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 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
1403.1320 | Kiyoshi Shiraishi | Takuya Maki and Kiyoshi Shiraishi | Multi-black hole solutions in cosmological Einstein-Maxwell-dilaton
theory | 10 pages, no figure. a typo fixed | Classical and Quantum Gravity 10, No. 10, pp.2171-2178 (1993) | 10.1088/0264-9381/10/10/024 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Adopting a simple ansatz, we find exact solutions to the
Einstein-Maxwell-dilaton equations, which stand for the multi-black hole
configuration with maximal charge in a cosmological metric and dilaton field
background driven by a cosmological term.
| [
{
"created": "Thu, 6 Mar 2014 01:48:26 GMT",
"version": "v1"
},
{
"created": "Fri, 1 Mar 2019 07:06:19 GMT",
"version": "v2"
}
] | 2019-03-04 | [
[
"Maki",
"Takuya",
""
],
[
"Shiraishi",
"Kiyoshi",
""
]
] | Adopting a simple ansatz, we find exact solutions to the Einstein-Maxwell-dilaton equations, which stand for the multi-black hole configuration with maximal charge in a cosmological metric and dilaton field background driven by a cosmological term. |
0902.0292 | Jack Gegenberg | J. Gegenberg, G. Kunstatter | 2-D Midisuperspace Models for Quantum Black Holes | 16 pages; to appear in a World Scientific Review Volume | null | 10.1142/9789814277839_0013 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Dimensionally reduced spherically symmetric gravity and its generalization,
generic 2-D dilaton gravity, provide ideal theoretical laboratories for the
study of black hole quantum mechanics and thermodynamics. They are sufficiently
simple to be tractable but contain enough structure to allow the study of many
deep issues in quantum gravity, such as the endpoint of Hawking radiation and
the source of black hole entropy. This article reviews recent progress in a
particular geometrical approach to the study of quantum black holes in generic
2-d dilaton gravity.
| [
{
"created": "Mon, 2 Feb 2009 14:46:29 GMT",
"version": "v1"
}
] | 2016-12-21 | [
[
"Gegenberg",
"J.",
""
],
[
"Kunstatter",
"G.",
""
]
] | Dimensionally reduced spherically symmetric gravity and its generalization, generic 2-D dilaton gravity, provide ideal theoretical laboratories for the study of black hole quantum mechanics and thermodynamics. They are sufficiently simple to be tractable but contain enough structure to allow the study of many deep issues in quantum gravity, such as the endpoint of Hawking radiation and the source of black hole entropy. This article reviews recent progress in a particular geometrical approach to the study of quantum black holes in generic 2-d dilaton gravity. |
1211.4807 | Claudio Perini | Claudio Perini | Holonomy-flux spinfoam amplitude | 33 pages | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We introduce a holomorphic representation for the Lorentzian EPRL spinfoam on
arbitrary 2-complexes. The representation is obtained via the
Ashtekar-Lewandowski-Marolf-Mour\~ao-Thiemann heat kernel coherent state
transform. The new variables are classical holonomy-flux phase space variables
$(h,X)\simeq \mathcal T^*SU(2)$ of Hamiltonian loop quantum gravity prescribing
the holonomies of the Ashtekar connection $A=\Gamma + \gamma K$, and their
conjugate gravitational fluxes. For small heat kernel `time' the spinfoam
amplitude is peaked on classical space-time geometries, where at most countably
many curvatures are allowed for non-zero Barbero-Immirzi parameter. We briefly
comment on the possibility to use the alternative flipped classical limit.
