parameters) should satisfy, we argue that there are two types of
noncommutative phase space with Lie-algebraic structure. The exact classical
solutions in commutative and type I noncommutative cases are presented. In the
framework of this type of deformed phase space, we investigate the possibility
of building a Bianchi I model with cyclic scale factors in which the size of
the universe in each direction experiences an endless sequence of contractions
and re-expansions. We also obtain some approximate solutions for the type II
noncommutative structure by numerical methods and show that the cyclic behavior
is repeated as well. These results are compared with the standard commutative
case, and similarities and differences of these solutions are discussed.
| [
{
"created": "Sun, 10 Oct 2010 16:05:20 GMT",
"version": "v1"
},
{
"created": "Fri, 5 Nov 2010 18:07:26 GMT",
"version": "v2"
}
] | 2015-05-20 | [
[
"Vakili",
"Babak",
""
],
[
"Khosravi",
"Nima",
""
]
] | We study the effects of noncommutativity, in the form of a Lie-algebraically deformed Poisson commutation relations, on the evolution of a Bianchi type I cosmological model with a positive cosmological constant. The phase space variables turn out to correspond to the scale factors of this model in $x$, $y$ and $z$ directions. According to the conditions that the structure constants (deformation parameters) should satisfy, we argue that there are two types of noncommutative phase space with Lie-algebraic structure. The exact classical solutions in commutative and type I noncommutative cases are presented. In the framework of this type of deformed phase space, we investigate the possibility of building a Bianchi I model with cyclic scale factors in which the size of the universe in each direction experiences an endless sequence of contractions and re-expansions. We also obtain some approximate solutions for the type II noncommutative structure by numerical methods and show that the cyclic behavior is repeated as well. These results are compared with the standard commutative case, and similarities and differences of these solutions are discussed. |
gr-qc/0102102 | Alessandra Buonanno | Alessandra Buonanno and Thibault Damour | The fate of classical tensor inhomogeneities in pre-big-bang string
cosmology | 16 pages, 2 figures | Phys.Rev. D64 (2001) 043501 | 10.1103/PhysRevD.64.043501 | GRP/00/553, IHES/P/01/05 | gr-qc | null | In pre-big-bang string cosmology one uses a phase of dilaton-driven inflation
to stretch an initial (microscopic) spatial patch to the (much larger) size of
the big-bang fireball. We show that the dilaton-driven inflationary phase does
not naturally iron out the initial classical tensor inhomogeneities unless the
initial value of the string coupling is smaller than 10^(-35).
| [
{
"created": "Fri, 23 Feb 2001 23:48:15 GMT",
"version": "v1"
}
] | 2009-11-07 | [
[
"Buonanno",
"Alessandra",
""
],
[
"Damour",
"Thibault",
""
]
] | In pre-big-bang string cosmology one uses a phase of dilaton-driven inflation to stretch an initial (microscopic) spatial patch to the (much larger) size of the big-bang fireball. We show that the dilaton-driven inflationary phase does not naturally iron out the initial classical tensor inhomogeneities unless the initial value of the string coupling is smaller than 10^(-35). |
1906.02866 | Yuta Michimura Dr. | Yuta Michimura, Masaki Ando, Eleonora Capocasa, Yutaro Enomoto,
Raffaele Flaminio, Sadakazu Haino, Kazuhiro Hayama, Eiichi Hirose, Yousuke
Itoh, Tomoya Kinugawa, Kentro Komori, Matteo Leonardi, Norikatsu Mio, Koji
Nagano, Hiroyuki Nakano, Atsushi Nishizawa, Norichika Sago, Masaru Shibata,
Hisaaki Shinkai, Kentaro Somiya, Hiroki Takeda, Takahiro Tanaka, Satoshi
Tanioka, Li-Wei Wei, Kazuhiro Yamamoto | Prospects for improving the sensitivity of KAGRA gravitational wave
detector | 7 pages, 3 figures, Proceedings for the Fifteenth Marcel Grossmann
Meeting, Rome, July 1-7, 2018 | null | 10.1142/9789811258251_0236 | JGW-P1910276 | gr-qc astro-ph.IM physics.ins-det | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | KAGRA is a new gravitational wave detector which aims to begin joint
observation with Advanced LIGO and Advanced Virgo from late 2019. Here, we
present KAGRA's possible upgrade plans to improve the sensitivity in the decade
ahead. Unlike other state-of-the-art detectors, KAGRA requires different
investigations for the upgrade since it is the only detector which employs
cryogenic cooling of the test mass mirrors. In this paper, investigations on
the upgrade plans which can be realized by changing the input laser power,
increasing the mirror mass, and injecting frequency dependent squeezed vacuum
are presented. We show how each upgrade affects to the detector frequency bands
and also discuss impacts on gravitational-wave science. We then propose an
effective progression of upgrades based on technical feasibility and scientific
scenarios.
| [
{
"created": "Fri, 7 Jun 2019 02:22:13 GMT",
"version": "v1"
}
] | 2023-02-22 | [
[
"Michimura",
"Yuta",
""
],
[
"Ando",
"Masaki",
""
],
[
"Capocasa",
"Eleonora",
""
],
[
"Enomoto",
"Yutaro",
""
],
[
"Flaminio",
"Raffaele",
""
],
[
"Haino",
"Sadakazu",
""
],
[
"Hayama",
"Kazuhiro",
""
],
[
"Hirose",
"Eiichi",
""
],
[
"Itoh",
"Yousuke",
""
],
[
"Kinugawa",
"Tomoya",
""
],
[
"Komori",
"Kentro",
""
],
[
"Leonardi",
"Matteo",
""
],
[
"Mio",
"Norikatsu",
""
],
[
"Nagano",
"Koji",
""
],
[
"Nakano",
"Hiroyuki",
""
],
[
"Nishizawa",
"Atsushi",
""
],
[
"Sago",
"Norichika",
""
],
[
"Shibata",
"Masaru",
""
],
[
"Shinkai",
"Hisaaki",
""
],
[
"Somiya",
"Kentaro",
""
],
[
"Takeda",
"Hiroki",
""
],
[
"Tanaka",
"Takahiro",
""
],
[
"Tanioka",
"Satoshi",
""
],
[
"Wei",
"Li-Wei",
""
],
[
"Yamamoto",
"Kazuhiro",
""
]
] | KAGRA is a new gravitational wave detector which aims to begin joint observation with Advanced LIGO and Advanced Virgo from late 2019. Here, we present KAGRA's possible upgrade plans to improve the sensitivity in the decade ahead. Unlike other state-of-the-art detectors, KAGRA requires different investigations for the upgrade since it is the only detector which employs cryogenic cooling of the test mass mirrors. In this paper, investigations on the upgrade plans which can be realized by changing the input laser power, increasing the mirror mass, and injecting frequency dependent squeezed vacuum are presented. We show how each upgrade affects to the detector frequency bands and also discuss impacts on gravitational-wave science. We then propose an effective progression of upgrades based on technical feasibility and scientific scenarios. |
2003.10175 | Naveena Kumara A | A. Naveena Kumara, C.L. Ahmed Rizwan, Kartheek Hegde, Ajith K.M | Repulsive Interactions in the Microstructure of Regular Hayward Black
Hole in Anti-de Sitter Spacetime | 14 pages, 5 figures. Version accepted for publication on Physics
Letters B | Physics Letters B 807 (2020) 135556 | 10.1016/j.physletb.2020.135556 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the interaction between the microstructures of Hayward-AdS black
hole using Ruppeiner geometry. Our investigation shows that the dominant
interaction between the black hole molecules is attractive in most part of the
parametric space of temperature and volume, as in van der Waals system.
However, in contrast to the van der Waals fluid, there exists a weak dominant
repulsive interaction for small black hole phase in some parameter range. This
result clearly distinguishes the interactions in a magnetically charged black
hole from that of van der Waals fluid. However, these sort of interactions are
characteristic for charged black holes since they do not dependent on magnetic
charge or temperature.
| [
{
"created": "Mon, 23 Mar 2020 10:44:56 GMT",
"version": "v1"
},
{
"created": "Sun, 28 Jun 2020 09:44:24 GMT",
"version": "v2"
}
] | 2020-06-30 | [
[
"Kumara",
"A. Naveena",
""
],
[
"Rizwan",
"C. L. Ahmed",
""
],
[
"Hegde",
"Kartheek",
""
],
[
"M",
"Ajith K.",
""
]
] | We study the interaction between the microstructures of Hayward-AdS black hole using Ruppeiner geometry. Our investigation shows that the dominant interaction between the black hole molecules is attractive in most part of the parametric space of temperature and volume, as in van der Waals system. However, in contrast to the van der Waals fluid, there exists a weak dominant repulsive interaction for small black hole phase in some parameter range. This result clearly distinguishes the interactions in a magnetically charged black hole from that of van der Waals fluid. However, these sort of interactions are characteristic for charged black holes since they do not dependent on magnetic charge or temperature. |
1102.0936 | Sumati Surya | Onkar Parrikar and Sumati Surya | Causal Topology in Future and Past Distinguishing Spacetimes | 20 pages, 4 figures. Minor revisions. In particular, (i) terminology
in one of the Lemmas corrected, (ii) numbering of Lemmas, Theorems, etc.
uniformised. To appear in Classical and Quantum Gravity | Class.Quant.Grav.28:155020,2011 | 10.1088/0264-9381/28/15/155020 | null | gr-qc math.DG | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The causal structure of a strongly causal spacetime is particularly well
endowed. Not only does it determine the conformal spacetime geometry when the
spacetime dimension n >2, as shown by Malament and Hawking-King-McCarthy
(MHKM), but also the manifold dimension. The MHKM result, however, applies more
generally to spacetimes satisfying the weaker causality condition of future and
past distinguishability (FPD), and it is an important question whether the
causal structure of such spacetimes can determine the manifold dimension. In
this work we show that the answer to this question is in the affirmative. We
investigate the properties of future or past distinguishing spacetimes and show
that their causal structures determine the manifold dimension. This gives a
non-trivial generalisation of the MHKM theorem and suggests that there is a
causal topology for FPD spacetimes which encodes manifold dimension and which
is strictly finer than the Alexandrov topology. We show that such a causal
topology does exist. We construct it using a convergence criterion based on
sequences of "chain-intervals" which are the causal analogs of null geodesic
segments. We show that when the region of strong causality violation satisfies
a local achronality condition, this topology is equivalent to the manifold
topology in an FPD spacetime.
| [
{
"created": "Fri, 4 Feb 2011 15:11:09 GMT",
"version": "v1"
},
{
"created": "Fri, 17 Jun 2011 13:15:49 GMT",
"version": "v2"
}
] | 2015-03-18 | [
[
"Parrikar",
"Onkar",
""
],
[
"Surya",
"Sumati",
""
]
] | The causal structure of a strongly causal spacetime is particularly well endowed. Not only does it determine the conformal spacetime geometry when the spacetime dimension n >2, as shown by Malament and Hawking-King-McCarthy (MHKM), but also the manifold dimension. The MHKM result, however, applies more generally to spacetimes satisfying the weaker causality condition of future and past distinguishability (FPD), and it is an important question whether the causal structure of such spacetimes can determine the manifold dimension. In this work we show that the answer to this question is in the affirmative. We investigate the properties of future or past distinguishing spacetimes and show that their causal structures determine the manifold dimension. This gives a non-trivial generalisation of the MHKM theorem and suggests that there is a causal topology for FPD spacetimes which encodes manifold dimension and which is strictly finer than the Alexandrov topology. We show that such a causal topology does exist. We construct it using a convergence criterion based on sequences of "chain-intervals" which are the causal analogs of null geodesic segments. We show that when the region of strong causality violation satisfies a local achronality condition, this topology is equivalent to the manifold topology in an FPD spacetime. |
2301.10456 | Kensuke Sueto | Kensuke Sueto, Hirotaka Yoshino | Evaporation of a nonsingular Reissner-Nordstr\"om black hole and
information loss problem | 46 pages, 14 figures | Prog Theor Exp Phys (2023) | 10.1093/ptep/ptad111 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | One of the attractive solutions to the information loss problem is that the
event horizon does not appear in the process of gravitational collapse and
subsequent evaporation once the spacetime singularity is regularized by some
mechanism, as pointed out by Hayward and Frolov. In this paper, we examine
whether this Hayward-Frolov scenario holds for the evaporation of a charged
black hole. The process of collapse and evaporation is modeled with the charged
Vaidya spacetime and two kinds of regularization of the central singularity are
considered. Analyzing the spacetime structure of the evaporating black hole, we
find that the appropriately regularized evaporating Reissner-Nordstr\"{o}m
"black hole" has no event and Cauchy horizons, indicating the possibility that
the Hayward-Frolov scenario may have sufficient generality as the solution to
the information loss problem. In addition, the properties of the non-singular
evaporating Reissner-Nordsto\"{o}m black hole are examined in detail.
| [
{
"created": "Wed, 25 Jan 2023 08:25:05 GMT",
"version": "v1"
},
{
"created": "Fri, 28 Apr 2023 14:44:12 GMT",
"version": "v2"
},
{
"created": "Tue, 13 Feb 2024 09:27:53 GMT",
"version": "v3"
}
] | 2024-02-14 | [
[
"Sueto",
"Kensuke",
""
],
[
"Yoshino",
"Hirotaka",
""
]
] | One of the attractive solutions to the information loss problem is that the event horizon does not appear in the process of gravitational collapse and subsequent evaporation once the spacetime singularity is regularized by some mechanism, as pointed out by Hayward and Frolov. In this paper, we examine whether this Hayward-Frolov scenario holds for the evaporation of a charged black hole. The process of collapse and evaporation is modeled with the charged Vaidya spacetime and two kinds of regularization of the central singularity are considered. Analyzing the spacetime structure of the evaporating black hole, we find that the appropriately regularized evaporating Reissner-Nordstr\"{o}m "black hole" has no event and Cauchy horizons, indicating the possibility that the Hayward-Frolov scenario may have sufficient generality as the solution to the information loss problem. In addition, the properties of the non-singular evaporating Reissner-Nordsto\"{o}m black hole are examined in detail. |
2306.05863 | Luca Guido Molinari | Carlo Alberto Mantica and Luca Guido Molinari | The covariant approach to static spacetimes in Einstein and extended
gravity theories | 25 pages. Some misprints corrected and references added | General Relativity and Gravitation, 2023 - open access | 10.1007/s10714-023-03149-w | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present a covariant study of static space-times, as such and as solutions
of gravity theories. By expressing the relevant tensors through the velocity
and the acceleration vectors that characterise static space-times, the field
equations provide a natural non-redundant set of scalar equations. The same
vectors suggest the form of a Faraday tensor, that is studied in itself and in
(non)-linear electrodynamics. In spherical symmetry, we evaluate the explicit
expressions of the Ricci, the Weyl, the Cotton and the Bach tensors. Simple
restrictions on the coefficients yield well known and new solutions in
Einstein, f(R), Cotton and Conformal gravity, with or without charges, in vacuo
or with fluid source.
| [
{
"created": "Fri, 9 Jun 2023 12:56:08 GMT",
"version": "v1"
},
{
"created": "Fri, 1 Sep 2023 13:36:49 GMT",
"version": "v2"
}
] | 2023-09-14 | [
[
"Mantica",
"Carlo Alberto",
""
],
[
"Molinari",
"Luca Guido",
""
]
] | We present a covariant study of static space-times, as such and as solutions of gravity theories. By expressing the relevant tensors through the velocity and the acceleration vectors that characterise static space-times, the field equations provide a natural non-redundant set of scalar equations. The same vectors suggest the form of a Faraday tensor, that is studied in itself and in (non)-linear electrodynamics. In spherical symmetry, we evaluate the explicit expressions of the Ricci, the Weyl, the Cotton and the Bach tensors. Simple restrictions on the coefficients yield well known and new solutions in Einstein, f(R), Cotton and Conformal gravity, with or without charges, in vacuo or with fluid source. |
1301.5103 | Igor Kalinichenko | I. S. Kalinichenko, P. O. Kazinski | High-temperature expansion of the one-loop free energy of a scalar field
on a curved background | 27 pages;considerable changes made,appendix B changed,equation (52)
changed abstract changed, conclusion added, some references added | Phys. Rev. D.87, 084036 (2013) | 10.1103/PhysRevD.87.084036 | null | gr-qc hep-th | http://creativecommons.org/licenses/publicdomain/ | The complete form of the high-temperature expansion of the one-loop
contribution to the free energy of a scalar field on a stationary gravitational
background is derived. The explicit expressions for the divergent and finite
parts of the high-temperature expansion in a three-dimensional space without
boundaries are obtained. These formulas generalize the known one for the
stationary spacetime. In particular, we confirm that for a massless conformal
scalar field the leading correction to the Planck law proportional to the
temperature squared turns out to be nonzero due to non-static nature of the
metric. The explicit expression for the so-called energy-time anomaly is found.
The interrelation between this anomaly and the conformal (trace) anomaly is
established. The natural simplest Lagrangian for the "Killing vector field" is
given.
| [
{
"created": "Tue, 22 Jan 2013 08:27:50 GMT",
"version": "v1"
},
{
"created": "Wed, 30 Jan 2013 11:06:32 GMT",
"version": "v2"
},
{
"created": "Tue, 12 Feb 2013 18:40:58 GMT",
"version": "v3"
},
{
"created": "Sat, 30 Mar 2013 10:03:34 GMT",
"version": "v4"
}
] | 2013-04-23 | [
[
"Kalinichenko",
"I. S.",
""
],
[
"Kazinski",
"P. O.",
""
]
] | The complete form of the high-temperature expansion of the one-loop contribution to the free energy of a scalar field on a stationary gravitational background is derived. The explicit expressions for the divergent and finite parts of the high-temperature expansion in a three-dimensional space without boundaries are obtained. These formulas generalize the known one for the stationary spacetime. In particular, we confirm that for a massless conformal scalar field the leading correction to the Planck law proportional to the temperature squared turns out to be nonzero due to non-static nature of the metric. The explicit expression for the so-called energy-time anomaly is found. The interrelation between this anomaly and the conformal (trace) anomaly is established. The natural simplest Lagrangian for the "Killing vector field" is given. |
1402.5767 | Yong-Chang Huang | Ming Chen, Yong-Chang Huang | Gas Model of Gravitons with Light Speed | 9 Pages | null | null | BJUT ITP01 | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We first review some aspects of gravitational wave and the thermodynamic
expression of Einstein field equations, these achieved conclusions allow people
to think of Einstein's gravitational wave as a kind of sound wave in ordinary
gas which propagates as an adiabatic compression wave. In the following, using
the properties of photon gas in "white wall box", we find an analogous
relationship between ordinary gas and photon gas through sound velocity
formula. At last, by taking the ordinary gas as an intermediary, we find that
gravitational wave is analogous to photon gas, or equally, gravitons are
analogous to photons although they are different in some ways such as spins and
coupling strengths, and these different properties don't affect their
propagation speeds. Utilizing this analogous relationship, we achieve the gas
model of gravitons and this model naturally gives out the light speed of
gravitons
| [
{
"created": "Mon, 24 Feb 2014 09:53:02 GMT",
"version": "v1"
},
{
"created": "Tue, 17 Jun 2014 16:04:50 GMT",
"version": "v2"
}
] | 2014-06-18 | [
[
"Chen",
"Ming",
""
],
[
"Huang",
"Yong-Chang",
""
]
] | We first review some aspects of gravitational wave and the thermodynamic expression of Einstein field equations, these achieved conclusions allow people to think of Einstein's gravitational wave as a kind of sound wave in ordinary gas which propagates as an adiabatic compression wave. In the following, using the properties of photon gas in "white wall box", we find an analogous relationship between ordinary gas and photon gas through sound velocity formula. At last, by taking the ordinary gas as an intermediary, we find that gravitational wave is analogous to photon gas, or equally, gravitons are analogous to photons although they are different in some ways such as spins and coupling strengths, and these different properties don't affect their propagation speeds. Utilizing this analogous relationship, we achieve the gas model of gravitons and this model naturally gives out the light speed of gravitons |
2208.03004 | Pankaj Saini | Pankaj Saini, Sajad A. Bhat, and K. G. Arun | Premerger localization of intermediate mass binary black holes with LISA
and prospects of joint observations with Athena and LSST | 13 pages, 4 figures; Published in Phys. Rev. D. v2: Fig.1 added,
minor changes to match the published version | Phys. Rev. D 106, 104015 (2022) | 10.1103/PhysRevD.106.104015 | null | gr-qc astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The planned Laser Interferometric Space Antenna (LISA) will be able to detect
gravitational waves (GWs) from intermediate mass binary black holes (IMBBHs) in
the mass range $\sim 10^{2} \mbox{-} 10^{4}\,M_{\odot}$ up to a redshift
$z\sim20$. Modulation effects due to orbital motion of LISA around the Sun
facilitate precise premerger localization of the sources, which in turn would
help in electromagnetic (EM) followups. In this work, we calculate the
uncertainties in sky position, luminosity distance, and time of coalescence as
a function of time to coalescence. For representative masses of the IMBBHs, we
synthesize a population of binaries uniformly located and oriented on a sphere
of radius 3 Gpc and compute the projected parameter measurement uncertainties
using the Fisher information matrix. We find that for systems with a total mass
of $10^3\,M_{\odot}$, the errors in the sky position and luminosity distance
are $\sim 0.4\,\text{deg}^2$ and $\sim 6\%$, respectively, one day prior to
coalescence. The coalescence time can be predicted with an uncertainty
$\lesssim 10$ sec, one day before coalescence. We also find that for
$10^3\,M_{\odot}$, around $40\%$ ($100\%$) of the population has a source
localization that is smaller than the field of view of Athena (LSST) one day
before the merger. These extremely precise measurements can be used to alert
ground-based GW detectors and EM telescopes about the time and location of
these mergers. We also discuss mechanisms that may produce EM emission from
IMBBH mergers and study its detectability using the planned Legacy Survey of
Space and Time (LSST) in the optical and Athena in the x-ray bands. Detection
of an EM transient may provide us vital clues about the environments where
these mergers occur and the distance estimation can pave the way for
cosmography.