| [
{
"created": "Tue, 20 Nov 2012 17:22:01 GMT",
"version": "v1"
}
] | 2012-11-21 | [
[
"Perini",
"Claudio",
""
]
] | We introduce a holomorphic representation for the Lorentzian EPRL spinfoam on arbitrary 2-complexes. The representation is obtained via the Ashtekar-Lewandowski-Marolf-Mour\~ao-Thiemann heat kernel coherent state transform. The new variables are classical holonomy-flux phase space variables $(h,X)\simeq \mathcal T^*SU(2)$ of Hamiltonian loop quantum gravity prescribing the holonomies of the Ashtekar connection $A=\Gamma + \gamma K$, and their conjugate gravitational fluxes. For small heat kernel `time' the spinfoam amplitude is peaked on classical space-time geometries, where at most countably many curvatures are allowed for non-zero Barbero-Immirzi parameter. We briefly comment on the possibility to use the alternative flipped classical limit. |
gr-qc/0606016 | Spiros Cotsakis | Spiros Cotsakis | Future Singularities and Completeness in Cosmology | 10 pages, latex. To appear in the Proceedings of the Thessaloniki
Meeting on Cosmology and Gravitational Physics, Thessaloniki, December 2005,
Greece | null | null | Samos-RG-MPC/060604-1 | gr-qc | null | We review recent work on the existence and nature of cosmological
singularities that can be formed during the evolution of generic as well as
specific cosmological spacetimes in general relativity. We first discuss
necessary and sufficient conditions for the existence of geodesically
incomplete spacetimes based on a tensorial analysis of the geodesic equations.
We then classify the possible singularities of isotropic globally hyperbolic
universes using the Bel-Robinson slice energy that closely monitors the
asymptotic properties of fields near the singularity. This classification
includes all known forms of spacetime singularities in isotropic universes and
also predicts new types.
| [
{
"created": "Sun, 4 Jun 2006 11:33:02 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Cotsakis",
"Spiros",
""
]
] | We review recent work on the existence and nature of cosmological singularities that can be formed during the evolution of generic as well as specific cosmological spacetimes in general relativity. We first discuss necessary and sufficient conditions for the existence of geodesically incomplete spacetimes based on a tensorial analysis of the geodesic equations. We then classify the possible singularities of isotropic globally hyperbolic universes using the Bel-Robinson slice energy that closely monitors the asymptotic properties of fields near the singularity. This classification includes all known forms of spacetime singularities in isotropic universes and also predicts new types. |
2002.05029 | Branislav Cvetkovi\'c | Milutin Blagojevi\'c and Branislav Cvetkovi\'c | Entropy in general relativity: Kerr-AdS black hole | LaTeX, 12 pages | Phys. Rev. D 101, 084023 (2020) | 10.1103/PhysRevD.101.084023 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A general Hamiltonian approach to black hole thermodynamics is used to study
entropy and conserved charges for Kerr-AdS solutions in general relativity.
These thermodynamic variables are first consistently defined by choosing
suitable boundary conditions, and then, they are shown to satisfy the first law
of black hole dynamics
| [
{
"created": "Wed, 12 Feb 2020 14:37:55 GMT",
"version": "v1"
}
] | 2020-04-15 | [
[
"Blagojević",
"Milutin",
""
],
[
"Cvetković",
"Branislav",
""
]
] | A general Hamiltonian approach to black hole thermodynamics is used to study entropy and conserved charges for Kerr-AdS solutions in general relativity. These thermodynamic variables are first consistently defined by choosing suitable boundary conditions, and then, they are shown to satisfy the first law of black hole dynamics |
2110.11378 | Pablo Antonio Cano Molina-Ni\~nirola | Pablo A. Cano, Kwinten Fransen, Thomas Hertog, Simon Maenaut | Gravitational ringing of rotating black holes in higher-derivative
gravity | 10 pages + appendices, 2 figures, double column. v2: references
added, version sent to the journal | null | 10.1103/PhysRevD.105.024064 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study gravitational perturbations of slowly-rotating black holes in a
general effective-field-theory extension of general relativity that includes up
to eight-derivative terms. We show that two Schr\"odinger-like equations with
spin-dependent effective potentials govern the odd - and even-parity master
variables. These equations are coupled for parity-violating corrections, and
this coupling affects the quasinormal modes even at linear order in the
higher-derivative corrections, due to their isospectrality in general
relativity. We provide results for the shifts in the fundamental quasinormal
mode frequencies at linear order in the spin, which we expect to be valuable
for high-precision phenomenology through future gravitational wave
observations.
| [
{
"created": "Thu, 21 Oct 2021 18:00:12 GMT",
"version": "v1"
},
{
"created": "Thu, 4 Nov 2021 09:14:21 GMT",
"version": "v2"
}
] | 2022-02-02 | [
[
"Cano",
"Pablo A.",
""
],
[
"Fransen",
"Kwinten",
""
],
[
"Hertog",
"Thomas",
""
],
[
"Maenaut",
"Simon",
""
]
] | We study gravitational perturbations of slowly-rotating black holes in a general effective-field-theory extension of general relativity that includes up to eight-derivative terms. We show that two Schr\"odinger-like equations with spin-dependent effective potentials govern the odd - and even-parity master variables. These equations are coupled for parity-violating corrections, and this coupling affects the quasinormal modes even at linear order in the higher-derivative corrections, due to their isospectrality in general relativity. We provide results for the shifts in the fundamental quasinormal mode frequencies at linear order in the spin, which we expect to be valuable for high-precision phenomenology through future gravitational wave observations. |
gr-qc/9610023 | Pedro. Silva | Ian G. Moss and Pedro J. Silva | BRST Invariant Boundary Conditions for Gauge Theories | 15 pages, RevTeX | Phys.Rev. D55 (1997) 1072-1078 | 10.1103/PhysRevD.55.1072 | NCL96-TP2 | gr-qc | null | A systematic way of generating sets of local boundary conditions on the gauge
fields in a path integral is presented. These boundary conditions are suitable
for one--loop effective action calculations on manifolds with boundary and for
quantum cosmology. For linearised gravity, the general proceedure described
here leads to new sets of boundary conditions.
| [
{
"created": "Mon, 14 Oct 1996 16:21:42 GMT",
"version": "v1"
}
] | 2009-10-28 | [
[
"Moss",
"Ian G.",
""
],
[
"Silva",
"Pedro J.",
""
]
] | A systematic way of generating sets of local boundary conditions on the gauge fields in a path integral is presented. These boundary conditions are suitable for one--loop effective action calculations on manifolds with boundary and for quantum cosmology. For linearised gravity, the general proceedure described here leads to new sets of boundary conditions. |
1304.5296 | Lior M. Burko | Lior M. Burko and Gaurav Khanna | Self-force gravitational waveforms for extreme and intermediate mass
ratio inspirals. II: Importance of the second-order dissipative effect | 8 pages, 10 figures, accepted to Phys. Rev. D. Version 2 includes
elaboration of the justification for the model used and for the gauge
invariance of our results, and correction of typos | Physical Review D 88 (2013), 024002 | 10.1103/PhysRevD.88.024002 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We consider the importance of the second-order dissipative self force for
gravitational wave dephasing for an extreme or intermediate mass ratio system
moving along a quasi-circular Schwarzschild orbit. For the first-order self
force we use the fully relativistic force in the Lorenz gauge for eternally
circular geodesics. The second-order self force is modeled by its 3.5 post
Newtonian counterpart. We evolve the system using the osculating orbits method,
and obtain the gravitational waveforms, whose phase includes all the terms -
within our approximation (and using the self force along circular geodesics) -
that are independent of the system's mass ratio. The partial dephasing due to
the second-order dissipative self force is substantially smaller than that of
the first-order conservative self force, although they are both at the same
order in the mass ratio.
| [
{
"created": "Fri, 19 Apr 2013 02:10:18 GMT",
"version": "v1"
},
{
"created": "Wed, 19 Jun 2013 21:36:17 GMT",
"version": "v2"
}
] | 2013-07-12 | [
[
"Burko",
"Lior M.",
""
],
[
"Khanna",
"Gaurav",
""
]
] | We consider the importance of the second-order dissipative self force for gravitational wave dephasing for an extreme or intermediate mass ratio system moving along a quasi-circular Schwarzschild orbit. For the first-order self force we use the fully relativistic force in the Lorenz gauge for eternally circular geodesics. The second-order self force is modeled by its 3.5 post Newtonian counterpart. We evolve the system using the osculating orbits method, and obtain the gravitational waveforms, whose phase includes all the terms - within our approximation (and using the self force along circular geodesics) - that are independent of the system's mass ratio. The partial dephasing due to the second-order dissipative self force is substantially smaller than that of the first-order conservative self force, although they are both at the same order in the mass ratio. |
gr-qc/9909009 | Heribert Genreith | H. Genreith | The Large Numbers Hypothesis: Outline of a self-similar
quantum-cosmological Model | Latex, 10 pages | null | null | null | gr-qc astro-ph | null | In 1919 A. Einstein suspected first that gravitational fields could play an
essential role in the structure of elementary particles. In 1937, P.A.M. Dirac
found a miraculous link between the properties of the visible Universe and
elementary particles. Both conjectures stayed alive through the following
decades but still no final theory could be derived to this issues. The herein
suggested fractal model of the Universe gives a consistent explanation to
Dirac's Large Numbers Hypothesis and combines the conjectures of Einstein and
Dirac.