| [
{
"created": "Fri, 5 Aug 2022 06:40:01 GMT",
"version": "v1"
},
{
"created": "Fri, 18 Nov 2022 12:18:40 GMT",
"version": "v2"
}
] | 2022-11-21 | [
[
"Saini",
"Pankaj",
""
],
[
"Bhat",
"Sajad A.",
""
],
[
"Arun",
"K. G.",
""
]
] | The planned Laser Interferometric Space Antenna (LISA) will be able to detect gravitational waves (GWs) from intermediate mass binary black holes (IMBBHs) in the mass range $\sim 10^{2} \mbox{-} 10^{4}\,M_{\odot}$ up to a redshift $z\sim20$. Modulation effects due to orbital motion of LISA around the Sun facilitate precise premerger localization of the sources, which in turn would help in electromagnetic (EM) followups. In this work, we calculate the uncertainties in sky position, luminosity distance, and time of coalescence as a function of time to coalescence. For representative masses of the IMBBHs, we synthesize a population of binaries uniformly located and oriented on a sphere of radius 3 Gpc and compute the projected parameter measurement uncertainties using the Fisher information matrix. We find that for systems with a total mass of $10^3\,M_{\odot}$, the errors in the sky position and luminosity distance are $\sim 0.4\,\text{deg}^2$ and $\sim 6\%$, respectively, one day prior to coalescence. The coalescence time can be predicted with an uncertainty $\lesssim 10$ sec, one day before coalescence. We also find that for $10^3\,M_{\odot}$, around $40\%$ ($100\%$) of the population has a source localization that is smaller than the field of view of Athena (LSST) one day before the merger. These extremely precise measurements can be used to alert ground-based GW detectors and EM telescopes about the time and location of these mergers. We also discuss mechanisms that may produce EM emission from IMBBH mergers and study its detectability using the planned Legacy Survey of Space and Time (LSST) in the optical and Athena in the x-ray bands. Detection of an EM transient may provide us vital clues about the environments where these mergers occur and the distance estimation can pave the way for cosmography. |
2205.02077 | Iver Brevik | I. Brevik and A. V. Timoshkin | Holographic description of the dissipative model of universe with
curvature | 6 pages, no figures, to appear in JETP. A reference added | JETP 135 No. 3, 320-323 (2022) | 10.1134/S1063776122090023 | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | We investigate the accelerated expansion of the late-time universe in the
Friedmann-Robertson-Walker metric with nonzero curvature, applying a
holographic principle based on a generalized holographic dark energy model
introduced by Nojiri and Odintsov (2005,2006). We describe the evolution of the
universe using a generalized equation of state in the presence of a viscous
fluid. Solutions of the gravitational equation of motions are obtained in
explicit form for a constant value of the thermodynamic parameter, and for
various forms of the bulk viscosity. We calculate analytic expressions for
infrared cut-offs in terms of the particle horizon, and derive the energy
conservation law in the holographic picture. We show that the inclusion of
nonzero curvature in the Friedmann equation leads to the appearance of
additional singularities of type Big Rip in the Universe.
| [
{
"created": "Wed, 4 May 2022 14:14:26 GMT",
"version": "v1"
},
{
"created": "Sat, 21 May 2022 14:03:17 GMT",
"version": "v2"
}
] | 2022-10-25 | [
[
"Brevik",
"I.",
""
],
[
"Timoshkin",
"A. V.",
""
]
] | We investigate the accelerated expansion of the late-time universe in the Friedmann-Robertson-Walker metric with nonzero curvature, applying a holographic principle based on a generalized holographic dark energy model introduced by Nojiri and Odintsov (2005,2006). We describe the evolution of the universe using a generalized equation of state in the presence of a viscous fluid. Solutions of the gravitational equation of motions are obtained in explicit form for a constant value of the thermodynamic parameter, and for various forms of the bulk viscosity. We calculate analytic expressions for infrared cut-offs in terms of the particle horizon, and derive the energy conservation law in the holographic picture. We show that the inclusion of nonzero curvature in the Friedmann equation leads to the appearance of additional singularities of type Big Rip in the Universe. |
0912.2146 | Lu\'is Filipe de Pinho Oliveira e Costa | L. Filipe O. Costa, Carlos A. R. Herdeiro | Reference Frames and the Physical Gravito-Electromagnetic Analogy | 9 Pages, 1 figure. To appear in the Proceedings of the IAU Symposium
261 "Relativity in Fundamental Astronomy: Dynamics, Reference Frames, and
Data Analysis", Virginia Beach, USA, 27 April - 1 May 2009 | Proceedings of the International Astronomical Union, Volume 5,
Symposium S261, April 2009, pp 31-39. Published by Cambridge University
Press. | 10.1017/S1743921309990111 | null | gr-qc astro-ph.HE hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The similarities between linearized gravity and electromagnetism are known
since the early days of General Relativity. Using an exact approach based on
tidal tensors, we show that such analogy holds only on very special conditions
and depends crucially on the reference frame. This places restrictions on the
validity of the "gravito-electromagnetic" equations commonly found in the
literature.
| [
{
"created": "Fri, 11 Dec 2009 18:07:12 GMT",
"version": "v1"
}
] | 2010-01-07 | [
[
"Costa",
"L. Filipe O.",
""
],
[
"Herdeiro",
"Carlos A. R.",
""
]
] | The similarities between linearized gravity and electromagnetism are known since the early days of General Relativity. Using an exact approach based on tidal tensors, we show that such analogy holds only on very special conditions and depends crucially on the reference frame. This places restrictions on the validity of the "gravito-electromagnetic" equations commonly found in the literature. |
1812.06193 | Daniele Oriti | John W. Barrett, Daniele Oriti, Ruth M. Williams | Tullio Regge's legacy: Regge calculus and discrete gravity | 15 pages; a contribution to the forthcoming volume "Tullio Regge: an
eclectic genius, from quantum gravity to computer play", Eds. L Castellani,
A. Ceresole, R. D'Auria and P. Fr\`e (World Scientific); v2: added references
to more relevant work, minor changes to the text | null | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The review paper "Discrete Structures in Physics", written in 2000, describes
how Regge's discretization of Einstein's theory has been applied in classical
relativity and quantum gravity. Here, developments since 2000 are reviewed
briefly, with particular emphasis on progress in quantum gravity through spin
foam models and group field theories.
| [
{
"created": "Fri, 14 Dec 2018 22:20:58 GMT",
"version": "v1"
},
{
"created": "Wed, 29 May 2019 21:21:35 GMT",
"version": "v2"
}
] | 2019-05-31 | [
[
"Barrett",
"John W.",
""
],
[
"Oriti",
"Daniele",
""
],
[
"Williams",
"Ruth M.",
""
]
] | The review paper "Discrete Structures in Physics", written in 2000, describes how Regge's discretization of Einstein's theory has been applied in classical relativity and quantum gravity. Here, developments since 2000 are reviewed briefly, with particular emphasis on progress in quantum gravity through spin foam models and group field theories. |
1709.09178 | Aron Jansen | Aron Jansen | Overdamped modes in Schwarzschild-de Sitter and a Mathematica package
for the numerical computation of quasinormal modes | Typos fixed, citations added | null | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present a package for Mathematica that facilitates the numerical
computation of the quasinormal mode (QNM) spectrum of a black hole/black brane.
Requiring as input only the QNM equation(s), the application of a single
Mathematica function will compute the spectrum efficiently, by discretizing the
equation(s) and solving the resulting generalized eigenvalue equation. It is
applicable to a large variety of black holes, independent of their asymptotics.
The package comes fully documented and with several tutorials. Here we present
a self-contained review of the method and consider several applications. We
illustrate the method in the simplest case of scalar QNMs of a Schwarzschild
black brane in anti-de Sitter. Then we go on to look at the scalar QNMs of the
Schwarzschild black hole in de Sitter, in anti-de Sitter and in asymptotically
flat spacetimes, finding a novel infinite set of purely imaginary modes in the
first case. We also derive the QNM equations for a generic
Einstein-Maxwell-scalar background and use these to compute the QNMs of the
asymptotically anti-de Sitter Reissner-Nordstr\"{o}m black brane, as a further
illustration and check of the method.
| [
{
"created": "Tue, 26 Sep 2017 18:00:04 GMT",
"version": "v1"
},
{
"created": "Fri, 17 Nov 2017 10:03:11 GMT",
"version": "v2"
}
] | 2017-11-20 | [
[
"Jansen",
"Aron",
""
]
] | We present a package for Mathematica that facilitates the numerical computation of the quasinormal mode (QNM) spectrum of a black hole/black brane. Requiring as input only the QNM equation(s), the application of a single Mathematica function will compute the spectrum efficiently, by discretizing the equation(s) and solving the resulting generalized eigenvalue equation. It is applicable to a large variety of black holes, independent of their asymptotics. The package comes fully documented and with several tutorials. Here we present a self-contained review of the method and consider several applications. We illustrate the method in the simplest case of scalar QNMs of a Schwarzschild black brane in anti-de Sitter. Then we go on to look at the scalar QNMs of the Schwarzschild black hole in de Sitter, in anti-de Sitter and in asymptotically flat spacetimes, finding a novel infinite set of purely imaginary modes in the first case. We also derive the QNM equations for a generic Einstein-Maxwell-scalar background and use these to compute the QNMs of the asymptotically anti-de Sitter Reissner-Nordstr\"{o}m black brane, as a further illustration and check of the method. |
2012.13465 | Juan Carlos Del \'Aguila Rodr\'iguez | Juan Carlos Del \'Aguila and Tonatiuh Matos | Geodesics near a curvature singularity of stationary and axially
symmetric space-times | 16 pages, 2 figues. To be published in Classical and Quantum Gravity | Class. Quantum Grav. 38 055008 (2021) | 10.1088/1361-6382/abd595 | Cinvestav 127/2021 | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work we study the local behavior of geodesics in the neighborhood of
a curvature singularity contained in stationary and axially symmetric
space-times. Apart from these properties, the metrics we shall focus on will
also be required to admit a quadratic first integral for their geodesics. In
particular, we search for the conditions on the geometry of the space-time for
which null and time-like geodesics can reach the singularity. These conditions
are determined by the equations of motion of a freely-falling particle. We also
analyze the possible existence of geodesics that do not become incomplete when
encountering the singularity in their path. The results are stated as criteria
that depend on the inverse metric tensor along with conserved quantities such
as energy and angular momentum. As an example, the derived criteria are applied
to the Plebanski-Demianski class of space-times. Lastly, we propose a line
element that describes a wormhole whose curvature singularities are, according
to our results, inaccessible to causal geodesics.
| [
{
"created": "Thu, 24 Dec 2020 23:49:05 GMT",
"version": "v1"
}
] | 2022-11-08 | [
[
"Del Águila",
"Juan Carlos",
""
],
[
"Matos",
"Tonatiuh",
""
]
] | In this work we study the local behavior of geodesics in the neighborhood of a curvature singularity contained in stationary and axially symmetric space-times. Apart from these properties, the metrics we shall focus on will also be required to admit a quadratic first integral for their geodesics. In particular, we search for the conditions on the geometry of the space-time for which null and time-like geodesics can reach the singularity. These conditions are determined by the equations of motion of a freely-falling particle. We also analyze the possible existence of geodesics that do not become incomplete when encountering the singularity in their path. The results are stated as criteria that depend on the inverse metric tensor along with conserved quantities such as energy and angular momentum. As an example, the derived criteria are applied to the Plebanski-Demianski class of space-times. Lastly, we propose a line element that describes a wormhole whose curvature singularities are, according to our results, inaccessible to causal geodesics. |
2204.13220 | Valeri Frolov P | Valeri P. Frolov | Black holes in the limiting curvature theory of gravity | 11 pages, 1 figure | null | 10.1142/S0217751X22430096 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We discuss a recently proposed limiting curvature theory of gravity and its
application to the problem of singularities inside black holes. In this theory
the growth of the curvature is suppressed by specially chosen inequality
constraints included in the gravity action. We consider a case of a spherically
symmetric four dimensional black hole and demonstrated that imposed curvature
constraints modify a solution in the black hole interior. Instead of forming
the curvature singularity the modified metric describes a space which is
exponentially expanding in one direction and oscillating the other two
directions. The spacetime is complete and its polynomial curvature invariants
are uniformly bounded.
| [
{
"created": "Wed, 27 Apr 2022 22:42:34 GMT",
"version": "v1"
}
] | 2022-10-26 | [
[
"Frolov",
"Valeri P.",
""
]
] | We discuss a recently proposed limiting curvature theory of gravity and its application to the problem of singularities inside black holes. In this theory the growth of the curvature is suppressed by specially chosen inequality constraints included in the gravity action. We consider a case of a spherically symmetric four dimensional black hole and demonstrated that imposed curvature constraints modify a solution in the black hole interior. Instead of forming the curvature singularity the modified metric describes a space which is exponentially expanding in one direction and oscillating the other two directions. The spacetime is complete and its polynomial curvature invariants are uniformly bounded. |
1105.3710 | Norbert Bodendorfer | Norbert Bodendorfer, Thomas Thiemann, Andreas Thurn | Towards Loop Quantum Supergravity (LQSG) II. p-Form Sector | 12 pages. v2: Journal version. Minor clarifications and corrections | Class. Quantum Grav. 30 (2013) 045007 | 10.1088/0264-9381/30/4/045007 | null | gr-qc hep-th math-ph math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In our companion paper, we focussed on the quantisation of the
Rarita-Schwinger sector of Supergravity theories in various dimensions by using
an extension of Loop Quantum Gravity to all spacetime dimensions. In this
paper, we extend this analysis by considering the quantisation of additional
bosonic fields necessary to obtain a complete SUSY multiplet next to graviton
and gravitino in various dimensions. As a generic example, we study concretely
the quantisation of the 3-index photon of 11d SUGRA, but our methods easily
extend to more general p-form fields. Due to the presence of a Chern-Simons
term for the 3-index photon, which is due to local SUSY, the theory is
self-interacting and its quantisation far from straightforward. Nevertheless,
we show that a reduced phase space quantisation with respect to the 3-index
photon Gauss constraint is possible. Specifically, the Weyl algebra of
observables, which deviates from the usual CCR Weyl algebras by an interesting
twist contribution proportional to the level of the Chern-Simons theory, admits
a background independent state of the Narnhofer-Thirring type.
| [
{
"created": "Wed, 18 May 2011 18:25:14 GMT",
"version": "v1"
},
{
"created": "Tue, 12 Feb 2013 19:17:57 GMT",
"version": "v2"
}
] | 2013-02-13 | [
[
"Bodendorfer",
"Norbert",
""
],
[
"Thiemann",
"Thomas",
""
],
[
"Thurn",
"Andreas",
""
]
] | In our companion paper, we focussed on the quantisation of the Rarita-Schwinger sector of Supergravity theories in various dimensions by using an extension of Loop Quantum Gravity to all spacetime dimensions. In this paper, we extend this analysis by considering the quantisation of additional bosonic fields necessary to obtain a complete SUSY multiplet next to graviton and gravitino in various dimensions. As a generic example, we study concretely the quantisation of the 3-index photon of 11d SUGRA, but our methods easily extend to more general p-form fields. Due to the presence of a Chern-Simons term for the 3-index photon, which is due to local SUSY, the theory is self-interacting and its quantisation far from straightforward. Nevertheless, we show that a reduced phase space quantisation with respect to the 3-index photon Gauss constraint is possible. Specifically, the Weyl algebra of observables, which deviates from the usual CCR Weyl algebras by an interesting twist contribution proportional to the level of the Chern-Simons theory, admits a background independent state of the Narnhofer-Thirring type. |
gr-qc/9908053 | Alvaro L. | H. N. N\'u\~nez-Y\'epez | The initial fate of an anisotropic JBD universe | null | Phys.Lett. A258 (1999) 210-216 | 10.1016/S0375-9601(99)00357-6 | null | gr-qc | null | The dynamical effects on the scale factors due to the scalar $\phi$-field at
the early stages of a supposedly anisotropic Universe expansion in the
scalar-tensor cosmology of Jordan-Brans and Dicke is studied. This universe
shows an {\sl isotropic} evolution and, depending on the value of the theorie's
coupling parameter $\omega$, it can begin from a singularity if $\omega>0$ and
after expanding shrink to another one; or, if $\omega <0$ and $-3/2< \omega\leq
-4/3$, it can evolve from a flat spatially-infinite state to a non extended
singularity; or, if $ -4/3 < \omega < 0$, evolve from an extended singularity
to a non singular state and, at last, proceed towards a singularity.
| [
{
"created": "Thu, 19 Aug 1999 17:59:50 GMT",
"version": "v1"
}
] | 2009-10-31 | [
[
"Núñez-Yépez",
"H. N.",
""
]
] | The dynamical effects on the scale factors due to the scalar $\phi$-field at the early stages of a supposedly anisotropic Universe expansion in the scalar-tensor cosmology of Jordan-Brans and Dicke is studied. This universe shows an {\sl isotropic} evolution and, depending on the value of the theorie's coupling parameter $\omega$, it can begin from a singularity if $\omega>0$ and after expanding shrink to another one; or, if $\omega <0$ and $-3/2< \omega\leq -4/3$, it can evolve from a flat spatially-infinite state to a non extended singularity; or, if $ -4/3 < \omega < 0$, evolve from an extended singularity to a non singular state and, at last, proceed towards a singularity. |
gr-qc/0208041 | Yuan-Zhong Zhang | C.G. Shao, Y.Z. Zhang, J. Luo and Z.Z. Liu | Effect of Earth's rotation on the trajectories of free-fall bodies in
Equivalence Principle Experiment | 6 pages, 4 figures | null | 10.1088/0253-6102/39/3/297 | null | gr-qc | null | Owing to Earth's rotation a free-fall body would move in an elliptical orbit
rather than along a straight line forward to the center of the Earth. In this
paper on the basis of the theory for spin-spin coupling between macroscopic
rotating bodies we study violation of the equivalence principle from
long-distance free-fall experiments by means of a rotating ball and a
non-rotating sell. For the free-fall time of 40 seconds, the difference between
the orbits of the two free-fall bodies is of the order of 10^{-9}cm which could
be detected by a SQUID magnetometer owing to such a magnetometer can be used to
measure displacements as small as 10^{-13} centimeters.
| [
{
"created": "Fri, 16 Aug 2002 09:14:59 GMT",
"version": "v1"
}
] | 2018-01-17 | [
[
"Shao",
"C. G.",
""
],
[
"Zhang",
"Y. Z.",
""
],
[
"Luo",
"J.",
""
],
[
"Liu",
"Z. Z.",
""
]
] | Owing to Earth's rotation a free-fall body would move in an elliptical orbit rather than along a straight line forward to the center of the Earth. In this paper on the basis of the theory for spin-spin coupling between macroscopic rotating bodies we study violation of the equivalence principle from long-distance free-fall experiments by means of a rotating ball and a non-rotating sell. For the free-fall time of 40 seconds, the difference between the orbits of the two free-fall bodies is of the order of 10^{-9}cm which could be detected by a SQUID magnetometer owing to such a magnetometer can be used to measure displacements as small as 10^{-13} centimeters. |
gr-qc/0612085 | Chris Van Den Broeck | Chris Van Den Broeck, Anand S. Sengupta | Compact binary inspiral and the science potential of third-generation
ground-based gravitational wave detectors | 3 pages, 4 figures. Brief summary of a talk given at the 11th Marcel
Grossmann meeting, Berlin, July 2006; to appear in the Proceedings | null | null | null | gr-qc astro-ph | null | We consider EGO as a possible third-generation ground-based gravitational
wave detector and evaluate its capabilities for the detection and
interpretation of compact binary inspiral signals. We identify areas of
astrophysics and cosmology where EGO would have qualitative advantages, using
Advanced LIGO as a benchmark for comparison.
| [
{
"created": "Wed, 13 Dec 2006 18:12:49 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Broeck",
"Chris Van Den",
""
],
[
"Sengupta",
"Anand S.",
""
]
] | We consider EGO as a possible third-generation ground-based gravitational wave detector and evaluate its capabilities for the detection and interpretation of compact binary inspiral signals. We identify areas of astrophysics and cosmology where EGO would have qualitative advantages, using Advanced LIGO as a benchmark for comparison. |
gr-qc/0110043 | Carl H. Brans | Torsten Asselmeyer-Maluga and Carl H. Brans | Cosmological anomalies and exotic smoothness structures | null | Gen.Rel.Grav. 34 (2002) 1767-1771 | null | null | gr-qc | null | It seems to be generally accepted that apparently anomalous cosmological
observations, such as accelerating expansion, etc., necessarily are
inconsistent with standard general relativity and standard matter sources.