| [
{
"created": "Thu, 2 Sep 1999 19:51:58 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Genreith",
"H.",
""
]
] | In 1919 A. Einstein suspected first that gravitational fields could play an essential role in the structure of elementary particles. In 1937, P.A.M. Dirac found a miraculous link between the properties of the visible Universe and elementary particles. Both conjectures stayed alive through the following decades but still no final theory could be derived to this issues. The herein suggested fractal model of the Universe gives a consistent explanation to Dirac's Large Numbers Hypothesis and combines the conjectures of Einstein and Dirac. |
1801.10374 | Mariano Cadoni | Mariano Cadoni, Roberto Casadio, Andrea Giusti, Matteo Tuveri | Emergence of a Dark Force in Corpuscular Gravity | 20 pages, no figures | Phys. Rev. D 97, 044047 (2018) | 10.1103/PhysRevD.97.044047 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We investigate the emergent laws of gravity when Dark Energy and the de
Sitter space-time are modelled as a critical Bose-Einstein condensate of a
large number of soft gravitons $N_{\rm G}$. We argue that this scenario
requires the presence of various regimes of gravity in which $N_{\rm G}$ scales
in different ways. Moreover, the local gravitational interaction affecting
baryonic matter can be naturally described in terms of gravitons pulled out
from this Dark Energy condensate (DEC). We then explain the additional
component of the acceleration at galactic scales, commonly attributed to dark
matter, as the reaction of the DEC to the presence of baryonic matter. This
additional dark force is also associated to gravitons pulled out from the DEC
and correctly reproduces the MOND acceleration. It also allows for an effective
description in terms of General Relativity sourced by an anisotropic fluid. We
finally calculate the mass ratio between the contribution of the apparent dark
matter and the baryonic matter in a region of size $r$ at galactic scales and
show that it is consistent with the $\Lambda$CDM predictions.
| [
{
"created": "Wed, 31 Jan 2018 09:40:37 GMT",
"version": "v1"
}
] | 2018-03-07 | [
[
"Cadoni",
"Mariano",
""
],
[
"Casadio",
"Roberto",
""
],
[
"Giusti",
"Andrea",
""
],
[
"Tuveri",
"Matteo",
""
]
] | We investigate the emergent laws of gravity when Dark Energy and the de Sitter space-time are modelled as a critical Bose-Einstein condensate of a large number of soft gravitons $N_{\rm G}$. We argue that this scenario requires the presence of various regimes of gravity in which $N_{\rm G}$ scales in different ways. Moreover, the local gravitational interaction affecting baryonic matter can be naturally described in terms of gravitons pulled out from this Dark Energy condensate (DEC). We then explain the additional component of the acceleration at galactic scales, commonly attributed to dark matter, as the reaction of the DEC to the presence of baryonic matter. This additional dark force is also associated to gravitons pulled out from the DEC and correctly reproduces the MOND acceleration. It also allows for an effective description in terms of General Relativity sourced by an anisotropic fluid. We finally calculate the mass ratio between the contribution of the apparent dark matter and the baryonic matter in a region of size $r$ at galactic scales and show that it is consistent with the $\Lambda$CDM predictions. |
1304.0209 | Yongge Ma | Yu Han, Yongge Ma, Xiangdong Zhang | Connection Dynamics for Higher Dimensional Scalar-Tensor Theories of
Gravity | 13 pages | Mod. Phys. Lett. A, Vol. 29, No. 28 (2014) 1450134 | 10.1142/S021773231450134X | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The scalar-tensor theories of gravity in spacetime dimensions $D+1>2$ are
studied. By doing Hamiltonian analysis, we obtain the geometrical dynamics of
the theories from their Lagrangian. The Hamiltonian formalism indicates that
the theories are naturally divided into two sectors by the coupling parameter
$\omega$. The Hamiltonian structure in both sectors are similar to the
corresponding structure of 4-dimensional cases. It turns out that there is a
symplectic reduction from the canonical structure of $so(D+1)$ Yang-Mills
theories coupled to the scalar field to the canonical structure of the
geometrical scalar-tensor theories. Therefore the non-perturbative loop quantum
gravity techniques can also be applied to the scalar-tensor theories in $D+1$
dimensions based on their connection-dynamical formalism.