Following the suggestions of S{\l}adkowski, we point out that in addition to
exotic theories and exotic matter there is another possibility. We refer to
exotic differential structures on ${\mathbb R}^4$ which could be the source of
the observed anomalies without changing the Einstein equations or introducing
strange forms of matter.
| [
{
"created": "Mon, 8 Oct 2001 21:43:33 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Asselmeyer-Maluga",
"Torsten",
""
],
[
"Brans",
"Carl H.",
""
]
] | It seems to be generally accepted that apparently anomalous cosmological observations, such as accelerating expansion, etc., necessarily are inconsistent with standard general relativity and standard matter sources. Following the suggestions of S{\l}adkowski, we point out that in addition to exotic theories and exotic matter there is another possibility. We refer to exotic differential structures on ${\mathbb R}^4$ which could be the source of the observed anomalies without changing the Einstein equations or introducing strange forms of matter. |
1301.4726 | Guoying Chee | G. Y. Chee | Acceleration of the cosmic expansion induced by symmetry breaking | 6 papes, 2 figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | It is proved that in order to obtain a model of the accelerated cosmic
expansion the thing one only need to do is to add a perturbation term to the
Einstein-Hilbert Lagrangian. This term leads to some symmetry breaking terms in
the fields equation, which makes the cosmic expansion accelerating. A vacuum de
Sitter solution is obtained. A new explanation of the acceleration of the
cosmic expansion is presented. In this model the changing of the expansion from
decelerating to accelerating is an intrinsic property of the universe without
need of an exotic dark energy. The acceleration of the cosmic expansion is
induced by the symmetry breaking perturbation of the gravitational energy. The
cosmological constant problem, the coincidence problem and the problem of
phantom divide line crossing are naturally solved. The results of the model are
roughly consistent with the observations.
| [
{
"created": "Mon, 21 Jan 2013 02:00:52 GMT",
"version": "v1"
}
] | 2013-01-22 | [
[
"Chee",
"G. Y.",
""
]
] | It is proved that in order to obtain a model of the accelerated cosmic expansion the thing one only need to do is to add a perturbation term to the Einstein-Hilbert Lagrangian. This term leads to some symmetry breaking terms in the fields equation, which makes the cosmic expansion accelerating. A vacuum de Sitter solution is obtained. A new explanation of the acceleration of the cosmic expansion is presented. In this model the changing of the expansion from decelerating to accelerating is an intrinsic property of the universe without need of an exotic dark energy. The acceleration of the cosmic expansion is induced by the symmetry breaking perturbation of the gravitational energy. The cosmological constant problem, the coincidence problem and the problem of phantom divide line crossing are naturally solved. The results of the model are roughly consistent with the observations. |
2211.15555 | Stefano Ansoldi | Stefano Ansoldi and Takahiro Tanaka | Pathology in WKB wave function for tunneling assisted by gravity | 20 pages, 7 figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | There are several exotic tunneling processes that can be realized only by
incorporating the effect of gravity. Here, we point out that we encounter
difficulties in constructing the WKB wave function, once we try to describe
quantum fluctuations around the semi-classical tunneling path. We present
examples of pathology in the true vacuum decay/upward tunneling, the false
vacuum decay catalyzed by a black hole and the tunneling with black
hole/wormhole production.
| [
{
"created": "Mon, 28 Nov 2022 16:58:19 GMT",
"version": "v1"
}
] | 2022-11-29 | [
[
"Ansoldi",
"Stefano",
""
],
[
"Tanaka",
"Takahiro",
""
]
] | There are several exotic tunneling processes that can be realized only by incorporating the effect of gravity. Here, we point out that we encounter difficulties in constructing the WKB wave function, once we try to describe quantum fluctuations around the semi-classical tunneling path. We present examples of pathology in the true vacuum decay/upward tunneling, the false vacuum decay catalyzed by a black hole and the tunneling with black hole/wormhole production. |
gr-qc/9901038 | Sang Pyo Kim | Sang Pyo Kim, Sung Ku Kim, Kwang-Sup Soh, Jae Hyung Yee | Renormalization of Black Hole Entropy | Proceedings of the 5th Korean-Italian Symposium on Relativistic
Astrophysics, Seoul Korea, 1997; 10 pages, RevTex | J.KoreanPhys.Soc.33:S524-S531,1998 | null | null | gr-qc | null | We review the renormalization of one-loop effective action for gravity
coupled to a scalar field and that of the Bekenstein-Hawking entropy of a black
hole plus the statistical entropy of the scalar field. It is found that the
total entropy of the black hole's geometric entropy and the statistical entropy
yields the renormalized Bekenstein-Hawking area-law of black hole entropy only
for even dimensional Reissner-N\"{o}rdstrom (Schwarzschild) black holes. We
discuss the problem of the microscopic origin of black hole entropy in
connection with the renormalization of black hole entropy.
| [
{
"created": "Thu, 14 Jan 1999 04:53:39 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Kim",
"Sang Pyo",
""
],
[
"Kim",
"Sung Ku",
""
],
[
"Soh",
"Kwang-Sup",
""
],
[
"Yee",
"Jae Hyung",
""
]
] | We review the renormalization of one-loop effective action for gravity coupled to a scalar field and that of the Bekenstein-Hawking entropy of a black hole plus the statistical entropy of the scalar field. It is found that the total entropy of the black hole's geometric entropy and the statistical entropy yields the renormalized Bekenstein-Hawking area-law of black hole entropy only for even dimensional Reissner-N\"{o}rdstrom (Schwarzschild) black holes. We discuss the problem of the microscopic origin of black hole entropy in connection with the renormalization of black hole entropy. |
1506.08076 | Muhammad Azam | M. Azam, S. A. Mardan and M. A. Rehman | Fate of Electromagnetic Field on the Cracking of PSR J1614-2230 in
Quadratic Regime | 21 pages, 8 figures, version to appear in advances in high energy
physics | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, we study the cracking of compact object PSR J1614-2230 in
quadratic regime with electromagnetic field. For this purpose, we develop a
general formalism to determine the cracking of charged compact objects. We
apply the local density perturbations to the hydrostatic equilibrium equation
as well as all the physical variables involve in the model. We plot the force
distribution function against radius of the star with different values of model
parameters both with and without charge. It is found that PSR J1614-2230
remains stable (no cracking) corresponding to different values of parameters
when charge is zero, while it exhibit cracking (unstable) when charge is
introduced. We conclude that stability region increases as amount of charge
increases.
| [
{
"created": "Thu, 25 Jun 2015 11:53:00 GMT",
"version": "v1"
},
{
"created": "Fri, 16 Oct 2015 06:35:27 GMT",
"version": "v2"
}
] | 2015-10-19 | [
[
"Azam",
"M.",
""
],
[
"Mardan",
"S. A.",
""
],
[
"Rehman",
"M. A.",
""
]
] | In this paper, we study the cracking of compact object PSR J1614-2230 in quadratic regime with electromagnetic field. For this purpose, we develop a general formalism to determine the cracking of charged compact objects. We apply the local density perturbations to the hydrostatic equilibrium equation as well as all the physical variables involve in the model. We plot the force distribution function against radius of the star with different values of model parameters both with and without charge. It is found that PSR J1614-2230 remains stable (no cracking) corresponding to different values of parameters when charge is zero, while it exhibit cracking (unstable) when charge is introduced. We conclude that stability region increases as amount of charge increases. |
gr-qc/0410140 | Leonardo Gualtieri | O. Benhar, V. Ferrari, L. Gualtieri | Gravitational waves from neutron stars described by modern EOS | 3 pages, 1+1 figures, to appear in the Proceedings of "XVI SIGRAV
Conference", Vietri sul Mare (Italy), 13-16 September 2004 | null | 10.1063/1.1891555 | null | gr-qc | null | The frequencies and damping times of neutron star (and quark star)
oscillations have been computed using the most recent equations of state
available in the literature. We find that some of the empirical relations that
connect the frequencies and damping times of the modes to the mass and radius
of the star, and that were previously derived in the literature need to be
modified.
| [
{
"created": "Thu, 28 Oct 2004 14:34:12 GMT",
"version": "v1"
}
] | 2009-11-10 | [
[
"Benhar",
"O.",
""
],
[
"Ferrari",
"V.",
""
],
[
"Gualtieri",
"L.",
""
]
] | The frequencies and damping times of neutron star (and quark star) oscillations have been computed using the most recent equations of state available in the literature. We find that some of the empirical relations that connect the frequencies and damping times of the modes to the mass and radius of the star, and that were previously derived in the literature need to be modified. |
2207.03841 | Valerio Faraoni | Valerio Faraoni, Pierre-Antoine Graham, Alexandre Leblanc | Critical solutions of nonminimally coupled scalar field theory and
first-order thermodynamics of gravity | 11 pages, LaTeX | null | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Analytical solutions of nonminimally coupled scalar field cosmology
corresponding to critical scalar field values constitute a potential challenge
to the recent first-order thermodynamics of scalar-tensor gravity (a formalism
picturing general relativity as the zero-temperature equilibrium state for
modified gravity). The critical solutions are unstable with respect to
homogeneous perturbations, hence unphysical.
| [
{
"created": "Fri, 8 Jul 2022 11:51:01 GMT",
"version": "v1"
}
] | 2022-07-11 | [
[
"Faraoni",
"Valerio",
""
],
[
"Graham",
"Pierre-Antoine",
""
],
[
"Leblanc",
"Alexandre",
""
]
] | Analytical solutions of nonminimally coupled scalar field cosmology corresponding to critical scalar field values constitute a potential challenge to the recent first-order thermodynamics of scalar-tensor gravity (a formalism picturing general relativity as the zero-temperature equilibrium state for modified gravity). The critical solutions are unstable with respect to homogeneous perturbations, hence unphysical. |
1810.10418 | Angelos Lykkas | I. Antoniadis, A. Karam, A. Lykkas, K. Tamvakis | Palatini inflation in models with an $R^2$ term | 22 pages, 8 figures, JCAP accepted version | null | 10.1088/1475-7516/2018/11/028 | null | gr-qc astro-ph.CO hep-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Starobinsky model, considered in the framework of the Palatini formalism,
in contrast to the metric formulation, does not provide us with a model for
inflation, due to the absence of a propagating scalar degree of freedom that
can play the role of the inflaton. In the present article we study the Palatini
formulation of the Starobinsky model coupled, in general nonminimally, to
scalar fields and analyze its inflationary behavior. We consider scalars,
minimally or nonminimally coupled to the Starobinsky model, such as a quadratic
model, the induced gravity model or the standard Higgs-like inflation model and
analyze the corresponding modifications favorable to inflation. In addition we
examine the case of a classically scale-invariant model driven by the
Coleman-Weinberg mechanism. In the slow-roll approximation, we analyze the
inflationary predictions of these models and compare them to the latest
constraints from the Planck collaboration. In all cases, we find that the
effect of the $R^2$ term is to lower the value of the tensor-to-scalar ratio.
| [
{
"created": "Wed, 24 Oct 2018 14:26:59 GMT",
"version": "v1"
},
{
"created": "Tue, 20 Nov 2018 14:23:19 GMT",
"version": "v2"
}
] | 2018-11-28 | [
[
"Antoniadis",
"I.",
""
],
[
"Karam",
"A.",
""
],
[
"Lykkas",
"A.",
""
],
[
"Tamvakis",
"K.",
""
]
] | The Starobinsky model, considered in the framework of the Palatini formalism, in contrast to the metric formulation, does not provide us with a model for inflation, due to the absence of a propagating scalar degree of freedom that can play the role of the inflaton. In the present article we study the Palatini formulation of the Starobinsky model coupled, in general nonminimally, to scalar fields and analyze its inflationary behavior. We consider scalars, minimally or nonminimally coupled to the Starobinsky model, such as a quadratic model, the induced gravity model or the standard Higgs-like inflation model and analyze the corresponding modifications favorable to inflation. In addition we examine the case of a classically scale-invariant model driven by the Coleman-Weinberg mechanism. In the slow-roll approximation, we analyze the inflationary predictions of these models and compare them to the latest constraints from the Planck collaboration. In all cases, we find that the effect of the $R^2$ term is to lower the value of the tensor-to-scalar ratio. |
gr-qc/9909068 | N. K. Dadhich | L.K. Patel and Naresh Dadhich | Exact solutions for null fluid collapse in higher dimensions | 10 pages, LaTEX version | null | null | IUCAA-37/99 | gr-qc | null | A large family of inhomogeneous non-static spherically symmetric solutions of
the Einstein equation for null fluid in higher dimensions has been obtained. It
encompasses higher dimensional versions of many previously known solutions such
as Vaidya, charged Vaidya and Husain solutions and also some new solutions
representing global monopole or string dust. It turns out that physical
properties of the solutions carry over to higher dimensions.
| [
{
"created": "Tue, 21 Sep 1999 12:17:23 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Patel",
"L. K.",
""
],
[
"Dadhich",
"Naresh",
""
]
] | A large family of inhomogeneous non-static spherically symmetric solutions of the Einstein equation for null fluid in higher dimensions has been obtained. It encompasses higher dimensional versions of many previously known solutions such as Vaidya, charged Vaidya and Husain solutions and also some new solutions representing global monopole or string dust. It turns out that physical properties of the solutions carry over to higher dimensions. |
1910.01880 | Keitaro Tomikawa | Keitaro Tomikawa, Tsutomu Kobayashi | On the gauge dependence of gravitational waves generated at second order
from scalar perturbations | 12 pages, 3 figures | Phys. Rev. D 101, 083529 (2020) | 10.1103/PhysRevD.101.083529 | RUP-19-27 | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We revisit and clarify the gauge dependence of gravitational waves generated
at second order from scalar perturbations. In a universe dominated by a perfect
fluid with a constant equation-of-state parameter $w$, we compute the energy
density of such induced gravitational waves in the Newtonian, comoving, and
uniform curvature gauges. Huge differences are found between the Newtonian and
comoving gauge results for any $w \,(\ge 0)$. This is always caused by the
perturbation of the shift vector. Interestingly, the Newtonian and uniform
curvature gauge calculations give the same energy density for $w>0$. In the
case of $w=0$, the uniform curvature gauge result differs only by a factor from
that of the comoving gauge, but deviates significantly from that of the
Newtonian gauge. Our calculation is done analytically for $w=0$ and $w=1/3$,
and our result is consistent with the previous numerical one.
| [
{
"created": "Fri, 4 Oct 2019 11:43:52 GMT",
"version": "v1"
},
{
"created": "Wed, 30 Oct 2019 09:27:43 GMT",
"version": "v2"
}
] | 2020-04-29 | [
[
"Tomikawa",
"Keitaro",
""
],
[
"Kobayashi",
"Tsutomu",
""
]
] | We revisit and clarify the gauge dependence of gravitational waves generated at second order from scalar perturbations. In a universe dominated by a perfect fluid with a constant equation-of-state parameter $w$, we compute the energy density of such induced gravitational waves in the Newtonian, comoving, and uniform curvature gauges. Huge differences are found between the Newtonian and comoving gauge results for any $w \,(\ge 0)$. This is always caused by the perturbation of the shift vector. Interestingly, the Newtonian and uniform curvature gauge calculations give the same energy density for $w>0$. In the case of $w=0$, the uniform curvature gauge result differs only by a factor from that of the comoving gauge, but deviates significantly from that of the Newtonian gauge. Our calculation is done analytically for $w=0$ and $w=1/3$, and our result is consistent with the previous numerical one. |
gr-qc/0301122 | Shahar Hod | Shahar Hod | Kerr black hole quasinormal frequencies | 3 pages, 2 figures | Phys.Rev. D67 (2003) 081501 | 10.1103/PhysRevD.67.081501 | null | gr-qc astro-ph hep-th quant-ph | null | Black-hole quasinormal modes (QNM) have been the subject of much recent
attention, with the hope that these oscillation frequencies may shed some light
on the elusive theory of quantum gravity. We compare numerical results for the
QNM spectrum of the (rotating) Kerr black hole with an {\it exact} formula
Re$\omega \to T_{BH}\ln 3+\Omega m$, which is based on Bohr's correspondence
principle. We find a close agreement between the two. Possible implications of
this result to the area spectrum of quantum black holes are discussed.
| [
{
"created": "Thu, 30 Jan 2003 11:40:03 GMT",
"version": "v1"
},
{
"created": "Wed, 5 Feb 2003 09:27:27 GMT",
"version": "v2"
}
] | 2009-11-10 | [
[
"Hod",
"Shahar",
""
]
] | Black-hole quasinormal modes (QNM) have been the subject of much recent attention, with the hope that these oscillation frequencies may shed some light on the elusive theory of quantum gravity. We compare numerical results for the QNM spectrum of the (rotating) Kerr black hole with an {\it exact} formula Re$\omega \to T_{BH}\ln 3+\Omega m$, which is based on Bohr's correspondence principle. We find a close agreement between the two. Possible implications of this result to the area spectrum of quantum black holes are discussed. |
1804.07346 | Eric Gourgoulhon | Eric Gourgoulhon and Marco Mancini | Symbolic tensor calculus on manifolds: a SageMath implementation | Lectures at JNCF 2018, CIRM, Marseille (France); 58 pages; to appear
in "Les Cours du CIRM" (cedram.org); changes with respect to v1: cedram
format, some updates, LaTeX rendering of Jupyter cells | Les cours du CIRM 6, I (2018) | 10.5802/ccirm.26 | null | gr-qc hep-th math-ph math.MP | http://creativecommons.org/licenses/by/4.0/ | These lecture notes present a method for symbolic tensor calculus that (i)
runs on fully specified smooth manifolds (described by an atlas), (ii) is not
limited to a single coordinate chart or vector frame, (iii) runs even on
non-parallelizable manifolds and (iv) is independent of the symbolic backend
used to perform calculus at the level of coordinate expressions. In addition to
the main ideas, we discuss some details of the implementation in the
open-source mathematics software system SageMath, which has been performed via
the SageManifolds project.
| [
{
"created": "Thu, 19 Apr 2018 19:33:53 GMT",
"version": "v1"
},
{
"created": "Mon, 12 Nov 2018 20:36:19 GMT",
"version": "v2"
}
] | 2019-03-14 | [
[
"Gourgoulhon",
"Eric",
""
],
[
"Mancini",
"Marco",
""
]
] | These lecture notes present a method for symbolic tensor calculus that (i) runs on fully specified smooth manifolds (described by an atlas), (ii) is not limited to a single coordinate chart or vector frame, (iii) runs even on non-parallelizable manifolds and (iv) is independent of the symbolic backend used to perform calculus at the level of coordinate expressions. In addition to the main ideas, we discuss some details of the implementation in the open-source mathematics software system SageMath, which has been performed via the SageManifolds project. |
2111.03467 | Jose Alejandro Rosabal Rodriguez | J. A. Rosabal | Quantum Gravity on a Manifold with boundaries: Schr\"{o}dinger Evolution
and Constraints | Published in EPJC | null | 10.1140/epjc/s10052-022-10543-2 | null | gr-qc hep-th | http://creativecommons.org/licenses/by/4.0/ | In this work, we derive the boundary Schr\"{o}dinger (functional) equation
for the wave function of a quantum gravity system on a manifold with boundaries
together with a new constraint equation defined on the timelike boundary. From
a detailed analysis of the gravity boundary condition on the spatial boundary,
we find that while the lapse and the shift functions are independent Lagrange
multipliers on the bulk, on the spatial boundary, these two are related;
namely, they are not independent. In the Hamiltonian ADM formalism, a new
Lagrange multiplier, solving the boundary conditions involving the lapse and
the shift functions evaluated on the spatial boundary, is introduced. The
classical equation of motion associated with this Lagrange multiplier turns out
to be an identity when evaluated on a classical solution of Einstein's
equations. On the other hand, its quantum counterpart is a constraint equation
involving the gravitational degrees of freedom defined only on the boundary.