| [
{
"created": "Sun, 31 Mar 2013 14:27:38 GMT",
"version": "v1"
},
{
"created": "Tue, 11 Feb 2014 16:53:00 GMT",
"version": "v2"
}
] | 2015-06-15 | [
[
"Han",
"Yu",
""
],
[
"Ma",
"Yongge",
""
],
[
"Zhang",
"Xiangdong",
""
]
] | The scalar-tensor theories of gravity in spacetime dimensions $D+1>2$ are studied. By doing Hamiltonian analysis, we obtain the geometrical dynamics of the theories from their Lagrangian. The Hamiltonian formalism indicates that the theories are naturally divided into two sectors by the coupling parameter $\omega$. The Hamiltonian structure in both sectors are similar to the corresponding structure of 4-dimensional cases. It turns out that there is a symplectic reduction from the canonical structure of $so(D+1)$ Yang-Mills theories coupled to the scalar field to the canonical structure of the geometrical scalar-tensor theories. Therefore the non-perturbative loop quantum gravity techniques can also be applied to the scalar-tensor theories in $D+1$ dimensions based on their connection-dynamical formalism. |
2112.12491 | Stephen Adler | Stephen L. Adler | A mechanism for a "leaky" black hole to catalyze galaxy formation | 6 pages | Int. J. Mod. Phys. D 31, 2242007 (2022) | 10.1142/S021827182242007X | null | gr-qc astro-ph.GA | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In the gravitational field of a Schwarzschild-like black hole, particles
infalling from rest at infinity, and black hole "wind" particles with
relativistic velocity leaking radially out from the nominal horizon, both have
the same magnitude of velocity at any radius from the hole. Hence when equally
massive infalling and wind particles collide at any radius, they yield
collision products with zero center of mass radial velocity, which can then
nucleate star formation at the collision radius. We suggest that this gives a
mechanism by which a central black hole can catalyze galaxy formation. For disk
galaxies, this mechanism explains the observed approximately exponential
falloff of the surface brightness with radius, and gives an estimate of the
associated scale length.
| [
{
"created": "Thu, 23 Dec 2021 12:32:28 GMT",
"version": "v1"
},
{
"created": "Mon, 27 Dec 2021 17:29:18 GMT",
"version": "v2"
},
{
"created": "Mon, 7 Mar 2022 13:40:35 GMT",
"version": "v3"
},
{
"created": "Tue, 8 Mar 2022 13:23:03 GMT",
"version": "v4"
},
{
"created": "Tue, 15 Mar 2022 21:43:17 GMT",
"version": "v5"
},
{
"created": "Sat, 19 Mar 2022 12:37:11 GMT",
"version": "v6"
}
] | 2023-01-03 | [
[
"Adler",
"Stephen L.",
""
]
] | In the gravitational field of a Schwarzschild-like black hole, particles infalling from rest at infinity, and black hole "wind" particles with relativistic velocity leaking radially out from the nominal horizon, both have the same magnitude of velocity at any radius from the hole. Hence when equally massive infalling and wind particles collide at any radius, they yield collision products with zero center of mass radial velocity, which can then nucleate star formation at the collision radius. We suggest that this gives a mechanism by which a central black hole can catalyze galaxy formation. For disk galaxies, this mechanism explains the observed approximately exponential falloff of the surface brightness with radius, and gives an estimate of the associated scale length. |
2111.05288 | Soichiro Isoyama | Soichiro Isoyama, Ryuichi Fujita, Alvin J. K. Chua, Hiroyuki Nakano,
Adam Pound, Norichika Sago | Adiabatic waveforms from extreme-mass-ratio inspirals: an analytical
approach | 9+5 pages,4+1 figures,5PN-e10 Teukolsky data are all available at the
Black Hole Perturbation Club: https://sites.google.com/view/bhpc1996/data
v2:updated references,expanded supplemental discussion of initial
phases.v3:contains minor corrections and more references.Matches version
published in PRL | Phys. Rev. Lett. 128, 231101 (2022) | 10.1103/PhysRevLett.128.231101 | YITP-21-114,KUNS-2901,OCU-PHYS-551,AP-GR-175 | gr-qc astro-ph.HE | http://creativecommons.org/licenses/by/4.0/ | Scientific analysis for the gravitational-wave detector LISA will require
theoretical waveforms from extreme-mass-ratio inspirals (EMRIs) that
extensively cover all possible orbital and spin configurations around
astrophysical Kerr black holes. However, on-the-fly calculations of these
waveforms have not yet overcome the high dimensionality of the parameter space.