This constraint has not been taken into account before when studying the
quantum gravity Schr\"{o}dinger evolution on manifolds with boundaries.
| [
{
"created": "Fri, 5 Nov 2021 12:43:44 GMT",
"version": "v1"
},
{
"created": "Wed, 6 Jul 2022 09:57:43 GMT",
"version": "v2"
}
] | 2022-07-07 | [
[
"Rosabal",
"J. A.",
""
]
] | In this work, we derive the boundary Schr\"{o}dinger (functional) equation for the wave function of a quantum gravity system on a manifold with boundaries together with a new constraint equation defined on the timelike boundary. From a detailed analysis of the gravity boundary condition on the spatial boundary, we find that while the lapse and the shift functions are independent Lagrange multipliers on the bulk, on the spatial boundary, these two are related; namely, they are not independent. In the Hamiltonian ADM formalism, a new Lagrange multiplier, solving the boundary conditions involving the lapse and the shift functions evaluated on the spatial boundary, is introduced. The classical equation of motion associated with this Lagrange multiplier turns out to be an identity when evaluated on a classical solution of Einstein's equations. On the other hand, its quantum counterpart is a constraint equation involving the gravitational degrees of freedom defined only on the boundary. This constraint has not been taken into account before when studying the quantum gravity Schr\"{o}dinger evolution on manifolds with boundaries. |
gr-qc/0602025 | Gaurav Khanna | Daniel Cartin, Gaurav Khanna | Wave functions for the Schwarschild black hole interior | 15 pages, 4 figures, published version | Phys.Rev. D73 (2006) 104009 | 10.1103/PhysRevD.73.104009 | null | gr-qc hep-th | null | Using the Hamiltonian constraint derived by Ashtekar and Bojowald, we look
for pre-classical wave functions in the Schwarzschild interior. In particular,
when solving this difference equation by separation of variables, an inequality
is obtained relating the Immirzi parameter $\gamma$ to the quantum ambiguity
$\delta$ appearing in the model. This bound is violated when we use a natural
value for $\delta$ based on loop quantum gravity together with a recent
proposal for $\gamma$. We also present numerical solutions of the constraint.
| [
{
"created": "Tue, 7 Feb 2006 19:58:42 GMT",
"version": "v1"
},
{
"created": "Sat, 8 Apr 2006 16:08:25 GMT",
"version": "v2"
}
] | 2009-11-11 | [
[
"Cartin",
"Daniel",
""
],
[
"Khanna",
"Gaurav",
""
]
] | Using the Hamiltonian constraint derived by Ashtekar and Bojowald, we look for pre-classical wave functions in the Schwarzschild interior. In particular, when solving this difference equation by separation of variables, an inequality is obtained relating the Immirzi parameter $\gamma$ to the quantum ambiguity $\delta$ appearing in the model. This bound is violated when we use a natural value for $\delta$ based on loop quantum gravity together with a recent proposal for $\gamma$. We also present numerical solutions of the constraint. |
2003.05491 | Pedro Fernandes | Pedro G. S. Fernandes | Charged Black Holes in AdS Spaces in $4D$ Einstein Gauss-Bonnet Gravity | 6 pages, 1 figure. v3: accepted in Physics Letters B | Physics Letters B 805, 135468 (2020) | 10.1016/j.physletb.2020.135468 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Recently a non-trivial 4-dimensional theory of gravity that claims to
circumvent Lovelock's theorem and avoid Ostrogradsky instability was formulated
in [D. Glavan and C. Lin, Phys. Rev. Lett. 124, 081301 (2020)]. This theory,
named "$4D$ Einstein Gauss-Bonnet gravity", presents several novel predictions
for cosmology and black hole physics. In this paper, we generalize the vacuum
black hole solution of Glavan \& Lin to include electric charge in an anti-de
Sitter space and explore some properties of this solution such as the
asymptotics, properties of the horizons, the general relativity limit and
thermodynamics.
| [
{
"created": "Wed, 11 Mar 2020 19:10:31 GMT",
"version": "v1"
},
{
"created": "Fri, 13 Mar 2020 16:22:27 GMT",
"version": "v2"
},
{
"created": "Wed, 6 May 2020 15:41:23 GMT",
"version": "v3"
}
] | 2020-05-14 | [
[
"Fernandes",
"Pedro G. S.",
""
]
] | Recently a non-trivial 4-dimensional theory of gravity that claims to circumvent Lovelock's theorem and avoid Ostrogradsky instability was formulated in [D. Glavan and C. Lin, Phys. Rev. Lett. 124, 081301 (2020)]. This theory, named "$4D$ Einstein Gauss-Bonnet gravity", presents several novel predictions for cosmology and black hole physics. In this paper, we generalize the vacuum black hole solution of Glavan \& Lin to include electric charge in an anti-de Sitter space and explore some properties of this solution such as the asymptotics, properties of the horizons, the general relativity limit and thermodynamics. |
gr-qc/9612009 | B. S. Sathyaprakash | B.S. Sathyaprakash (IUCAA, UWCC) | Signal analysis of gravitational waves | 12 pages (including 1 figure); latex (needs cupconf.sty bundled
together with source); to appear in "Relativistic Gravitation and
Gravitational Radiation", eds. Jean-Alain Marck and Jean-Pierre Lasota (CUP) | null | null | null | gr-qc | null | In this lecture we describe the data analysis problem for insparlling
binaries. We discuss the detection statistic, how to make realiable estimation
and how to compute bias in the estimation of parameters. A combination of
geometrical ideas and numerical methods are employed to estimate computational
costs involved in searching for post-Newtonian wave forms.
| [
{
"created": "Tue, 3 Dec 1996 15:20:11 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Sathyaprakash",
"B. S.",
"",
"IUCAA, UWCC"
]
] | In this lecture we describe the data analysis problem for insparlling binaries. We discuss the detection statistic, how to make realiable estimation and how to compute bias in the estimation of parameters. A combination of geometrical ideas and numerical methods are employed to estimate computational costs involved in searching for post-Newtonian wave forms. |
0803.0915 | Piotr Jaranowski | Thibault Damour, Piotr Jaranowski, and Gerhard Sch\"afer | Effective one body approach to the dynamics of two spinning black holes
with next-to-leading order spin-orbit coupling | REVTeX, 22 pages, 7 figures | Phys.Rev.D78:024009,2008 | 10.1103/PhysRevD.78.024009 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Using a recent, novel Hamiltonian formulation of the gravitational
interaction of spinning binaries, we extend the Effective One Body (EOB)
description of the dynamics of two spinning black holes to next-to-leading
order (NLO) in the spin-orbit interaction. The spin-dependent EOB Hamiltonian
is constructed from four main ingredients: (i) a transformation between the
``effective'' Hamiltonian and the ``real'' one, (ii) a generalized effective
Hamilton-Jacobi equation involving higher powers of the momenta, (iii) a
Kerr-type effective metric (with Pad\'e-resummed coefficients) which depends on
the choice of some basic ``effective spin vector'' $\bf{S}_{\rm eff}$, and
which is deformed by comparable-mass effects, and (iv) an additional effective
spin-orbit interaction term involving another spin vector $\bsigma$. As a first
application of the new, NLO spin-dependent EOB Hamiltonian, we compute the
binding energy of circular orbits (for parallel spins) as a function of the
orbital frequency, and of the spin parameters. We also study the
characteristics of the last stable circular orbit: binding energy, orbital
frequency, and the corresponding dimensionless spin parameter $\hat{a}_{\rm
LSO}\equiv c J_{\rm LSO}/\boldsymbol(G(H_{\rm LSO}/c^2)^2\boldsymbol)$. We find
that the inclusion of NLO spin-orbit terms has a significant ``moderating''
effect on the dynamical characteristics of the circular orbits for large and
parallel spins.
| [
{
"created": "Thu, 6 Mar 2008 17:20:27 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Damour",
"Thibault",
""
],
[
"Jaranowski",
"Piotr",
""
],
[
"Schäfer",
"Gerhard",
""
]
] | Using a recent, novel Hamiltonian formulation of the gravitational interaction of spinning binaries, we extend the Effective One Body (EOB) description of the dynamics of two spinning black holes to next-to-leading order (NLO) in the spin-orbit interaction. The spin-dependent EOB Hamiltonian is constructed from four main ingredients: (i) a transformation between the ``effective'' Hamiltonian and the ``real'' one, (ii) a generalized effective Hamilton-Jacobi equation involving higher powers of the momenta, (iii) a Kerr-type effective metric (with Pad\'e-resummed coefficients) which depends on the choice of some basic ``effective spin vector'' $\bf{S}_{\rm eff}$, and which is deformed by comparable-mass effects, and (iv) an additional effective spin-orbit interaction term involving another spin vector $\bsigma$. As a first application of the new, NLO spin-dependent EOB Hamiltonian, we compute the binding energy of circular orbits (for parallel spins) as a function of the orbital frequency, and of the spin parameters. We also study the characteristics of the last stable circular orbit: binding energy, orbital frequency, and the corresponding dimensionless spin parameter $\hat{a}_{\rm LSO}\equiv c J_{\rm LSO}/\boldsymbol(G(H_{\rm LSO}/c^2)^2\boldsymbol)$. We find that the inclusion of NLO spin-orbit terms has a significant ``moderating'' effect on the dynamical characteristics of the circular orbits for large and parallel spins. |
1701.01028 | Rafael Augusto Couceiro Correa | P. H. R. S. Moraes, R. A. C. Correa, R. V. Lobato | Analytical general solutions for static wormholes in $f(R,T)$ gravity | null | null | 10.1088/1475-7516/2017/07/029 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Originally proposed as a tool for teaching the general theory of relativity,
wormholes are today approached in many different ways and are seeing as an
efficient alternative for interstellar and time travel. Attempts to achieve
observational signatures of wormholes have been growing as the subject has
became more and more popular. In this article we investigate some $f(R,T)$
theoretical predictions for static wormholes, i.e., wormholes whose throat
radius can be considered a constant. Since the $T$-dependence in $f(R,T)$
gravity is due to the consideration of quantum effects, a further investigation
of wormholes in such a theory is well motivated. We obtain the energy
conditions of static wormholes in $f(R,T)$ gravity and apply an analytical
approach to find the solutions. We highlight that our results are in agreement
with previous solutions presented in the literature.
| [
{
"created": "Mon, 26 Dec 2016 14:35:50 GMT",
"version": "v1"
}
] | 2017-07-26 | [
[
"Moraes",
"P. H. R. S.",
""
],
[
"Correa",
"R. A. C.",
""
],
[
"Lobato",
"R. V.",
""
]
] | Originally proposed as a tool for teaching the general theory of relativity, wormholes are today approached in many different ways and are seeing as an efficient alternative for interstellar and time travel. Attempts to achieve observational signatures of wormholes have been growing as the subject has became more and more popular. In this article we investigate some $f(R,T)$ theoretical predictions for static wormholes, i.e., wormholes whose throat radius can be considered a constant. Since the $T$-dependence in $f(R,T)$ gravity is due to the consideration of quantum effects, a further investigation of wormholes in such a theory is well motivated. We obtain the energy conditions of static wormholes in $f(R,T)$ gravity and apply an analytical approach to find the solutions. We highlight that our results are in agreement with previous solutions presented in the literature. |
gr-qc/9701044 | Louis Marchildon | Louis Marchildon (Universite du Quebec) | Lie Symmetries of Einstein's Vacuum Equations in N Dimensions | 14 pages, LaTeX, no figures | J. Nonlin. Math. Phys. 5 (1998) 68-81 | 10.2991/jnmp.1998.5.1.7 | null | gr-qc | null | We investigate Lie symmetries of Einstein's vacuum equations in N dimensions,
with a cosmological term. For this purpose, we first write down the second
prolongation of the symmetry generating vector fields, and compute its action
on Einstein's equations. Instead of setting to zero the coefficients of all
independent partial derivatives (which involves a very complicated substitution
of Einstein's equations), we set to zero the coefficients of derivatives that
do not appear in Einstein's equations. This considerably constrains the
coefficients of symmetry generating vector fields. Using the Lie algebra
property of generators of symmetries and the fact that general coordinate
transformations are symmetries of Einstein's equations, we are then able to
obtain all the Lie symmetries. The method we have used can likely be applied to
other types of equations.
| [
{
"created": "Mon, 20 Jan 1997 16:47:15 GMT",
"version": "v1"
}
] | 2015-05-26 | [
[
"Marchildon",
"Louis",
"",
"Universite du Quebec"
]
] | We investigate Lie symmetries of Einstein's vacuum equations in N dimensions, with a cosmological term. For this purpose, we first write down the second prolongation of the symmetry generating vector fields, and compute its action on Einstein's equations. Instead of setting to zero the coefficients of all independent partial derivatives (which involves a very complicated substitution of Einstein's equations), we set to zero the coefficients of derivatives that do not appear in Einstein's equations. This considerably constrains the coefficients of symmetry generating vector fields. Using the Lie algebra property of generators of symmetries and the fact that general coordinate transformations are symmetries of Einstein's equations, we are then able to obtain all the Lie symmetries. The method we have used can likely be applied to other types of equations. |
2009.11179 | Peter K.F. Kuhfittig | Peter K.F. Kuhfittig | A note on the stability of Morris-Thorne wormholes | 6 pages, no figures | Fundamental J. Mod. Phys., vol. 14, pp. 23-31, 2020 | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Two critical issues in the study of Morris-Thorne wormholes concerns the
stability of such structures, as well as their compatibility with quantum field
theory. This note discusses an important subset characterized by zero tidal
forces. It is shown that such wormholes (1) are in stable equilibrium using a
criterion based on the Tolman-Oppenheimer-Volkoff (TOV) equation and (2) are
not in direct conflict with quantum field theory.
| [
{
"created": "Wed, 23 Sep 2020 14:42:48 GMT",
"version": "v1"
}
] | 2020-09-24 | [
[
"Kuhfittig",
"Peter K. F.",
""
]
] | Two critical issues in the study of Morris-Thorne wormholes concerns the stability of such structures, as well as their compatibility with quantum field theory. This note discusses an important subset characterized by zero tidal forces. It is shown that such wormholes (1) are in stable equilibrium using a criterion based on the Tolman-Oppenheimer-Volkoff (TOV) equation and (2) are not in direct conflict with quantum field theory. |
gr-qc/9606079 | Thibault Damour | Thibault Damour | Gravitation, experiment and cosmology | 37 pages, Latex, uses hep93.sty, based on lectures given at Les
Houches 1992, SUSY-95 and Corfu 1995, to appear in the Proceedings of the 5th
Hellenic School of Elementary Particle Physics | null | null | IHES/P/95/104 | gr-qc | null | The confrontation between general relativity (and its theoretically most
plausible deviations) and experimental or observational results is summarized.
Some discussion is devoted to the various methodologies used in confronting
theory and experiment. Both weak-field (solar system) and strong-field (binary
pulsar) tests are discussed in detail. A special discussion is devoted to the
cosmology of moduli fields, i.e. scalar fields having only
gravitational-strength couplings to matter.
| [
{
"created": "Thu, 27 Jun 1996 19:32:08 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Damour",
"Thibault",
""
]
] | The confrontation between general relativity (and its theoretically most plausible deviations) and experimental or observational results is summarized. Some discussion is devoted to the various methodologies used in confronting theory and experiment. Both weak-field (solar system) and strong-field (binary pulsar) tests are discussed in detail. A special discussion is devoted to the cosmology of moduli fields, i.e. scalar fields having only gravitational-strength couplings to matter. |
gr-qc/0312009 | Sami Mohammad | M. Sami and Alexey Toporensky | Phantom Field and the Fate of Universe | RevTeX4, 5 pages and 3 eps figures; references updated | Mod.Phys.Lett.A19:1509,2004 | 10.1142/S0217732304013921 | null | gr-qc astro-ph hep-ph hep-th | null | In this paper we analyze the cosmological dynamics of phantom field in a
variety of potentials unbounded from above. We demonstrate that the nature of
future evolution generically depends upon the steepness of the phantom
potential and discuss the fate of Universe accordingly.
| [
{
"created": "Mon, 1 Dec 2003 18:10:27 GMT",
"version": "v1"
},
{
"created": "Fri, 5 Dec 2003 13:19:43 GMT",
"version": "v2"
}
] | 2008-11-26 | [
[
"Sami",
"M.",
""
],
[
"Toporensky",
"Alexey",
""
]
] | In this paper we analyze the cosmological dynamics of phantom field in a variety of potentials unbounded from above. We demonstrate that the nature of future evolution generically depends upon the steepness of the phantom potential and discuss the fate of Universe accordingly. |
1010.5949 | Mikhail Smolyakov | Mikhail N. Smolyakov | Bulk metric of brane world models and submanifolds in 6D
pseudo-Euclidean space-time | 5 pages, typos corrected | Int.J.Geom.Meth.Mod.Phys.8:239-243,2011 | 10.1142/S0219887811005105 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this short note, five-dimensional brane world models with dS_{4} metric on
the branes are discussed. The explicit coordinate transformations, which show
the equivalence between the bulk metric of these brane world models and the
metric induced on an appropriate submanifolds in the flat six-dimensional
pseudo-Euclidean space-time, are presented. The cases of the zero and non-zero
cosmological constant in the bulk are discussed in detail.
| [
{
"created": "Thu, 28 Oct 2010 12:55:21 GMT",
"version": "v1"
},
{
"created": "Wed, 3 Nov 2010 20:38:06 GMT",
"version": "v2"
}
] | 2011-03-22 | [
[
"Smolyakov",
"Mikhail N.",
""
]
] | In this short note, five-dimensional brane world models with dS_{4} metric on the branes are discussed. The explicit coordinate transformations, which show the equivalence between the bulk metric of these brane world models and the metric induced on an appropriate submanifolds in the flat six-dimensional pseudo-Euclidean space-time, are presented. The cases of the zero and non-zero cosmological constant in the bulk are discussed in detail. |
gr-qc/9712075 | Piotr Jaranowski | Piotr Jaranowski and Gerhard Schaefer | 3rd post-Newtonian higher order Hamilton dynamics for two-body
point-mass systems | LaTeX, 27 pages, submitted to Physical Review D | Phys.Rev.D57:7274-7291,1998; Erratum-ibid.D63:029902,2001 | 10.1103/PhysRevD.57.7274 10.1103/PhysRevD.63.029902 | null | gr-qc | null | The paper presents the conservative dynamics of two-body point-mass systems
up to the third post-Newtonian order ($1/c^6$). The two-body dynamics is given
in terms of a higher order ADM Hamilton function which results from a third
post-Newtonian Routh functional for the total field-plus-matter system. The
applied regularization procedures, together with making use of distributional
differentiation of homogeneous functions, give unique results for the terms in
the Hamilton function apart from the coefficient of the term $(\nu
p_{i}{\pa_{i}})^2r^{-1}$. The result suggests an invalidation of the binary
point-mass model at the third post-Newtonian order.
| [
{
"created": "Wed, 17 Dec 1997 14:54:20 GMT",
"version": "v1"
}
] | 2014-11-17 | [
[
"Jaranowski",
"Piotr",
""
],
[
"Schaefer",
"Gerhard",
""
]
] | The paper presents the conservative dynamics of two-body point-mass systems up to the third post-Newtonian order ($1/c^6$). The two-body dynamics is given in terms of a higher order ADM Hamilton function which results from a third post-Newtonian Routh functional for the total field-plus-matter system. The applied regularization procedures, together with making use of distributional differentiation of homogeneous functions, give unique results for the terms in the Hamilton function apart from the coefficient of the term $(\nu p_{i}{\pa_{i}})^2r^{-1}$. The result suggests an invalidation of the binary point-mass model at the third post-Newtonian order. |
1911.04398 | Vishnu S. Namboothiri | Vishnu S Namboothiri | Raychaudhuri Equation in Kaluza Klein space time | 12 pages | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We studied the Raychaudhuri equation in Kaluza-Klein space-time. We derived
an additional term that is solely due to Kaluza-Klein's unification. This term
affects the defocus of world lines near the singularity of charged
higher-dimensional black holes. We illustrated it with a static
higher-dimensional black hole generated by Einstein-Maxwell equations. It has
been found that the term derived modifies the repulsive effect of kaluza Klein
scalar on world lines. We proved some mathematical theorems which give an
insight into the interior of the black holes.
| [
{
"created": "Mon, 11 Nov 2019 17:10:29 GMT",
"version": "v1"
},
{
"created": "Sun, 24 Nov 2019 05:21:03 GMT",
"version": "v2"
}
] | 2019-11-26 | [
[
"Namboothiri",
"Vishnu S",
""
]
] | We studied the Raychaudhuri equation in Kaluza-Klein space-time. We derived an additional term that is solely due to Kaluza-Klein's unification. This term affects the defocus of world lines near the singularity of charged higher-dimensional black holes. We illustrated it with a static higher-dimensional black hole generated by Einstein-Maxwell equations. It has been found that the term derived modifies the repulsive effect of kaluza Klein scalar on world lines. We proved some mathematical theorems which give an insight into the interior of the black holes. |
1203.0395 | Varun Sahni | Varun Sahni and Aleksey Toporensky | Cosmological Hysteresis and the Cyclic Universe | 31 pages, 8 figures. Matches version published in Phys Rev D85,
123542 (2012) | Phys Rev D85, 123542 (2012) | 10.1103/PhysRevD.85.123542 | null | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A Universe filled with a homogeneous scalar field exhibits `Cosmological
hysteresis'. Cosmological hysteresis is caused by the asymmetry in the equation
of state during expansion and contraction. This asymmetry results in the
formation of a hysteresis loop: $\oint pdV$, whose value can be non-vanishing
during each oscillatory cycle. For flat potentials, a negative value of the
hysteresis loop leads to the increase in amplitude of consecutive cycles and to
a universe with older and larger successive cycles. Such a universe appears to
possess an arrow of time even though entropy production is absent and all of
the equations respect time-reversal symmetry ! Cosmological hysteresis appears
to be widespread and exists for a large class of scalar field potentials and
mechanisms for making the universe bounce. For steep potentials, the value of
the hysteresis loop can be positive as well as negative. The expansion factor
in this case displays quasi-periodic behaviour in which successive cycles can
be both larger as well as smaller than previous ones. This quasi-regular
pattern resembles the phenomenon of BEATS displayed by acoustic systems.
Remarkably, the expression relating the increase/decrease in oscillatory cycles
to the quantum of hysteresis appears to be model independent. The cyclic
scenario is extended to spatially anisotropic models and it is shown that the
anisotropy density decreases during successive cycles if the hysteresis loop is
negative.
| [
{
"created": "Fri, 2 Mar 2012 09:07:07 GMT",
"version": "v1"
},
{
"created": "Sat, 10 Mar 2012 07:43:03 GMT",
"version": "v2"
},
{
"created": "Tue, 3 Jul 2012 09:11:34 GMT",
"version": "v3"
}
] | 2013-05-30 | [
[
"Sahni",
"Varun",
""
],
[
"Toporensky",
"Aleksey",
""
]
] | A Universe filled with a homogeneous scalar field exhibits `Cosmological hysteresis'. Cosmological hysteresis is caused by the asymmetry in the equation of state during expansion and contraction. This asymmetry results in the formation of a hysteresis loop: $\oint pdV$, whose value can be non-vanishing during each oscillatory cycle. For flat potentials, a negative value of the hysteresis loop leads to the increase in amplitude of consecutive cycles and to a universe with older and larger successive cycles. Such a universe appears to possess an arrow of time even though entropy production is absent and all of the equations respect time-reversal symmetry ! Cosmological hysteresis appears to be widespread and exists for a large class of scalar field potentials and mechanisms for making the universe bounce. For steep potentials, the value of the hysteresis loop can be positive as well as negative. The expansion factor in this case displays quasi-periodic behaviour in which successive cycles can be both larger as well as smaller than previous ones. This quasi-regular pattern resembles the phenomenon of BEATS displayed by acoustic systems. Remarkably, the expression relating the increase/decrease in oscillatory cycles to the quantum of hysteresis appears to be model independent. The cyclic scenario is extended to spatially anisotropic models and it is shown that the anisotropy density decreases during successive cycles if the hysteresis loop is negative. |
2201.12824 | Xiaoning Wu | Xiaokai He, Xiaoning Wu and Naqing Xie | On the angular momentum of compact binary coalescence | 8 pages | null | 10.1088/1572-9494/acb7cf | null | gr-qc | http://creativecommons.org/licenses/by/4.0/ | The supertranslation ambiguity issue of angular momentum is a long-standing
problem in general relativity. Recently, there appeared the first definition of
angular momentum at null infinity that is supertranslation invariant. However,
in the compact binary coalescence community, supertranslation ambiguity is
often ignored. This paper demonstrates that we have the happy circumstance that
the newly defined angular momentum coincides with the classical definition at
the quadrupole level.
| [
{
"created": "Sun, 30 Jan 2022 14:12:10 GMT",
"version": "v1"
},
{
"created": "Thu, 5 May 2022 12:49:57 GMT",
"version": "v2"
}
] | 2023-04-26 | [
[
"He",
"Xiaokai",
""
],
[
"Wu",
"Xiaoning",
""
],
[
"Xie",
"Naqing",
""
]
] | The supertranslation ambiguity issue of angular momentum is a long-standing problem in general relativity. Recently, there appeared the first definition of angular momentum at null infinity that is supertranslation invariant. However, in the compact binary coalescence community, supertranslation ambiguity is often ignored. This paper demonstrates that we have the happy circumstance that the newly defined angular momentum coincides with the classical definition at the quadrupole level. |
1107.5410 | Anne Nzioki | Anne Marie Nzioki, Rituparno Goswami, Peter K.S. Dunsby and George F.
R. Ellis | On Shear-Free perturbations of FLRW Universes | null | Phys.Rev.D84:124028,2011 | 10.1103/PhysRevD.84.124028 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A surprising exact result for the Einstein Field Equations is that if
pressure-free matter is moving in a shear-free way, then it must be either
expansion-free or rotation-free. It has been suggested this result is also true
for any barotropic perfect fluid, but a proof has remained elusive. We consider
the case of barotropic perfect fluid solutions linearized about a
Robertson-Walker geometry, and prove that the result remains true except for
the case of a specific highly non-linear equation of state. We argue that this
equation of state is non-physical, and hence the result is true in the
linearized case for all physically realistic barotropic perfect fluids. This
result, which is not true in Newtonian cosmology, demonstrates that the
linearized solutions, believed to result in standard local Newtonian theory, do
not always give the usual behaviour of Newtonian solutions.
| [
{
"created": "Wed, 27 Jul 2011 08:29:56 GMT",
"version": "v1"
}
] | 2012-02-20 | [
[
"Nzioki",
"Anne Marie",
""
],
[
"Goswami",
"Rituparno",
""
],
[
"Dunsby",
"Peter K. S.",
""
],
[
"Ellis",
"George F. R.",
""
]
] | A surprising exact result for the Einstein Field Equations is that if pressure-free matter is moving in a shear-free way, then it must be either expansion-free or rotation-free. It has been suggested this result is also true for any barotropic perfect fluid, but a proof has remained elusive. We consider the case of barotropic perfect fluid solutions linearized about a Robertson-Walker geometry, and prove that the result remains true except for the case of a specific highly non-linear equation of state. We argue that this equation of state is non-physical, and hence the result is true in the linearized case for all physically realistic barotropic perfect fluids. This result, which is not true in Newtonian cosmology, demonstrates that the linearized solutions, believed to result in standard local Newtonian theory, do not always give the usual behaviour of Newtonian solutions. |
gr-qc/9607066 | Fernando Barbero | A. Tiemblo and R. Tresguerres | Time Evolution in Dynamical Spacetimes | 27 pages, TeX | null | null | null | gr-qc | null | We present a gauge--theoretical derivation of the notion of time, suitable to
describe the Hamiltonian time evolution of gravitational systems. It is based
on a nonlinear coset realization of the Poincar\'e group, implying the time
component of the coframe to be invariant, and thus to represent a metric time.
The unitary gauge fixing of the boosts gives rise to the foliation of spacetime
along the time direction. The three supressed degrees of freedom correspond to
Goldstone--like fields, whereas the remaining time component is a Higgs--like
boson.
| [
{
"created": "Fri, 26 Jul 1996 08:48:44 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Tiemblo",
"A.",
""
],
[
"Tresguerres",
"R.",
""
]
] | We present a gauge--theoretical derivation of the notion of time, suitable to describe the Hamiltonian time evolution of gravitational systems. It is based on a nonlinear coset realization of the Poincar\'e group, implying the time component of the coframe to be invariant, and thus to represent a metric time. The unitary gauge fixing of the boosts gives rise to the foliation of spacetime along the time direction. The three supressed degrees of freedom correspond to Goldstone--like fields, whereas the remaining time component is a Higgs--like boson. |
gr-qc/9312005 | null | Nadja S. Magalhaes and Carlos O. Escobar | Optimal Filters for the Detection of Continuous Gravitational Waves | 14 pages, REVTEX, Preprint IFUSP/P-1090 | null | null | null | gr-qc | null | We determine the transfer functions of two kinds of filters that can be used
in the detection of continuous gravitational radiation. The first one optimizes
the signal-to-noise ratio, and the second reproduces the wave with minimum
error. We analyse the behaviour of these filters in connection with actual
detection schemes.
| [
{
"created": "Thu, 2 Dec 1993 15:48:59 GMT",
"version": "v1"
}
] | 2009-09-25 | [
[
"Magalhaes",
"Nadja S.",
""
],
[
"Escobar",
"Carlos O.",
""
]
] | We determine the transfer functions of two kinds of filters that can be used in the detection of continuous gravitational radiation. The first one optimizes the signal-to-noise ratio, and the second reproduces the wave with minimum error. We analyse the behaviour of these filters in connection with actual detection schemes. |
1208.6158 | Ernesto Nungesser | Ernesto Nungesser | Future non-linear stability for solutions of the Einstein-Vlasov system
of Bianchi types II and VI$_0$ | 18 pages | (2012) J. Math. Phys. 53 102503 | 10.1063/1.4758930 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In a recent paper arXiv:1208.4231 we have treated the future non-linear
stability for reflection symmetric solutions of the Einstein-Vlasov system of
Bianchi types II and VI$_0$. We have been able now to remove the reflection
symmetry assumption, thus treating the non-diagonal case. Apart from the
increasing complexity the methods have been essentially the same as in the
diagonal case, showing that they are thus quite powerful.
Here the challenge was to put the equations in a form that permits the use of
the previous results. We are able to conclude that after a possible basis
change the future of the non-diagonal spacetimes in consideration is
asymptotically diagonal.
| [
{
"created": "Thu, 30 Aug 2012 12:59:43 GMT",
"version": "v1"
}
] | 2015-06-11 | [
[
"Nungesser",
"Ernesto",
""
]
] | In a recent paper arXiv:1208.4231 we have treated the future non-linear stability for reflection symmetric solutions of the Einstein-Vlasov system of Bianchi types II and VI$_0$. We have been able now to remove the reflection symmetry assumption, thus treating the non-diagonal case. Apart from the increasing complexity the methods have been essentially the same as in the diagonal case, showing that they are thus quite powerful. Here the challenge was to put the equations in a form that permits the use of the previous results. We are able to conclude that after a possible basis change the future of the non-diagonal spacetimes in consideration is asymptotically diagonal. |
1009.4332 | Wung-Hong Huang | Wung-Hong Huang | ADM Mass on General Spacetime and Hawking-Page Phase Transition in
Magnetic Black Brane | null | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We derive a formula which enable us to evaluate the ADM mass in a more
general curved spacetime. We apply the formula to evaluate the thermodynamical
quantities of the Melvin magnetic black D-branes. We see that there is the
Hawking-Page phase transition and the corresponding dual gauge theory will show
the confinement-deconfinement transition under magnetic flux.
| [
{
"created": "Wed, 22 Sep 2010 11:37:15 GMT",
"version": "v1"
}
] | 2010-09-23 | [
[
"Huang",
"Wung-Hong",
""
]
] | We derive a formula which enable us to evaluate the ADM mass in a more general curved spacetime. We apply the formula to evaluate the thermodynamical quantities of the Melvin magnetic black D-branes. We see that there is the Hawking-Page phase transition and the corresponding dual gauge theory will show the confinement-deconfinement transition under magnetic flux. |
gr-qc/0012007 | Jeremy S. Heyl | Jeremy S. Heyl | Electron-Positron Jets from a Critically Magnetized Black Hole | 10 pages, 6 figures, submitted to Phys. Rev. D | Phys.Rev.D63:064028,2001 | 10.1103/PhysRevD.63.064028 | null | gr-qc astro-ph hep-ph | null | The curved spacetime surrounding a rotating black hole dramatically alters
the structure of nearby electromagnetic fields. The Wald field which is an
asymptotically uniform magnetic field aligned with the angular momentum of the
hole provides a convenient starting point to analyze the effects of radiative
corrections on electrodynamics in curved spacetime. Since the curvature of the
spacetime is small on the scale of the electron's Compton wavelength, the tools
of quantum field theory in flat spacetime are reliable and show that a rotating
black hole immersed in a magnetic field approaching the quantum critical value
of $B_k=m^2 c^3/(e\hbar) \approx 4.4 \times 10^{13}$~G $\approx
1.3\times10^{-11}$ cm$^{-1}$ is unstable. Specifically, a maximally rotating
three-solar-mass black hole immersed in a magnetic field of $2.3 \times
10^{12}$~G would be a copious producer of electron-positron pairs with a
luminosity of $3 \times 10^{52}$ erg s$^{-1}$.
| [
{
"created": "Fri, 1 Dec 2000 19:40:30 GMT",
"version": "v1"
}
] | 2010-11-19 | [
[
"Heyl",
"Jeremy S.",
""
]
] | The curved spacetime surrounding a rotating black hole dramatically alters the structure of nearby electromagnetic fields. The Wald field which is an asymptotically uniform magnetic field aligned with the angular momentum of the hole provides a convenient starting point to analyze the effects of radiative corrections on electrodynamics in curved spacetime. Since the curvature of the spacetime is small on the scale of the electron's Compton wavelength, the tools of quantum field theory in flat spacetime are reliable and show that a rotating black hole immersed in a magnetic field approaching the quantum critical value of $B_k=m^2 c^3/(e\hbar) \approx 4.4 \times 10^{13}$~G $\approx 1.3\times10^{-11}$ cm$^{-1}$ is unstable. Specifically, a maximally rotating three-solar-mass black hole immersed in a magnetic field of $2.3 \times 10^{12}$~G would be a copious producer of electron-positron pairs with a luminosity of $3 \times 10^{52}$ erg s$^{-1}$. |
gr-qc/0408038 | Mauricio Bellini | Mauricio Bellini (Mar del Plata University & CONICET) | Back-reaction effect in power-law inflation | 6 pages, no figures (accepted in Il Nuovo Cimento B) | Nuovo Cim. B119 (2004) 191-195 | 10.1393/ncb/i2004-10066-1 | null | gr-qc astro-ph hep-ph | null | I consider a power-law inflationary model taking into account back-reaction
effects. The interesting result is that the spectrum for the scalar field
fluctuations does not depends on the expansion rate of the universe $p$ and
that it result to be scale invariant for cosmological scales. However, the
amplitude for these fluctuations depends on $p$.
| [
{
"created": "Thu, 12 Aug 2004 16:09:22 GMT",
"version": "v1"
}
] | 2009-11-10 | [
[
"Bellini",
"Mauricio",
"",
"Mar del Plata University & CONICET"
]
] | I consider a power-law inflationary model taking into account back-reaction effects. The interesting result is that the spectrum for the scalar field fluctuations does not depends on the expansion rate of the universe $p$ and that it result to be scale invariant for cosmological scales. However, the amplitude for these fluctuations depends on $p$. |
0809.1915 | Tiberiu Harko | M. E. Kahil, T. Harko | Is dark matter an extra-dimensional effect? | 11 pages, no figures, accepted for publication in MPLA; references
added | Mod.Phys.Lett.A24:667-682,2009 | 10.1142/S0217732309028667 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We investigate the possibility that the observed behavior of test particles
outside galaxies, which is usually explained by assuming the presence of dark
matter, is the result of the dynamical evolution of particles in higher
dimensional space-times. Hence, dark matter may be a direct consequence of the
presence of an extra force, generated by the presence of extra-dimensions,
which modifies the dynamic law of motion, but does not change the intrinsic
properties of the particles, like, for example, the mass (inertia). We discuss
in some detail several possible particular forms for the extra force, and the
acceleration law of the particles is derived. Therefore, the constancy of the
galactic rotation curves may be considered as an empirical evidence for the
existence of the extra dimensions.
| [
{
"created": "Thu, 11 Sep 2008 04:57:56 GMT",
"version": "v1"
},
{
"created": "Thu, 26 Mar 2009 05:02:42 GMT",
"version": "v2"
}
] | 2009-04-21 | [
[
"Kahil",
"M. E.",
""
],
[
"Harko",
"T.",
""
]
] | We investigate the possibility that the observed behavior of test particles outside galaxies, which is usually explained by assuming the presence of dark matter, is the result of the dynamical evolution of particles in higher dimensional space-times. Hence, dark matter may be a direct consequence of the presence of an extra force, generated by the presence of extra-dimensions, which modifies the dynamic law of motion, but does not change the intrinsic properties of the particles, like, for example, the mass (inertia). We discuss in some detail several possible particular forms for the extra force, and the acceleration law of the particles is derived. Therefore, the constancy of the galactic rotation curves may be considered as an empirical evidence for the existence of the extra dimensions. |
1305.0777 | Jose Geraldo Pereira | J. G. Pereira | Gravitational waves: a foundational review | This manuscript is a (revised and updated) compilation of the results
published in arXiv:0709.1603 and arXiv:0809.2911, and is intended as an arXiv
paper. V3: presentation changes aiming at clarifying the discussion | null | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The standard linear approach to the gravitational waves theory is critically
reviewed. Contrary to the prevalent understanding, it is pointed out that this
theory contains many conceptual and technical obscure issues that require
further analysis.
| [
{
"created": "Fri, 3 May 2013 16:55:54 GMT",
"version": "v1"
},
{
"created": "Thu, 25 Jul 2013 13:47:08 GMT",
"version": "v2"
},
{
"created": "Wed, 27 May 2015 12:06:22 GMT",
"version": "v3"
}
] | 2015-05-28 | [
[
"Pereira",
"J. G.",
""
]
] | The standard linear approach to the gravitational waves theory is critically reviewed. Contrary to the prevalent understanding, it is pointed out that this theory contains many conceptual and technical obscure issues that require further analysis. |
2010.09048 | Julio Arrechea | Julio Arrechea, Carlos Barcel\'o, Valentin Boyanov, Luis J. Garay | Vacuum semiclassical gravity does not leave space for safe singularities | 13 pages, 5 figures. Version accepted for publication in Universe.
This article belongs to the Special Issue "Gravitational Singularities and
Their Quantum Fates" | null | 10.3390/universe7080281 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | General relativity predicts its own demise at singularities, but also appears
to conveniently shield itself from the catastrophic consequences of such
singularities, making them safe. For instance, if strong cosmic censorship were
ultimately satisfied, spacetime singularities, although present, would not pose
any practical problems to predictability. Here we argue that under
semiclassical effects the situation should be rather different: the potential
singularities which could appear in the theory will generically affect
predictability and so one will be forced to analyse whether there is a way to
regularise them. For these possible regularisations, the presence and behaviour
of matter during gravitational collapse and stabilisation into new structures
will play a key role. First we show that the static semiclassical counterparts
to the Schwarzschild and Reissner-Nordstr\"om geometries have singularities
which are no longer hidden behind horizons. Then we argue that in dynamical
scenarios of formation and evaporation of black holes, we are left with only
three possible outcomes which could avoid singularities and eventual
predictability issues. We briefly analyse the viability of each one of them
within semiclassical gravity, and discuss the expected characteristic
timescales of their evolution.
| [
{
"created": "Sun, 18 Oct 2020 17:57:01 GMT",
"version": "v1"
},
{
"created": "Mon, 9 Aug 2021 09:18:56 GMT",
"version": "v2"
}
] | 2021-08-12 | [
[
"Arrechea",
"Julio",
""
],
[
"Barceló",
"Carlos",
""
],
[
"Boyanov",
"Valentin",
""
],
[
"Garay",
"Luis J.",
""
]
] | General relativity predicts its own demise at singularities, but also appears to conveniently shield itself from the catastrophic consequences of such singularities, making them safe. For instance, if strong cosmic censorship were ultimately satisfied, spacetime singularities, although present, would not pose any practical problems to predictability. Here we argue that under semiclassical effects the situation should be rather different: the potential singularities which could appear in the theory will generically affect predictability and so one will be forced to analyse whether there is a way to regularise them. For these possible regularisations, the presence and behaviour of matter during gravitational collapse and stabilisation into new structures will play a key role. First we show that the static semiclassical counterparts to the Schwarzschild and Reissner-Nordstr\"om geometries have singularities which are no longer hidden behind horizons. Then we argue that in dynamical scenarios of formation and evaporation of black holes, we are left with only three possible outcomes which could avoid singularities and eventual predictability issues. We briefly analyse the viability of each one of them within semiclassical gravity, and discuss the expected characteristic timescales of their evolution. |
1306.6441 | Nicholas Tsamis | N. C. Tsamis (U. Crete) and R. P. Woodard (U. Florida) | Pure Gravitational Back-Reaction Observables | 15 pages, uses LaTeX2e | null | 10.1103/PhysRevD.88.044040 | CCTP-2013-09, UFIFT-QG-13-06 | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | After discussing the various issues regarding and requirements on pure
quantum gravitational observables in homogeneous-isotropic conditions, we
construct a composite operator observable satisfying most of them. We also
expand it to first order in the loop counting parameter and suggest it as a
physical quantifier of gravitational back-reaction in an initially inflating
cosmology.
| [
{
"created": "Thu, 27 Jun 2013 09:18:27 GMT",
"version": "v1"
}
] | 2015-06-16 | [
[
"Tsamis",
"N. C.",
"",
"U. Crete"
],
[
"Woodard",
"R. P.",
"",
"U. Florida"
]
] | After discussing the various issues regarding and requirements on pure quantum gravitational observables in homogeneous-isotropic conditions, we construct a composite operator observable satisfying most of them. We also expand it to first order in the loop counting parameter and suggest it as a physical quantifier of gravitational back-reaction in an initially inflating cosmology. |
gr-qc/0405048 | Jian-Miin Liu | Jian-Miin Liu | Equilibrium velocity distribution of low-energy particles in spherically
symmetric gravitational field | 10 pages with no figure | Fronties in Field Theory, ed. O. Kovras, Nova Science Publishers
(New York, 2005), pp317-331 | null | null | gr-qc cond-mat.stat-mech | null | Based on Einstein's theory of gravitation, we discuss the influence of a
spherically symmetric gravitational field on Maxwell's law of velocity
distribution. We derive the equilibrium velocity distribution of low-energy
particles in the spherically symmetric gravitational field and calculate the
escape rate of low-energy particles in a container with a leak placed in the
spherically symmetric gravitational field. They can serve as the tests of
Einstein's theory of gravitation.
| [
{
"created": "Sun, 9 May 2004 12:00:50 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Liu",
"Jian-Miin",
""
]
] | Based on Einstein's theory of gravitation, we discuss the influence of a spherically symmetric gravitational field on Maxwell's law of velocity distribution. We derive the equilibrium velocity distribution of low-energy particles in the spherically symmetric gravitational field and calculate the escape rate of low-energy particles in a container with a leak placed in the spherically symmetric gravitational field. They can serve as the tests of Einstein's theory of gravitation. |
2311.01756 | Boris Latosh | Boris Latosh, Miok Park | Black Holes in Einstein-scalar-Gauss-Bonnet model probed with scattering
amplitudes | 28 pages, 4 figures | null | null | CTPU-PTC-23-46 | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We examined the quantum properties of scalar-tensor gravity with a coupling
to the Gauss-Bonnet term in the low energy limit, exploring both linear and
quadratic couplings. We calculated the leading-order corrections to the
non-relativistic one-body gravitational potential and the metric by studying
the gravitational field of a point-like scalar particle. We studied light-like
scattering and compared it with the classical theory. We found that the
non-minimal coupling does not contribute to the small-angle scattering for the
quadratic coupling but does in the case of linear coupling. The results provide
an opportunity to constrain the linear non-minimal coupling to the Gauss-Bonnet
term with forthcoming observational data.
| [
{
"created": "Fri, 3 Nov 2023 07:27:05 GMT",
"version": "v1"
},
{
"created": "Fri, 10 Nov 2023 06:01:03 GMT",
"version": "v2"
},
{
"created": "Fri, 21 Jun 2024 05:35:37 GMT",
"version": "v3"
}
] | 2024-06-24 | [
[
"Latosh",
"Boris",
""
],
[
"Park",
"Miok",
""
]
] | We examined the quantum properties of scalar-tensor gravity with a coupling to the Gauss-Bonnet term in the low energy limit, exploring both linear and quadratic couplings. We calculated the leading-order corrections to the non-relativistic one-body gravitational potential and the metric by studying the gravitational field of a point-like scalar particle. We studied light-like scattering and compared it with the classical theory. We found that the non-minimal coupling does not contribute to the small-angle scattering for the quadratic coupling but does in the case of linear coupling. The results provide an opportunity to constrain the linear non-minimal coupling to the Gauss-Bonnet term with forthcoming observational data. |
2405.12290 | Vitor Cardoso | Vitor Cardoso, Gregorio Carullo, Marina De Amicis, Francisco Duque,
Takuya Katagiri, David Pereniguez, Jaime Redondo-Yuste, Thomas F.M. Spieksma,
Zhen Zhong | Hushing black holes: tails in dynamical spacetimes | 13 pages, to appear in Physical Review D Letters | Phys. Rev. D 109, L121502 (2024) | 10.1103/PhysRevD.109.L121502 | null | gr-qc astro-ph.HE math-ph math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Stationary, asymptotically flat, black hole solutions of the vacuum field
equations of General Relativity belong to the Kerr family. But how does one
approach this state, dynamically? Linearized fluctuations decay at late times,
at fixed spatial position, as a Price power law for generic initial conditions.