To confront this challenge, we present a user-ready EMRI waveform model for
generic (eccentric and inclined) orbits in Kerr spacetime, using an analytical
self-force approach. Our model accurately covers all EMRIs with arbitrary
inclination and black hole spin, up to modest eccentricity ($\lesssim 0.3$) and
separation ($\gtrsim2$--$10M$ from the last stable orbit). In that regime, our
waveforms are accurate at the leading `adiabatic' order, and they approximately
capture transient self-force resonances that significantly impact the
gravitational-wave phase. The model fills an urgent need for extensive
waveforms in ongoing data-analysis studies, and its individual components will
continue to be useful in future science-adequate waveforms.
| [
{
"created": "Tue, 9 Nov 2021 17:36:48 GMT",
"version": "v1"
},
{
"created": "Wed, 24 Nov 2021 16:19:12 GMT",
"version": "v2"
},
{
"created": "Sun, 12 Jun 2022 09:16:56 GMT",
"version": "v3"
}
] | 2022-06-22 | [
[
"Isoyama",
"Soichiro",
""
],
[
"Fujita",
"Ryuichi",
""
],
[
"Chua",
"Alvin J. K.",
""
],
[
"Nakano",
"Hiroyuki",
""
],
[
"Pound",
"Adam",
""
],
[
"Sago",
"Norichika",
""
]
] | Scientific analysis for the gravitational-wave detector LISA will require theoretical waveforms from extreme-mass-ratio inspirals (EMRIs) that extensively cover all possible orbital and spin configurations around astrophysical Kerr black holes. However, on-the-fly calculations of these waveforms have not yet overcome the high dimensionality of the parameter space. To confront this challenge, we present a user-ready EMRI waveform model for generic (eccentric and inclined) orbits in Kerr spacetime, using an analytical self-force approach. Our model accurately covers all EMRIs with arbitrary inclination and black hole spin, up to modest eccentricity ($\lesssim 0.3$) and separation ($\gtrsim2$--$10M$ from the last stable orbit). In that regime, our waveforms are accurate at the leading `adiabatic' order, and they approximately capture transient self-force resonances that significantly impact the gravitational-wave phase. The model fills an urgent need for extensive waveforms in ongoing data-analysis studies, and its individual components will continue to be useful in future science-adequate waveforms. |
1612.09521 | Daniele Oriti | Daniele Oriti | The universe as a quantum gravity condensate | 20 pages; extended version of the invited contribution to the special
issue "Testing Quantum Gravity with Cosmology" of Comptes rendus Physique,
Acad\'emie des sciences, Paris, edited by A. Barrau | null | 10.1016/j.crhy.2017.02.003 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | This is an introduction to the approach to the extraction of cosmological
dynamics from full quantum gravity based on group field theory condensates. We
outline its general perspective, which sees cosmology as the hydrodynamics of
the fundamental quantum gravity degrees of freedom, as well as its concrete
implementation within the group field theory formalism. We summarise recent
work showing the emergence of a bouncing cosmological dynamics from a
fundamental group field theory model, and provide a brief but complete survey
of other results in the literature. Finally, we discuss open issues and
directions for further research.
| [
{
"created": "Fri, 30 Dec 2016 16:19:21 GMT",
"version": "v1"
}
] | 2017-04-25 | [
[
"Oriti",
"Daniele",
""
]
] | This is an introduction to the approach to the extraction of cosmological dynamics from full quantum gravity based on group field theory condensates. We outline its general perspective, which sees cosmology as the hydrodynamics of the fundamental quantum gravity degrees of freedom, as well as its concrete implementation within the group field theory formalism. We summarise recent work showing the emergence of a bouncing cosmological dynamics from a fundamental group field theory model, and provide a brief but complete survey of other results in the literature. Finally, we discuss open issues and directions for further research. |
1007.3973 | Jeffrey Kissel S | LIGO Scientific Collaboration: J. Abadie, B. P. Abbott, R. Abbott, M,
Abernathy, C. Adams, R. Adhikari, P. Ajith, B. Allen, G. Allen, E. Amador
Ceron, R. S. Amin, S. B. Anderson, W. G. Anderson, M. A. Arain, M. Araya, M.