However, little attention was paid to forced and nonlinear spacetimes, where
matter and nonlinearities play a role. We uncover a new, source-driven tail
governing waves generated by pointlike matter and nonlinearities, which can
dominate over Price's decay.
| [
{
"created": "Mon, 20 May 2024 18:00:20 GMT",
"version": "v1"
}
] | 2024-06-27 | [
[
"Cardoso",
"Vitor",
""
],
[
"Carullo",
"Gregorio",
""
],
[
"De Amicis",
"Marina",
""
],
[
"Duque",
"Francisco",
""
],
[
"Katagiri",
"Takuya",
""
],
[
"Pereniguez",
"David",
""
],
[
"Redondo-Yuste",
"Jaime",
""
],
[
"Spieksma",
"Thomas F. M.",
""
],
[
"Zhong",
"Zhen",
""
]
] | Stationary, asymptotically flat, black hole solutions of the vacuum field equations of General Relativity belong to the Kerr family. But how does one approach this state, dynamically? Linearized fluctuations decay at late times, at fixed spatial position, as a Price power law for generic initial conditions. However, little attention was paid to forced and nonlinear spacetimes, where matter and nonlinearities play a role. We uncover a new, source-driven tail governing waves generated by pointlike matter and nonlinearities, which can dominate over Price's decay. |
gr-qc/0606011 | Celine Cattoen | Celine Cattoen (Victoria University of Wellington) | Cosmological milestones and gravastars - topics in general relativity | 171 pages; MSc thesis | null | null | null | gr-qc | null | In this thesis, we consider two different problems relevant to general
relativity. Over the last few years, opinions on physically relevant
singularities occurring in FRW cosmologies have considerably changed. We
present an extensive catalogue of such cosmological milestones using
generalized power series both at the kinematical and dynamical level. We define
the notion of "scale factor singularity" and explore its relation to polynomial
and differential curvature singularities. We also extract dynamical information
using the Friedmann equations and derive necessary and sufficient conditions
for the existence of cosmological milestones such as big bangs, big crunches,
big rips, sudden singularities and extremality events. Specifically, we provide
a complete characterization of cosmological milestones for which the dominant
energy condition is satisfied. The second problem looks at one of the very
small number of serious alternatives to the usual concept of an astrophysical
black hole, that is, the gravastar model developed by Mazur and Mottola. By
considering a generalized class of similar models with continuous pressure (no
infinitesimally thin shells) and negative central pressure, we demonstrate that
gravastars cannot be perfect fluid spheres: anisotropic pressures are
unavoidable. We provide bounds on the necessary anisotropic pressure and show
that these transverse stresses that support a gravastar permit a higher
compactness than is given by the Buchdahl-Bondi bound for perfect fluid stars.
We also comment on the qualitative features of the equation of state that such
gravastar-like objects without any horizon must have.
| [
{
"created": "Fri, 2 Jun 2006 01:35:50 GMT",
"version": "v1"
},
{
"created": "Mon, 5 Jun 2006 22:30:18 GMT",
"version": "v2"
}
] | 2007-05-23 | [
[
"Cattoen",
"Celine",
"",
"Victoria University of Wellington"
]
] | In this thesis, we consider two different problems relevant to general relativity. Over the last few years, opinions on physically relevant singularities occurring in FRW cosmologies have considerably changed. We present an extensive catalogue of such cosmological milestones using generalized power series both at the kinematical and dynamical level. We define the notion of "scale factor singularity" and explore its relation to polynomial and differential curvature singularities. We also extract dynamical information using the Friedmann equations and derive necessary and sufficient conditions for the existence of cosmological milestones such as big bangs, big crunches, big rips, sudden singularities and extremality events. Specifically, we provide a complete characterization of cosmological milestones for which the dominant energy condition is satisfied. The second problem looks at one of the very small number of serious alternatives to the usual concept of an astrophysical black hole, that is, the gravastar model developed by Mazur and Mottola. By considering a generalized class of similar models with continuous pressure (no infinitesimally thin shells) and negative central pressure, we demonstrate that gravastars cannot be perfect fluid spheres: anisotropic pressures are unavoidable. We provide bounds on the necessary anisotropic pressure and show that these transverse stresses that support a gravastar permit a higher compactness than is given by the Buchdahl-Bondi bound for perfect fluid stars. We also comment on the qualitative features of the equation of state that such gravastar-like objects without any horizon must have. |
gr-qc/0604005 | Malik Rakhmanov | Malik Rakhmanov | Rank deficiency and Tikhonov regularization in the inverse problem for
gravitational-wave bursts | 12 pages, 5 figures | Class.Quant.Grav.23:S673-S686,2006 | 10.1088/0264-9381/23/19/S05 | LIGO-P060005 | gr-qc | null | Coherent techniques for searches of gravitational-wave bursts effectively
combine data from several detectors, taking into account differences in their
responses. The efforts are now focused on the maximum likelihood principle as
the most natural way to combine data, which can also be used without prior
knowledge of the signal. Recent studies however have shown that straightforward
application of the maximum likelihood method to gravitational waves with
unknown waveforms can lead to inconsistencies and unphysical results such as
discontinuity in the residual functional, or divergence of the variance of the
estimated waveforms for some locations in the sky. So far the solutions to
these problems have been based on rather different physical arguments.
Following these investigations, we now find that all these inconsistencies stem
from rank deficiency of the underlying network response matrix. In this paper
we show that the detection of gravitational-wave bursts with a network of
interferometers belongs to the category of ill-posed problems. We then apply
the method of Tikhonov regularization to resolve the rank deficiency and
introduce a minimal regulator which yields a well-conditioned solution to the
inverse problem for all locations on the sky.
| [
{
"created": "Mon, 3 Apr 2006 01:09:31 GMT",
"version": "v1"
},
{
"created": "Wed, 5 Apr 2006 01:16:09 GMT",
"version": "v2"
},
{
"created": "Tue, 19 Sep 2006 17:00:45 GMT",
"version": "v3"
}
] | 2009-11-11 | [
[
"Rakhmanov",
"Malik",
""
]
] | Coherent techniques for searches of gravitational-wave bursts effectively combine data from several detectors, taking into account differences in their responses. The efforts are now focused on the maximum likelihood principle as the most natural way to combine data, which can also be used without prior knowledge of the signal. Recent studies however have shown that straightforward application of the maximum likelihood method to gravitational waves with unknown waveforms can lead to inconsistencies and unphysical results such as discontinuity in the residual functional, or divergence of the variance of the estimated waveforms for some locations in the sky. So far the solutions to these problems have been based on rather different physical arguments. Following these investigations, we now find that all these inconsistencies stem from rank deficiency of the underlying network response matrix. In this paper we show that the detection of gravitational-wave bursts with a network of interferometers belongs to the category of ill-posed problems. We then apply the method of Tikhonov regularization to resolve the rank deficiency and introduce a minimal regulator which yields a well-conditioned solution to the inverse problem for all locations on the sky. |
1204.2015 | Hongwei Yu | Wenting Zhou and Hongwei Yu | Can spacetime curvature induced corrections to Lamb shift be observable? | 13 pages, 3 figures, slight title change, clarifications and more
discussions added, version to be published in JHEP | JHEP 10(2012)172 | 10.1007/JHEP10(2012)172 | null | gr-qc astro-ph.HE hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Lamb shift results from the coupling of an atom to vacuum fluctuations of
quantum fields, so corrections are expected to arise when the spacetime is
curved since the vacuum fluctuations are modified by the presence of spacetime
curvature. Here, we calculate the curvature-induced correction to the Lamb
shift outside a spherically symmetric object and demonstrate that this
correction can be remarkably significant outside a compact massive
astrophysical body. For instance, for a neutron star or a stellar mass black
hole, the correction is $\sim$ 25% at a radial distance of $4GM/c^2$, $\sim$
16% at $10GM/c^2$ and as large as $\sim$ 1.6% even at $100GM/c^2$, where $M$ is
the mass of the object, $G$ the Newtonian constant, and $c$ the speed of light.
In principle, we can look at the spectra from a distant compact super-massive
body to find such corrections. Therefore, our results suggest a possible way of
detecting fundamental quantum effects in astronomical observations.
| [
{
"created": "Tue, 10 Apr 2012 00:24:58 GMT",
"version": "v1"
},
{
"created": "Wed, 10 Oct 2012 04:52:04 GMT",
"version": "v2"
}
] | 2012-11-02 | [
[
"Zhou",
"Wenting",
""
],
[
"Yu",
"Hongwei",
""
]
] | The Lamb shift results from the coupling of an atom to vacuum fluctuations of quantum fields, so corrections are expected to arise when the spacetime is curved since the vacuum fluctuations are modified by the presence of spacetime curvature. Here, we calculate the curvature-induced correction to the Lamb shift outside a spherically symmetric object and demonstrate that this correction can be remarkably significant outside a compact massive astrophysical body. For instance, for a neutron star or a stellar mass black hole, the correction is $\sim$ 25% at a radial distance of $4GM/c^2$, $\sim$ 16% at $10GM/c^2$ and as large as $\sim$ 1.6% even at $100GM/c^2$, where $M$ is the mass of the object, $G$ the Newtonian constant, and $c$ the speed of light. In principle, we can look at the spectra from a distant compact super-massive body to find such corrections. Therefore, our results suggest a possible way of detecting fundamental quantum effects in astronomical observations. |
1907.12940 | Amir Hadi Ziaie | H. Moradpour, A. H. Ziaie, S. Ghaffari, and F. Feleppa | The generalized and extended uncertainty principles and their
implications on the Jeans mass | 6 pages, 2 figures | MNRAS 488 L69 (2019) | 10.1093/mnrasl/slz098 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The generalized and extended uncertainty principles affect the Newtonian
gravity and also the geometry of the thermodynamic phase space. Under the
influence of the latter, the energy-temperature relation of ideal gas may
change. Moreover, it seems that the Newtonian gravity is modified in the
framework of the R\'{e}nyi entropy formalism motivated by both the long-range
nature of gravity, and the extended uncertainty principle. Here, the
consequences of employing the generalized and extended uncertainty principles,
instead of the Heisenberg uncertainty principle, on the Jeans mass are studied.
The results of working in the R\'{e}nyi entropy formalism are also addressed.
It is shown that unlike the extended uncertainty principle and the R\'{e}nyi
entropy formalism which lead to the same increase in the Jeans mass, the
generalized uncertainty principle can decrease it. The latter means that a
cloud with mass smaller than the standard Jeans mass, obtained in the framework
of the Newtonian gravity, may also undergo the gravitational collapse process.
| [
{
"created": "Sun, 28 Jul 2019 07:25:05 GMT",
"version": "v1"
}
] | 2019-07-31 | [
[
"Moradpour",
"H.",
""
],
[
"Ziaie",
"A. H.",
""
],
[
"Ghaffari",
"S.",
""
],
[
"Feleppa",
"F.",
""
]
] | The generalized and extended uncertainty principles affect the Newtonian gravity and also the geometry of the thermodynamic phase space. Under the influence of the latter, the energy-temperature relation of ideal gas may change. Moreover, it seems that the Newtonian gravity is modified in the framework of the R\'{e}nyi entropy formalism motivated by both the long-range nature of gravity, and the extended uncertainty principle. Here, the consequences of employing the generalized and extended uncertainty principles, instead of the Heisenberg uncertainty principle, on the Jeans mass are studied. The results of working in the R\'{e}nyi entropy formalism are also addressed. It is shown that unlike the extended uncertainty principle and the R\'{e}nyi entropy formalism which lead to the same increase in the Jeans mass, the generalized uncertainty principle can decrease it. The latter means that a cloud with mass smaller than the standard Jeans mass, obtained in the framework of the Newtonian gravity, may also undergo the gravitational collapse process. |
1306.5820 | Jan Steinhoff | Sayan Chakrabarti, T\'erence Delsate, Jan Steinhoff | Effective action and linear response of compact objects in Newtonian
gravity | RevTeX, 19 pages, 1 figure, 1 table, relativistic generalization in
arXiv:1304.2228 [gr-qc]. v2: minor corrections and additions, v3: published
version | Phys. Rev. D 88, 084038 (2013) | 10.1103/PhysRevD.88.084038 | null | gr-qc astro-ph.SR | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We apply an effective field theory method for the gravitational interaction
of compact stars, developed within the context of general relativity, to
Newtonian gravity. In this effective theory a compact object is represented by
a point particle possessing generic gravitational multipole moments. The time
evolution of the multipoles depends on excitations due to external fields. This
can formally be described by a response function of the multipoles to applied
fields. The poles of this response correspond to the normal oscillation modes
of the star. This gives rise to resonances between modes and tidal forces in
binary systems. The connection to the standard formalism for tidal interactions
and resonances in Newtonian gravity is worked out. Our approach can be applied
to more complicated situations. In particular, a generalization to general
relativity is possible.
| [
{
"created": "Tue, 25 Jun 2013 01:11:14 GMT",
"version": "v1"
},
{
"created": "Tue, 2 Jul 2013 14:59:59 GMT",
"version": "v2"
},
{
"created": "Sat, 26 Oct 2013 18:28:19 GMT",
"version": "v3"
}
] | 2013-10-30 | [
[
"Chakrabarti",
"Sayan",
""
],
[
"Delsate",
"Térence",
""
],
[
"Steinhoff",
"Jan",
""
]
] | We apply an effective field theory method for the gravitational interaction of compact stars, developed within the context of general relativity, to Newtonian gravity. In this effective theory a compact object is represented by a point particle possessing generic gravitational multipole moments. The time evolution of the multipoles depends on excitations due to external fields. This can formally be described by a response function of the multipoles to applied fields. The poles of this response correspond to the normal oscillation modes of the star. This gives rise to resonances between modes and tidal forces in binary systems. The connection to the standard formalism for tidal interactions and resonances in Newtonian gravity is worked out. Our approach can be applied to more complicated situations. In particular, a generalization to general relativity is possible. |
2406.08813 | Yongqiang Wang | Tian-Xiang Ma, Yong-Qiang Wang | Frozen boson stars in an infinite tower of higher-derivative gravity | 19 pages, 8 figures | null | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, we present a solution for a five-dimensional boson star under
gravity with infinite tower of higher curvature corrections. We discover that
when the coupling constant exceeds a certain threshold, an alternative
configuration emerges, distinct from the conventional five-dimensional boson
star. This new structure is characterized by a broader frequency range, with
its minimum value approaching zero. At a truncation of $n=2$ for the correction
order, the solution and its scalar curvature diverge as the frequency
approaches zero. However, as the order of higher curvature corrections
increases, the singularity at the center vanishes, resulting in a globally
regular solution. Additionally, as the frequency approaches zero, the scalar
field's radial distribution becomes concentrated within the critical radius
$r_c$, forming what we term a ``frozen star". Beyond this radius, the metric of
the frozen star almost degenerates into that of an extreme black hole. The
solutions for such frozen stars offer a new avenue for exploring the enigmatic
interiors of compact celestial bodies, enhancing our understanding of the
internal structure of black holes under semi-classical conditions and
potentially addressing the series of paradoxes associated with information loss
due to singularities and horizons.
| [
{
"created": "Thu, 13 Jun 2024 05:11:14 GMT",
"version": "v1"
}
] | 2024-06-14 | [
[
"Ma",
"Tian-Xiang",
""
],
[
"Wang",
"Yong-Qiang",
""
]
] | In this paper, we present a solution for a five-dimensional boson star under gravity with infinite tower of higher curvature corrections. We discover that when the coupling constant exceeds a certain threshold, an alternative configuration emerges, distinct from the conventional five-dimensional boson star. This new structure is characterized by a broader frequency range, with its minimum value approaching zero. At a truncation of $n=2$ for the correction order, the solution and its scalar curvature diverge as the frequency approaches zero. However, as the order of higher curvature corrections increases, the singularity at the center vanishes, resulting in a globally regular solution. Additionally, as the frequency approaches zero, the scalar field's radial distribution becomes concentrated within the critical radius $r_c$, forming what we term a ``frozen star". Beyond this radius, the metric of the frozen star almost degenerates into that of an extreme black hole. The solutions for such frozen stars offer a new avenue for exploring the enigmatic interiors of compact celestial bodies, enhancing our understanding of the internal structure of black holes under semi-classical conditions and potentially addressing the series of paradoxes associated with information loss due to singularities and horizons. |
gr-qc/0106033 | Uzan Jean Philippe | Evelise Gausmann, Roland Lehoucq, Jean-Pierre Luminet, Jean-Philippe
Uzan, and Jeffrey Weeks | Topological Lensing in Spherical Spaces | 32 pages, 26 figures | Class.Quant.Grav.18:5155-5186,2001 | 10.1088/0264-9381/18/23/311 | null | gr-qc astro-ph | null | This article gives the construction and complete classification of all
three-dimensional spherical manifolds, and orders them by decreasing volume, in
the context of multiconnected universe models with positive spatial curvature.
It discusses which spherical topologies are likely to be detectable by
crystallographic methods using three-dimensional catalogs of cosmic objects.
The expected form of the pair separation histogram is predicted (including the
location and height of the spikes) and is compared to computer simulations,
showing that this method is stable with respect to observational uncertainties
and is well suited for detecting spherical topologies.
| [
{
"created": "Mon, 11 Jun 2001 09:48:03 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Gausmann",
"Evelise",
""
],
[
"Lehoucq",
"Roland",
""
],
[
"Luminet",
"Jean-Pierre",
""
],
[
"Uzan",
"Jean-Philippe",
""
],
[
"Weeks",
"Jeffrey",
""
]
] | This article gives the construction and complete classification of all three-dimensional spherical manifolds, and orders them by decreasing volume, in the context of multiconnected universe models with positive spatial curvature. It discusses which spherical topologies are likely to be detectable by crystallographic methods using three-dimensional catalogs of cosmic objects. The expected form of the pair separation histogram is predicted (including the location and height of the spikes) and is compared to computer simulations, showing that this method is stable with respect to observational uncertainties and is well suited for detecting spherical topologies. |
1308.4510 | Mojahed Parsi Mood | M. Parsi Mood, Javad T. Firouzjaee, Reza Mansouri | Gravitational Lensing by a structure in a cosmological background | 13 pages, 16 figures | Physical Review D 88, 083011 (2013) | 10.1103/PhysRevD.88.083011 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We use an exact general relativistic model structure within an FRW
cosmological background based on a LTB metric to study the gravitational
lensing by a cosmological and dynamical structure. Using different density
profiles for the model structure, the deviation angle and the time delay
through the gravitational lensing has been studied by solving the geodesic
equations. The results of these exact calculations have been compared to the
thin lens approximation. We have shown that the result for the thin lens
approximation based on a modified NFW density profile with a void before going
over to the FRW background matches very well with the exact general
relativistic calculations. However, the thin lens approximation based on a
normal NFW profile does differ from the exact relativistic calculation. The
difference is more the less compact the structure is. We have also looked at
the impact of our calculation on the observational interpretation of arcs in
the case of strong lensing and also the reduced shear in the case of weak
lensing. No significant difference has been seen in the data available.
| [
{
"created": "Wed, 21 Aug 2013 08:36:22 GMT",
"version": "v1"
}
] | 2013-11-28 | [
[
"Mood",
"M. Parsi",
""
],
[
"Firouzjaee",
"Javad T.",
""
],
[
"Mansouri",
"Reza",
""
]
] | We use an exact general relativistic model structure within an FRW cosmological background based on a LTB metric to study the gravitational lensing by a cosmological and dynamical structure. Using different density profiles for the model structure, the deviation angle and the time delay through the gravitational lensing has been studied by solving the geodesic equations. The results of these exact calculations have been compared to the thin lens approximation. We have shown that the result for the thin lens approximation based on a modified NFW density profile with a void before going over to the FRW background matches very well with the exact general relativistic calculations. However, the thin lens approximation based on a normal NFW profile does differ from the exact relativistic calculation. The difference is more the less compact the structure is. We have also looked at the impact of our calculation on the observational interpretation of arcs in the case of strong lensing and also the reduced shear in the case of weak lensing. No significant difference has been seen in the data available. |
2307.13026 | Geraint Pratten | Geraint Pratten, Patricia Schmidt, Hannah Middleton, Alberto Vecchio | Precision tracking of massive black hole spin evolution with LISA | 14+6 pages, 8 figures, fixed typo | null | null | null | gr-qc astro-ph.GA astro-ph.IM | http://creativecommons.org/licenses/by/4.0/ | The Laser Interferometer Space Antenna (LISA) will play a vital role in
constraining the origin and evolution of massive black holes throughout the
Universe. In this study we use a waveform model (IMRPhenomXPHM) that includes
both precession and higher multipoles, and full Bayesian inference to explore
the accuracy to which LISA can constrain the binary parameters. We demonstrate
that LISA will be able to track the evolution of the spins -- magnitude and
orientation -- to percent accuracy, providing crucial information on the
dynamics and evolution of massive black hole binaries and the galactic
environment in which the merger takes place. Such accurate spin-tracking
further allows LISA to measure the recoil velocity of the remnant black hole to
better than $100\,\mathrm{km}\,\mathrm{s}^{-1}$ (90\% credibility) and its
direction to a few degrees, which provides additional important astrophysical
information on the post-merger association. Using a systematic suite of
binaries, we showcase that the component masses will be measurable at the
sub-percent level, the sky area can be constrained to within $\Delta
\Omega_{90} \approx 0.01 \, \rm{deg}^2$, and the binary redshift to less than
$0.01$.
| [
{
"created": "Mon, 24 Jul 2023 18:00:01 GMT",
"version": "v1"
},
{
"created": "Thu, 27 Jul 2023 14:01:23 GMT",
"version": "v2"
}
] | 2023-07-28 | [
[
"Pratten",
"Geraint",
""
],
[
"Schmidt",
"Patricia",
""
],
[
"Middleton",
"Hannah",
""
],
[
"Vecchio",
"Alberto",
""
]
] | The Laser Interferometer Space Antenna (LISA) will play a vital role in constraining the origin and evolution of massive black holes throughout the Universe. In this study we use a waveform model (IMRPhenomXPHM) that includes both precession and higher multipoles, and full Bayesian inference to explore the accuracy to which LISA can constrain the binary parameters. We demonstrate that LISA will be able to track the evolution of the spins -- magnitude and orientation -- to percent accuracy, providing crucial information on the dynamics and evolution of massive black hole binaries and the galactic environment in which the merger takes place. Such accurate spin-tracking further allows LISA to measure the recoil velocity of the remnant black hole to better than $100\,\mathrm{km}\,\mathrm{s}^{-1}$ (90\% credibility) and its direction to a few degrees, which provides additional important astrophysical information on the post-merger association. Using a systematic suite of binaries, we showcase that the component masses will be measurable at the sub-percent level, the sky area can be constrained to within $\Delta \Omega_{90} \approx 0.01 \, \rm{deg}^2$, and the binary redshift to less than $0.01$. |
2209.00020 | Christian Pfeifer | Sebastian Bahamonde and Shokoufe Faraji and Eva Hackmann and Christian
Pfeifer | Thick accretion disk configurations in the Born-Infeld teleparallel
gravity | null | Physical Review D (Vol. 106, No. 8), 2022 | 10.1103/PhysRevD.106.084046 | null | gr-qc astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The main goal of this paper is to investigate one of the important
astrophysical systems, namely Thick accretion disks, in the background of the
spherically symmetric solution in Born-Infeld teleparallel gravity to examine
observable predictions of the theory in the vicinity of black holes. Thus, the
properties of the non-self-gravitating equilibrium surfaces characterising the
Thick accretion disks model are studied. In addition, we find an observational
bound on the parameter of the model as $\lambda\gtrsim 140$. We show this
analytical accretion disk model for different values of $\lambda$ and compare
the result with the corresponding Schwarzschild solution in the general theory
of relativity.
| [
{
"created": "Wed, 31 Aug 2022 18:00:01 GMT",
"version": "v1"
},
{
"created": "Wed, 26 Oct 2022 15:52:20 GMT",
"version": "v2"
}
] | 2022-10-27 | [
[
"Bahamonde",
"Sebastian",
""
],
[
"Faraji",
"Shokoufe",
""
],
[
"Hackmann",
"Eva",
""
],
[
"Pfeifer",
"Christian",
""
]
] | The main goal of this paper is to investigate one of the important astrophysical systems, namely Thick accretion disks, in the background of the spherically symmetric solution in Born-Infeld teleparallel gravity to examine observable predictions of the theory in the vicinity of black holes. Thus, the properties of the non-self-gravitating equilibrium surfaces characterising the Thick accretion disks model are studied. In addition, we find an observational bound on the parameter of the model as $\lambda\gtrsim 140$. We show this analytical accretion disk model for different values of $\lambda$ and compare the result with the corresponding Schwarzschild solution in the general theory of relativity. |
1805.11579 | LVC Publications | The LIGO Scientific Collaboration, the Virgo Collaboration, B. P.
Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, T. Adams,
P. Addesso, R. X. Adhikari, V. B. Adya, C. Affeldt, B. Agarwal, M. Agathos,
K. Agatsuma, N. Aggarwal, O. D. Aguiar, L. Aiello, A. Ain, P. Ajith, B.
Allen, G. Allen, A. Allocca, M. A. Aloy, P. A. Altin, A. Amato, A. Ananyeva,
S. B. Anderson, W. G. Anderson, S. V. Angelova, S. Antier, S. Appert, K.
Arai, M. C. Araya, J. S. Areeda, M. Ar`ene, N. Arnaud, K. G. Arun, S.
Ascenzi, G. Ashton, M. Ast, S. M. Aston, P. Astone, D. V. Atallah, F. Aubin,
P. Aufmuth, C. Aulbert, K. AultONeal, C. Austin, A. Avila-Alvarez, S. Babak,
P. Bacon, F. Badaracco, M. K. M. Bader, S. Bae, P. T. Baker, F. Baldaccini,
G. Ballardin, S. W. Ballmer, S. Banagiri, J. C. Barayoga, S. E. Barclay, B.
C. Barish, D. Barker, K. Barkett, S. Barnum, F. Barone, B. Barr, L. Barsotti,
M. Barsuglia, D. Barta, J. Bartlett, I. Bartos, R. Bassiri, A. Basti, J. C.
Batch, M. Bawaj, J. C. Bayley, M. Bazzan, B. B'ecsy, C. Beer, M. Bejger, I.
Belahcene, A. S. Bell, D. Beniwal, M. Bensch, B. K. Berger, G. Bergmann, S.
Bernuzzi, J. J. Bero, C. P. L. Berry, D. Bersanetti, A. Bertolini, J.
Betzwieser, R. Bhandare, I. A. Bilenko, S. A. Bilgili, G. Billingsley, C. R.
Billman, J. Birch, R. Birney, O. Birnholtz, S. Biscans, S. Biscoveanu, A.
Bisht, M. Bitossi, M. A. Bizouard, J. K. Blackburn, J. Blackman, C. D. Blair,
D. G. Blair, R. M. Blair, S. Bloemen, O. Bock, N. Bode, M. Boer, Y. Boetzel,
G. Bogaert, A. Bohe, 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, F. Brighenti, A. Brillet, M. Brinkmann, V.
Brisson, P. Brockill, A. F. Brooks, D. D. Brown, S. Brunett, C. C. Buchanan,
A. Buikema, T. Bulik, H. J. Bulten, A. Buonanno, D. Buskulic, C. Buy, R. L.
Byer, M. Cabero, L. Cadonati, G. Cagnoli, C. Cahillane, J. Calder'on
Bustillo, T. A. Callister, E. Calloni, J. B. Camp, M. Canepa, P. Canizares,
K. C. Cannon, H. Cao, J. Cao, C. D. Capano, 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, C. B. Cepeda, P.
Cerd'a-Dur'an, G. Cerretani, E. Cesarini, O. Chaibi, S. J. Chamberlin, M.
Chan, S. Chao, P. Charlton, E. Chase, E. Chassande-Mottin, D. Chatterjee, K.
Chatziioannou, B. D. Cheeseboro, H. Y. Chen, X. Chen, Y. Chen, H.-P. Cheng,
H. Y. Chia, A. Chincarini, A. Chiummo, T. Chmiel, H. S. Cho, M. Cho, J. H.
Chow, N. Christensen, Q. Chu, A. J. K. Chua, S. Chua, K. W. Chung, S. Chung,
G. Ciani, A. A. Ciobanu, R. Ciolfi, F. Cipriano, C. E. Cirelli, A. Cirone, F.
Clara, J. A. Clark, P. Clearwater, F. Cleva, C. Cocchieri, E. Coccia, P.-F.
Cohadon, D. Cohen, A. Colla, C. G. Collette, 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,
S. G. Crowder, T. J. Cullen, A. Cumming, L. Cunningham, E. Cuoco, T. Dal
Canton, G. D'alya, S. L. Danilishin, S. D'Antonio, K. Danzmann, A. Dasgupta,
C. F. Da Silva Costa, V. Dattilo, I. Dave, M. Davier, D. Davis, E. J. Daw, B.
Day, D. DeBra, M. Deenadayalan, J. Degallaix, M. De Laurentis, S. Del'eglise,
W. Del Pozzo, N. Demos, T. Denker, T. Dent, R. De Pietri, J. Derby, V.
Dergachev, 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,
V. Dolique, F. Donovan, K. L. Dooley, S. Doravari, I. Dorrington, M. Dovale
'Alvarez, T. P. Downes, M. Drago, C. Dreissigacker, J. C. Driggers, Z. Du, R.
Dudi, P. Dupej, S. E. Dwyer, P. J. Easter, T. B. Edo, M. C. Edwards, A.
Effler, H.-B. Eggenstein, P. Ehrens, J. Eichholz, S. S. Eikenberry, M.
Eisenmann, R. A. Eisenstein, 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, C. Fee, H. Fehrmann, J. Feicht, M. M. Fejer, F. Feng, A.
Fernandez-Galiana, I. Ferrante, E. C. Ferreira, F. Ferrini, F. Fidecaro, I.
Fiori, D. Fiorucci, M. Fishbach, R. P. Fisher, J. M. Fishner, M. Fitz-Axen,
R. Flaminio, M. Fletcher, H. Fong, J. A. Font, P. W. F. Forsyth, S. S.
Forsyth, J.-D. Fournier, S. Frasca, F. Frasconi, Z. Frei, A. Freise, R. Frey,
V. Frey, P. Fritschel, V. V. Frolov, 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. 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,
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, C. 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, X. Guo, A. Gupta, M. K. Gupta, K. E. Gushwa, E. K.
Gustafson, R. Gustafson, O. Halim, B. R. Hall, E. D. Hall, E. Z. Hamilton, H.
F. Hamilton, G. Hammond, M. Haney, M. M. Hanke, J. Hanks, C. Hanna, M. D.
Hannam, O. A. Hannuksela, J. Hanson, T. Hardwick, J. Harms, G. M. Harry, I.
W. Harry, M. J. Hart, C.-J. Haster, K. Haughian, J. Healy, A. Heidmann, M. C.
Heintze, H. Heitmann, P. Hello, G. Hemming, M. Hendry, I. S. Heng, J. Hennig,
A. W. Heptonstall, F. J. Hernandez, M. Heurs, S. Hild, T. Hinderer, D. Hoak,
S. Hochheim, D. Hofman, N. A. Holland, K. Holt, D. E. Holz, P. Hopkins, C.
Horst, J. Hough, E. A. Houston, E. J. Howell, A. Hreibi, E. A. Huerta, D.
Huet, B. Hughey, M. Hulko, S. Husa, S. H. Huttner, T. Huynh-Dinh, A. Iess, N.
Indik, C. Ingram, R. Inta, G. Intini, H. N. Isa, J.-M. Isac, M. Isi, B. R.
Iyer, K. Izumi, T. Jacqmin, K. Jani, P. Jaranowski, D. S. Johnson, W. W.
Johnson, D. I. Jones, R. Jones, R. J. G. Jonker, L. Ju, J. Junker, C. V.
Kalaghatgi, V. Kalogera, B. Kamai, S. Kandhasamy, G. Kang, J. B. Kanner, S.
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Lundgren, R. Lynch, Y. Ma, R. Macas, S. Macfoy, B. Machenschalk, M. MacInnis,
D. M. Macleod, I. Maga\~na Hernandez, F. Maga\~na-Sandoval, L. Maga\~na
Zertuche, R. M. Magee, E. Majorana, I. Maksimovic, N. Man, V. Mandic, V.
Mangano, G. L. Mansell, M. Manske, M. Mantovani, F. Marchesoni, F. Marion, S.
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T. McWilliams, D. Meacher, G. D. Meadors, M. Mehmet, J. Meidam, E.
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M. Mohan, S. R. P. Mohapatra, M. Montani, C. J. Moore, D. Moraru, G. Moreno,
S. Morisaki, B. Mours, C. M. Mow-Lowry, G. Mueller, A. W. Muir, Arunava
Mukherjee, D. Mukherjee, S. Mukherjee, N. Mukund, A. Mullavey, J. Munch, E.
A. Mu\~niz, M. Muratore, P. G. Murray, A. Nagar, K. Napier, I. Nardecchia, L.
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A. Neunzert, L. Nevin, J. M. Newport, K. Y. Ng, S. Ng, P. Nguyen, T. T.
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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
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Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, K. Venkateswara, G.
Venugopalan, D. Verkindt, F. Vetrano, A. Vicer'e, A. D. Viets, S.
Vinciguerra, D. J. Vine, J.-Y. Vinet, S. Vitale, T. Vo, H. Vocca, C. Vorvick,
S. P. Vyatchanin, A. R. Wade, L. E. Wade, M. Wade, R. Walet, M. Walker, L.
Wallace, S. Walsh, G. Wang, H. Wang, J. Z. Wang, W. H. Wang, Y. F. Wang, R.
L. Ward, J. Warner, M. Was, J. Watchi, B. Weaver, L.-W. Wei, M. Weinert, A.
J. Weinstein, R. Weiss, F. Wellmann, L. Wen, E. K. Wessel, P. Wessels, J.
Westerweck, K. Wette, J. T. Whelan, B. F. Whiting, C. Whittle, D. Wilken, D.
Williams, R. D. Williams, A. R. Williamson, J. L. Willis, B. Willke, M. H.
Wimmer, W. Winkler, C. C. Wipf, H. Wittel, G. Woan, J. Woehler, J. K.
Wofford, W. K. Wong, J. Worden, J. L. Wright, D. S. Wu, D. M. Wysocki, S.
Xiao, W. Yam, H. Yamamoto, C. C. Yancey, L. Yang, M. J. Yap, M. Yazback, Hang
Yu, Haocun Yu, M. Yvert, A. Zadro.zny, M. Zanolin, T. Zelenova, J.-P. Zendri,
M. Zevin, J. Zhang, L. Zhang, M. Zhang, T. Zhang, Y.-H. Zhang, C. Zhao, M.
Zhou, Z. Zhou, S. J. Zhu, X. J. Zhu, A. B. Zimmerman, Y. Zlochower, M. E.
Zucker, J. Zweizig | Properties of the binary neutron star merger GW170817 | 32 pages, 15 figures. Version 3 is the final published version;
results are unchanged compared to previous versions. Data behind the figures,
including posterior samples, are available at
dcc.ligo.org/LIGO-P1800061/public. The gravitational wave strain data for
this event are available at the LIGO Open Science Center,
gw-openscience.org/events/GW170817 | Phys. Rev. X 9, 011001 (2019) | 10.1103/PhysRevX.9.011001 | null | gr-qc astro-ph.HE | http://creativecommons.org/licenses/by/4.0/ | On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave
detectors observed a low-mass compact binary inspiral. The initial sky
localization of the source of the gravitational-wave signal, GW170817, allowed
electromagnetic observatories to identify NGC 4993 as the host galaxy. In this
work, we improve initial estimates of the binary's properties, including
component masses, spins, and tidal parameters, using the known source location,
improved modeling, and recalibrated Virgo data. We extend the range of
gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in
the initial analysis. We also compare results inferred using several signal
models, which are more accurate and incorporate additional physical effects as
compared to the initial analysis. We improve the localization of the
gravitational-wave source to a 90% credible region of $16~\mathrm{deg}^2$. We
find tighter constraints on the masses, spins, and tidal parameters, and
continue to find no evidence for nonzero component spins. The component masses
are inferred to lie between 1.00 and 1.89 $M_\odot$ when allowing for large
component spins, and to lie between 1.16 and 1.60 $M_\odot$ (with a total mass
$2.73^{+0.04}_{-0.01} \, M_\odot$) when the spins are restricted to be within
the range observed in Galactic binary neutron stars. Under minimal assumptions
about the nature of the compact objects, our constraints for the tidal
deformability parameter $\tilde \Lambda$ are $(0,630)$ when we allow for large
component spins, and $300^{+420}_{-230}$ (using a 90% highest posterior density
interval) when restricting the magnitude of the component spins, ruling out
several equation-of-state models at the 90% credible level. Finally, with LIGO
and GEO600 data, we use a Bayesian analysis to place upper limits on the
amplitude and spectral energy density of a possible post-merger signal.
(Abridged)
| [
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{
"created": "Mon, 15 Oct 2018 18:00:30 GMT",
"version": "v2"
},
{
"created": "Tue, 22 Jan 2019 19:56:03 GMT",
"version": "v3"
}
] | 2019-01-24 | [
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""
],
[
"Schale",
"P.",
""
],
[
"Scheel",
"M.",
""
],
[
"Scheuer",
"J.",
""
],
[
"Schmidt",
"P.",
""
],
[
"Schnabel",
"R.",
""
],
[
"Schofield",
"R. M. S.",
""
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[
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"A.",
""
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[
"Schreiber",
"E.",
""
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[
"Schuette",
"D.",
""
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[
"Schulte",
"B. W.",
""
],
[
"Schutz",
"B. F.",
""
],
[
"Schwalbe",
"S. G.",
""
],
[
"Scott",
"J.",
""
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[
"Scott",
"S. M.",
""
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[
"Seidel",
"E.",
""
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[
"Sellers",
"D.",
""
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[
"Sengupta",
"A. S.",
""
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[
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"D.",
""
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[
"Sequino",
"V.",
""
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[
"Sergeev",
"A.",
""
],
[
"Setyawati",
"Y.",
""
],
[
"Shaddock",
"D. A.",
""
],
[
"Shaffer",
"T. J.",
""
],
[
"Shah",
"A. A.",
""
],
[
"Shahriar",
"M. S.",
""
],
[
"Shaner",
"M. B.",
""
],
[
"Shao",
"L.",
""
],
[
"Shapiro",
"B.",
""
],
[
"Shawhan",
"P.",
""
],
[
"Shen",
"H.",
""
],
[
"Shoemaker",
"D. H.",
""
],
[
"Shoemaker",
"D. M.",
""
],
[
"Siellez",
"K.",
""
],
[
"Siemens",
"X.",
""
],
[
"Sieniawska",
"M.",
""
],
[
"Sigg",
"D.",
""
],
[
"Silva",
"A. D.",
""
],
[
"Singer",
"L. P.",
""
],
[
"Singh",
"A.",
""
],
[
"Singhal",
"A.",
""
],
[
"Sintes",
"A. M.",
""
],
[
"Slagmolen",
"B. J. J.",
""
],
[
"Slaven-Blair",
"T. J.",
""
],
[
"Smith",
"B.",
""
],
[
"Smith",
"J. R.",
""
],
[
"Smith",
"R. J. E.",
""
],
[
"Somala",
"S.",
""
],
[
"Son",
"E. J.",
""
],
[
"Sorazu",
"B.",
""
],
[
"Sorrentino",
"F.",
""
],
[
"Souradeep",
"T.",
""
],
[
"Spencer",
"A. P.",
""
],
[
"Srivastava",
"A. K.",
""
],
[
"Staats",
"K.",
""
],
[
"Steinke",
"M.",
""
],
[
"Steinlechner",
"J.",
""
],
[
"Steinlechner",
"S.",
""
],
[
"Steinmeyer",
"D.",
""
],
[
"Steltner",
"B.",
""
],
[
"Stevenson",
"S. P.",
""
],
[
"Stocks",
"D.",
""
],
[
"Stone",
"R.",
""
],
[
"Stops",
"D. J.",
""
],
[
"Strain",
"K. A.",
""
],
[
"Stratta",
"G.",
""
],
[
"Strigin",
"S. E.",
""
],
[
"Strunk",
"A.",
""
],
[
"Sturani",
"R.",
""
],
[
"Stuver",
"A. L.",
""
],
[
"Summerscales",
"T. Z.",
""
],
[
"Sun",
"L.",
""
],
[
"Sunil",
"S.",
""
],
[
"Suresh",
"J.",
""
],
[
"Sutton",
"P. J.",
""
],
[
"Swinkels",
"B. L.",
""
],
[
"Szczepa'nczyk",
"M. J.",
""
],
[
"Tacca",
"M.",
""
],
[
"Tait",
"S. C.",
""
],
[
"Talbot",
"C.",
""
],
[
"Talukder",
"D.",
""
],
[
"Tanner",
"D. B.",
""
],
[
"T'apai",
"M.",
""
],
[
"Taracchini",
"A.",
""
],
[
"Tasson",
"J. D.",
""
],
[
"Taylor",
"J. A.",
""
],
[
"Taylor",
"R.",
""
],
[
"Tewari",
"S. V.",
""
],
[
"Theeg",
"T.",
""
],
[
"Thies",
"F.",
""
],
[
"Thomas",
"E. G.",
""
],
[
"Thomas",
"M.",
""
],
[
"Thomas",
"P.",
""
],
[
"Thorne",
"K. A.",
""
],
[
"Thrane",
"E.",
""
],
[
"Tiwari",
"S.",
""
],
[
"Tiwari",
"V.",
""
],
[
"Tokmakov",
"K. V.",
""
],
[
"Toland",
"K.",
""
],
[
"Tonelli",
"M.",
""
],
[
"Tornasi",
"Z.",
""
],
[
"Torres-Forn'e",
"A.",
""
],
[
"Torrie",
"C. I.",
""
],
[
"T\"oyr\"a",
"D.",
""
],
[
"Travasso",
"F.",
""
],
[
"Traylor",
"G.",
""
],
[
"Trinastic",
"J.",
""
],
[
"Tringali",
"M. C.",
""
],
[
"Trozzo",
"L.",
""
],
[
"Tsang",
"K. W.",
""
],
[
"Tse",
"M.",
""
],
[
"Tso",
"R.",
""
],
[
"Tsuna",
"D.",
""
],
[
"Tsukada",
"L.",
""
],
[
"Tuyenbayev",
"D.",
""
],
[
"Ueno",
"K.",
""
],
[
"Ugolini",
"D.",
""
],
[
"Urban",
"A. L.",
""
],
[
"Usman",
"S. A.",
""
],
[
"Vahlbruch",
"H.",
""
],
[
"Vajente",
"G.",
""
],
[
"Valdes",
"G.",
""
],
[
"van Bakel",
"N.",
""
],
[
"van Beuzekom",
"M.",
""
],
[
"Brand",
"J. F. J. van den",
""
],
[
"Broeck",
"C. Van Den",
""
],
[
"Vander-Hyde",
"D. C.",
""
],
[
"van der Schaaf",
"L.",
""
],
[
"van Heijningen",
"J. V.",
""
],
[
"van Veggel",
"A. A.",
""
],
[
"Vardaro",
"M.",
""
],
[
"Varma",
"V.",
""
],
[
"Vass",
"S.",
""
],
[
"Vas'uth",
"M.",
""
],
[
"Vecchio",
"A.",
""
],
[
"Vedovato",
"G.",
""
],
[
"Veitch",
"J.",
""
],
[
"Veitch",
"P. J.",
""
],
[
"Venkateswara",
"K.",
""
],
[
"Venugopalan",
"G.",
""
],
[
"Verkindt",
"D.",
""
],
[
"Vetrano",
"F.",
""
],
[
"Vicer'e",
"A.",
""
],
[
"Viets",
"A. D.",
""
],
[
"Vinciguerra",
"S.",
""
],
[
"Vine",
"D. J.",
""
],
[
"Vinet",
"J. -Y.",
""
],
[
"Vitale",
"S.",
""
],
[
"Vo",
"T.",
""
],
[
"Vocca",
"H.",
""
],
[
"Vorvick",
"C.",
""
],
[
"Vyatchanin",
"S. P.",
""
],
[
"Wade",
"A. R.",
""
],
[
"Wade",
"L. E.",
""
],
[
"Wade",
"M.",
""
],
[
"Walet",
"R.",
""
],
[
"Walker",
"M.",
""
],
[
"Wallace",
"L.",
""
],
[
"Walsh",
"S.",
""
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[
"Wang",
"G.",
""
],
[
"Wang",
"H.",
""
],
[
"Wang",
"J. Z.",
""
],
[
"Wang",
"W. H.",
""
],
[
"Wang",
"Y. F.",
""
],
[
"Ward",
"R. L.",
""
],
[
"Warner",
"J.",
""
],
[
"Was",
"M.",
""
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[
"Watchi",
"J.",
""
],
[
"Weaver",
"B.",
""
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[
"Wei",
"L. -W.",
""
],
[
"Weinert",
"M.",
""
],
[
"Weinstein",
"A. J.",
""
],
[
"Weiss",
"R.",
""
],
[
"Wellmann",
"F.",
""
],
[
"Wen",
"L.",
""
],
[
"Wessel",
"E. K.",
""
],
[
"Wessels",
"P.",
""
],
[
"Westerweck",
"J.",
""
],
[
"Wette",
"K.",
""
],
[
"Whelan",
"J. T.",
""
],
[
"Whiting",
"B. F.",
""
],
[
"Whittle",
"C.",
""
],
[
"Wilken",
"D.",
""
],
[
"Williams",
"D.",
""
],
[
"Williams",
"R. D.",
""
],
[
"Williamson",
"A. R.",
""
],
[
"Willis",
"J. L.",
""
],
[
"Willke",
"B.",
""
],
[
"Wimmer",
"M. H.",
""
],
[
"Winkler",
"W.",
""
],
[
"Wipf",
"C. C.",
""
],
[
"Wittel",
"H.",
""
],
[
"Woan",
"G.",
""
],
[
"Woehler",
"J.",
""
],
[
"Wofford",
"J. K.",
""
],
[
"Wong",
"W. K.",
""
],
[
"Worden",
"J.",
""
],
[
"Wright",
"J. L.",
""
],
[
"Wu",
"D. S.",
""
],
[
"Wysocki",
"D. M.",
""
],
[
"Xiao",
"S.",
""
],
[
"Yam",
"W.",
""
],
[
"Yamamoto",
"H.",
""
],
[
"Yancey",
"C. C.",
""
],
[
"Yang",
"L.",
""
],
[
"Yap",
"M. J.",
""
],
[
"Yazback",
"M.",
""
],
[
"Yu",
"Hang",
""
],
[
"Yu",
"Haocun",
""
],
[
"Yvert",
"M.",
""
],
[
"zny",
"A. Zadro.",
""
],
[
"Zanolin",
"M.",
""
],
[
"Zelenova",
"T.",
""
],
[
"Zendri",
"J. -P.",
""
],
[
"Zevin",
"M.",
""
],
[
"Zhang",
"J.",
""
],
[
"Zhang",
"L.",
""
],
[
"Zhang",
"M.",
""
],
[
"Zhang",
"T.",
""
],
[
"Zhang",
"Y. -H.",
""
],
[
"Zhao",
"C.",
""
],
[
"Zhou",
"M.",
""
],
[
"Zhou",
"Z.",
""
],
[
"Zhu",
"S. J.",
""
],
[
"Zhu",
"X. J.",
""
],
[
"Zimmerman",
"A. B.",
""
],
[
"Zlochower",
"Y.",
""
],
[
"Zucker",
"M. E.",
""
],
[
"Zweizig",
"J.",
""
]
] | On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work, we improve initial estimates of the binary's properties, including component masses, spins, and tidal parameters, using the known source location, improved modeling, and recalibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as compared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of $16~\mathrm{deg}^2$. We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for nonzero component spins. The component masses are inferred to lie between 1.00 and 1.89 $M_\odot$ when allowing for large component spins, and to lie between 1.16 and 1.60 $M_\odot$ (with a total mass $2.73^{+0.04}_{-0.01} \, M_\odot$) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Under minimal assumptions about the nature of the compact objects, our constraints for the tidal deformability parameter $\tilde \Lambda$ are $(0,630)$ when we allow for large component spins, and $300^{+420}_{-230}$ (using a 90% highest posterior density interval) when restricting the magnitude of the component spins, ruling out several equation-of-state models at the 90% credible level. Finally, with LIGO and GEO600 data, we use a Bayesian analysis to place upper limits on the amplitude and spectral energy density of a possible post-merger signal. (Abridged) |
0810.1599 | J. Fernando Barbero G. | J. Fernando Barbero G., Eduardo J. S. Villase\~nor | On the computation of black hole entropy in loop quantum gravity | 25 pages | Class.Quant.Grav.26:035017,2009 | 10.1088/0264-9381/26/3/035017 | null | gr-qc math-ph math.CO math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We discuss some issues related to the computation of black hole entropy in
loop quantum gravity from the novel point of view provided by the recent
number-theoretical methods introduced by the authors and their collaborators.
In particular we give exact expressions, in the form of integral transforms,
for the black hole entropy in terms of the area. We do this by following
several approaches based both on our combinatorial techniques and also on
functional equations similar to those employed by Meissner in his pioneering
work on this subject. To put our results in perspective we compare them with
those of Meissner. We will show how our methods confirm some of his findings,
extend the validity of others, and correct some mistakes. At the end of the
paper we will discuss the delicate issue of the asymptotics of black hole
entropy.
| [
{
"created": "Thu, 9 Oct 2008 08:40:20 GMT",
"version": "v1"
}
] | 2010-05-19 | [
[
"G.",
"J. Fernando Barbero",
""
],
[
"Villaseñor",
"Eduardo J. S.",
""
]
] | We discuss some issues related to the computation of black hole entropy in loop quantum gravity from the novel point of view provided by the recent number-theoretical methods introduced by the authors and their collaborators. In particular we give exact expressions, in the form of integral transforms, for the black hole entropy in terms of the area. We do this by following several approaches based both on our combinatorial techniques and also on functional equations similar to those employed by Meissner in his pioneering work on this subject. To put our results in perspective we compare them with those of Meissner. We will show how our methods confirm some of his findings, extend the validity of others, and correct some mistakes. At the end of the paper we will discuss the delicate issue of the asymptotics of black hole entropy. |
1304.5675 | Ryuichi Fujita | Vijay Varma, Ryuichi Fujita, Ashok Choudhary and Bala R. Iyer | Comparison of post-Newtonian templates for extreme mass ratio inspirals | 10 pages | Phys. Rev. D 88, 024038 (2013) | 10.1103/PhysRevD.88.024038 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Extreme mass ratio inspirals (EMRIs), the inspirals of compact objects into
supermassive black holes, are important gravitational wave sources for the
Laser Interferometer Space Antenna (LISA). We study the performance of various
post-Newtonian (PN) template families relative to the high precision numerical
waveforms in the context of EMRI parameter estimation with LISA. Expressions
for the time domain waveforms TaylorT1, TaylorT2, TaylorT3, TaylorT4 and
TaylorEt are derived up to 22PN order, i.e $\mathcal{O}(v^{44})$ ($v$ is the
characteristic velocity of the binary) beyond the Newtonian term, for a test
particle in a circular orbit around a Schwarzschild black hole. The phase
difference between the above 22PN waveform families and numerical waveforms are
evaluated during two-year inspirals for two prototypical EMRI systems with mass
ratios $10^{-4}$ and $10^{-5}$. We find that the dephases (in radians) for
TaylorT1 and TaylorT2, respectively, are about $10^{-9}$ ($10^{-2}$) and
$10^{-9}$ ($10^{-3}$) for mass ratio $10^{-4}$ ($10^{-5}$). This suggests that
using 22PN TaylorT1 or TaylorT2 waveforms for parameter estimation of EMRIs
will result in accuracies comparable to numerical waveform accuracy for most of
the LISA parameter space. On the other hand, from the dephase results, we find
that TaylorT3, TaylorT4 and TaylorEt fare relatively poorly as one approaches
the last stable orbit. This implies that, as for comparable mass binaries using
the 3.5PN phase of waveforms, the 22PN TaylorT3 and TaylorEt approximants do
not perform well enough for the EMRIs. The reason underlying the poor
performance of TaylorT3, TaylorT4 and TaylorEt relative to TaylorT1 and
TaylorT2 is finally examined.
| [
{
"created": "Sat, 20 Apr 2013 23:04:47 GMT",
"version": "v1"
},
{
"created": "Tue, 30 Jul 2013 16:03:00 GMT",
"version": "v2"
}
] | 2013-07-31 | [
[
"Varma",
"Vijay",
""
],
[
"Fujita",
"Ryuichi",
""
],
[
"Choudhary",
"Ashok",
""
],
[
"Iyer",
"Bala R.",
""
]
] | Extreme mass ratio inspirals (EMRIs), the inspirals of compact objects into supermassive black holes, are important gravitational wave sources for the Laser Interferometer Space Antenna (LISA). We study the performance of various post-Newtonian (PN) template families relative to the high precision numerical waveforms in the context of EMRI parameter estimation with LISA. Expressions for the time domain waveforms TaylorT1, TaylorT2, TaylorT3, TaylorT4 and TaylorEt are derived up to 22PN order, i.e $\mathcal{O}(v^{44})$ ($v$ is the characteristic velocity of the binary) beyond the Newtonian term, for a test particle in a circular orbit around a Schwarzschild black hole. The phase difference between the above 22PN waveform families and numerical waveforms are evaluated during two-year inspirals for two prototypical EMRI systems with mass ratios $10^{-4}$ and $10^{-5}$. We find that the dephases (in radians) for TaylorT1 and TaylorT2, respectively, are about $10^{-9}$ ($10^{-2}$) and $10^{-9}$ ($10^{-3}$) for mass ratio $10^{-4}$ ($10^{-5}$). This suggests that using 22PN TaylorT1 or TaylorT2 waveforms for parameter estimation of EMRIs will result in accuracies comparable to numerical waveform accuracy for most of the LISA parameter space. On the other hand, from the dephase results, we find that TaylorT3, TaylorT4 and TaylorEt fare relatively poorly as one approaches the last stable orbit. This implies that, as for comparable mass binaries using the 3.5PN phase of waveforms, the 22PN TaylorT3 and TaylorEt approximants do not perform well enough for the EMRIs. The reason underlying the poor performance of TaylorT3, TaylorT4 and TaylorEt relative to TaylorT1 and TaylorT2 is finally examined. |
2010.00956 | Allan Alinea | Allan L. Alinea | On the Disformal Transformation of the Einstein-Hilbert Action | accepted for publication in Jordan Journal of Physics, 10 pages, one
figure, revisions: fixed typographical errors in some equations, updated one
reference | Jordan J. Phys. 16 (2024) no.5, 507 | 10.47011/16.5 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Disformal transformation is a generalisation of the well-known conformal
transformation commonly elaborated in mainstream graduate texts in gravity
(relativity) and modern cosmology. This transformation is one of the most
important mathematical operations in scalar tensor theories attempting to
address pressing problems involving dark energy and dark matter. With this
topic yet to penetrate these texts, we present a pedagogically oriented
derivation of the disformal transformation of the Einstein-Hilbert action.
Along the way of calculation, we encounter apparently problematic terms that
could be construed as leading to equations of motion that go beyond second
order in derivatives, signalling instability. We demonstrate that these terms
can be eliminated and absorbed through the definition of the Riemann curvature
tensor. The transformed Einstein-Hilbert action turns out to be a special case
of the Horndeski action and the equations of motion for the scalar field that
it describes are all up to second order only in derivatives, implying
stability.
| [
{
"created": "Thu, 1 Oct 2020 17:06:23 GMT",
"version": "v1"
},
{
"created": "Sun, 11 Oct 2020 17:43:01 GMT",
"version": "v2"
},
{
"created": "Sat, 9 Jul 2022 04:30:45 GMT",
"version": "v3"
}
] | 2024-01-23 | [
[
"Alinea",
"Allan L.",
""
]
] | Disformal transformation is a generalisation of the well-known conformal transformation commonly elaborated in mainstream graduate texts in gravity (relativity) and modern cosmology. This transformation is one of the most important mathematical operations in scalar tensor theories attempting to address pressing problems involving dark energy and dark matter. With this topic yet to penetrate these texts, we present a pedagogically oriented derivation of the disformal transformation of the Einstein-Hilbert action. Along the way of calculation, we encounter apparently problematic terms that could be construed as leading to equations of motion that go beyond second order in derivatives, signalling instability. We demonstrate that these terms can be eliminated and absorbed through the definition of the Riemann curvature tensor. The transformed Einstein-Hilbert action turns out to be a special case of the Horndeski action and the equations of motion for the scalar field that it describes are all up to second order only in derivatives, implying stability. |
gr-qc/0404106 | Giovanni Imponente | Giovanni Imponente and Giovanni Montani | Mixmaster Chaoticity as Semiclassical Limit of the Canonical Quantum
Dynamics | 9 pages, 1 figure | Int.J.Mod.Phys. D12 (2003) 977-984 | 10.1142/S0218271803003499 | null | gr-qc | null | Within a cosmological framework, we provide a Hamiltonian analysis of the
Mixmaster Universe dynamics on the base of a standard Arnowitt-Deser-Misner
approach, showing how the chaotic behavior characterizing the evolution of the
system near the cosmological singularity can be obtained as the semiclassical
limit of the canonical quantization of the model in the same dynamical
representation. The relation between this intrinsic chaotic behavior and the
indeterministic quantum dynamics is inferred through the coincidence between
the microcanonical probability distribution and the semiclassical quantum one.
| [
{
"created": "Mon, 26 Apr 2004 09:50:35 GMT",
"version": "v1"
}
] | 2009-11-10 | [
[
"Imponente",
"Giovanni",
""
],
[
"Montani",
"Giovanni",
""
]
] | Within a cosmological framework, we provide a Hamiltonian analysis of the Mixmaster Universe dynamics on the base of a standard Arnowitt-Deser-Misner approach, showing how the chaotic behavior characterizing the evolution of the system near the cosmological singularity can be obtained as the semiclassical limit of the canonical quantization of the model in the same dynamical representation. The relation between this intrinsic chaotic behavior and the indeterministic quantum dynamics is inferred through the coincidence between the microcanonical probability distribution and the semiclassical quantum one. |
2311.06021 | Sabrina D'Antonio | S. D'Antonio, C. Palomba, P. Astone, S. Dall'Osso, S. Dal Pra, S.
Frasca, P. Leaci, F. Muciaccia, O. J. Piccinni, L. Pierini, M. Serra | A semi-coherent generalization of the 5-vector method to search for
continuous gravitational waves | 16 pages, 12 figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The emission of continuous gravitational waves (CWs), with duration much
longer than the typical data taking runs, is expected from several sources,
notably spinning neutron stars, asymmetric with respect to their rotation axis
and more exotic sources, like ultra-light scalar boson clouds formed around
Kerr black holes and sub-solar mass primordial binary black holes. Unless the
signal time evolution is well predicted and its relevant parameters accurately
known, the search for CWs is typically based on semi-coherent methods, where
the full data set is divided in shorter chunks of given duration, which are
properly processed, and then incoherently combined. In this paper we present a
semi-coherent method, in which the so-called \textit{5-vector} statistics is
computed for the various data segments and then summed after the removal of the
Earth Doppler modulation and signal intrinsic spin-down. The method can work
with segment duration of several days, thanks to a double stage procedure in
which an initial rough correction of the Doppler and spin-down is followed by a
refined step in which the residual variations are removed. This method can be
efficiently applied for directed searches, where the source position is known
to a good level of accuracy, and in the candidate follow-up stage of
wide-parameter space searches.
| [
{
"created": "Fri, 10 Nov 2023 12:11:10 GMT",
"version": "v1"
}
] | 2023-11-13 | [
[
"D'Antonio",
"S.",
""
],
[
"Palomba",
"C.",
""
],
[
"Astone",
"P.",
""
],
[
"Dall'Osso",
"S.",
""
],
[
"Pra",
"S. Dal",
""
],
[
"Frasca",
"S.",
""
],
[
"Leaci",
"P.",
""
],
[
"Muciaccia",
"F.",
""
],
[
"Piccinni",
"O. J.",
""
],
[
"Pierini",
"L.",
""
],
[
"Serra",
"M.",
""
]
] | The emission of continuous gravitational waves (CWs), with duration much longer than the typical data taking runs, is expected from several sources, notably spinning neutron stars, asymmetric with respect to their rotation axis and more exotic sources, like ultra-light scalar boson clouds formed around Kerr black holes and sub-solar mass primordial binary black holes. Unless the signal time evolution is well predicted and its relevant parameters accurately known, the search for CWs is typically based on semi-coherent methods, where the full data set is divided in shorter chunks of given duration, which are properly processed, and then incoherently combined. In this paper we present a semi-coherent method, in which the so-called \textit{5-vector} statistics is computed for the various data segments and then summed after the removal of the Earth Doppler modulation and signal intrinsic spin-down. The method can work with segment duration of several days, thanks to a double stage procedure in which an initial rough correction of the Doppler and spin-down is followed by a refined step in which the residual variations are removed. This method can be efficiently applied for directed searches, where the source position is known to a good level of accuracy, and in the candidate follow-up stage of wide-parameter space searches. |
1812.04037 | Francisco Jos\'e Maldonado Torralba | \'Alvaro de la Cruz-Dombriz, Francisco Jos\'e Maldonado Torralba,
Anupam Mazumdar | Non-singular and ghost-free infinite derivative gravity with torsion | 5 pages, 1 figure. Minor changes, conclusions unchanged | Phys. Rev. D 99, 104021 (2019) | 10.1103/PhysRevD.99.104021 | null | gr-qc hep-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present the most general quadratic curvature action with torsion including
infinite covariant derivatives and study its implications around the Minkowski
background via the Palatini approach. Provided the torsion is solely given by
the background axial field, the metric and torsion are shown to decouple, and
both of them can be made ghost and singularity free for a fermionic source.
| [
{
"created": "Mon, 10 Dec 2018 19:23:22 GMT",
"version": "v1"
},
{
"created": "Thu, 17 Jan 2019 14:08:42 GMT",
"version": "v2"
}
] | 2019-05-22 | [
[
"de la Cruz-Dombriz",
"Álvaro",
""
],
[
"Torralba",
"Francisco José Maldonado",
""
],
[
"Mazumdar",
"Anupam",
""
]
] | We present the most general quadratic curvature action with torsion including infinite covariant derivatives and study its implications around the Minkowski background via the Palatini approach. Provided the torsion is solely given by the background axial field, the metric and torsion are shown to decouple, and both of them can be made ghost and singularity free for a fermionic source. |
gr-qc/0310058 | Christian Boehmer | Christian G. Boehmer | The Einstein static universe with torsion and the sign problem of the
cosmological constant | 8 pages, LaTeX; minor layout changes, typos corrected, one new
equation, new reference [5], completed reference [13], two references added | Class.Quant.Grav. 21 (2004) 1119-1124 | 10.1088/0264-9381/21/4/025 | TUW-03-31, Preprint ESI 1384 | gr-qc astro-ph hep-th | null | In the field equations of Einstein-Cartan theory with cosmological constant a
static spherically symmetric perfect fluid with spin density satisfying the
Weyssenhoff restriction is considered. This serves as a rough model of space
filled with (fermionic) dark matter. From this the Einstein static universe
with constant torsion is constructed, generalising the Einstein Cosmos to
Einstein-Cartan theory.
The interplay between torsion and the cosmological constant is discussed. A
possible way out of the cosmological constant's sign problem is suggested.
| [
{
"created": "Fri, 10 Oct 2003 16:14:57 GMT",
"version": "v1"
},
{
"created": "Sat, 11 Oct 2003 09:26:48 GMT",
"version": "v2"
},
{
"created": "Tue, 14 Oct 2003 10:46:54 GMT",
"version": "v3"
},
{
"created": "Fri, 23 Jan 2004 08:47:57 GMT",
"version": "v4"
},
{
"created": "Sat, 4 Feb 2006 18:47:04 GMT",
"version": "v5"
}
] | 2007-05-23 | [
[
"Boehmer",
"Christian G.",
""
]
] | In the field equations of Einstein-Cartan theory with cosmological constant a static spherically symmetric perfect fluid with spin density satisfying the Weyssenhoff restriction is considered. This serves as a rough model of space filled with (fermionic) dark matter. From this the Einstein static universe with constant torsion is constructed, generalising the Einstein Cosmos to Einstein-Cartan theory. The interplay between torsion and the cosmological constant is discussed. A possible way out of the cosmological constant's sign problem is suggested. |
1110.0686 | Lorenzo Sindoni | Lorenzo Sindoni | Emergent Models for Gravity: an Overview of Microscopic Models | null | SIGMA 8 (2012), 027, 45 pages | 10.3842/SIGMA.2012.027 | AEI-2011-68 | gr-qc hep-th | http://creativecommons.org/licenses/by-nc-sa/3.0/ | We give a critical overview of various attempts to describe gravity as an
emergent phenomenon, starting from examples of condensed matter physics, to
arrive to more sophisticated pregeometric models. The common line of thought is
to view the graviton as a composite particle/collective mode. However, we will
describe many different ways in which this idea is realized in practice.
| [
{
"created": "Tue, 4 Oct 2011 13:55:38 GMT",
"version": "v1"
},
{
"created": "Sat, 12 May 2012 06:16:46 GMT",
"version": "v2"
}
] | 2012-05-15 | [
[
"Sindoni",
"Lorenzo",
""
]
] | We give a critical overview of various attempts to describe gravity as an emergent phenomenon, starting from examples of condensed matter physics, to arrive to more sophisticated pregeometric models. The common line of thought is to view the graviton as a composite particle/collective mode. However, we will describe many different ways in which this idea is realized in practice. |
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