Aronsson, Y. Aso, S. Aston, D. E. Atkinson, P. Aufmuth, C. Aulbert, S. Babak,
P. Baker, S. Ballmer, D. Barker, S. Barnum, B. Barr, P. Barriga, L. Barsotti,
M. A. Barton, I. Bartos, R. Bassiri, M. Bastarrika, J. Bauchrowitz, B.
Behnke, M. Benacquista, A. Bertolini, J. Betzwieser, N. Beveridge, P. T.
Beyersdorf, I. A. Bilenko, G. Billingsley, J. Birch, R. Biswas, E. Black, J.
K. Blackburn, L. Blackburn, D. Blair, B. Bland, O. Bock, T. P. Bodiya, R.
Bondarescu, R. Bork, M. Born, S. Bose, M. Boyle, P. R. Brady, V. B.
Braginsky, J. E. Brau, J. Breyer, D. O. Bridges, M. Brinkmann, M. Britzger,
A. F. Brooks, D. A. Brown, A. Buonanno, J. Burguet--Castell, O. Burmeister,
R. L. Byer, L. Cadonati, J. B. Camp, P. Campsie, J. Cannizzo, K. C. Cannon,
J. Cao, C. Capano, S. Caride, S. Caudill, M. Cavagli\`a, C. Cepeda, T.
Chalermsongsak, E. Chalkley, P. Charlton, S. Chelkowski, Y. Chen, N.
Christensen, S. S. Y. Chua, C. T. Y. Chung, D. Clark, J. Clark, J. H.
Clayton, R. Conte, D. Cook, T. R. Corbitt, N. Cornish, C. A. Costa, D.
Coward, D. C. Coyne, J. D. E. Creighton, T. D. Creighton, A. M. Cruise, R. M.
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Fehrmann, D. Feldbaum, L. S. Finn, M. Flanigan, K. Flasch, S. Foley, C.
Forrest, E. Forsi, N. Fotopoulos, M. Frede, M. Frei, Z. Frei, A. Freise, R.
Frey, T. T. Fricke, D. Friedrich, P. Fritschel, V. V. Frolov, P. Fulda, M.
Fyffe, J. A. Garofoli, I. Gholami, S. Ghosh, J. A. Giaime, S. Giampanis, K.
D. Giardina, C. Gill, E. Goetz, L. M. Goggin, G. Gonz\'alez, M. L.
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Huttner, T. Huynh--Dinh, D. R. Ingram, R. Inta, T. Isogai, A. Ivanov, W. W.
Johnson, D. I. Jones, G. Jones, R. Jones, L. Ju, P. Kalmus, V. Kalogera, S.
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M. Trias, K. Tseng, D. Ugolini, K. Urbanek, H. Vahlbruch, B. Vaishnav, M.
Vallisneri, C. Van Den Broeck, M. V. van der Sluys, A. A. van Veggel, S.
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C. Vorvick, S. P. Vyachanin, S. J. Waldman, L. Wallace, A. Wanner, R. L.
Ward, P. Wei, M. Weinert, A. J. Weinstein, R. Weiss, L. Wen, S. Wen, P.
Wessels, M. West, T. Westphal, K. Wette, J. T. Whelan, S. E. Whitcomb, D. J.
White, B. F. Whiting, C. Wilkinson, P. A. Willems, L. Williams, B. Willke, L.
Winkelmann, W. Winkler, C. C. Wipf, A. G. Wiseman, G. Woan, R. Wooley, J.
Worden, I. Yakushin, H. Yamamoto, K. Yamamoto, D. Yeaton-Massey, S. Yoshida,
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Zweizig | Calibration of the LIGO Gravitational Wave Detectors in the Fifth
Science Run | 49 pages, 23 figures | Nucl.Instrum.Meth.A624:223-240,2010 | 10.1016/j.nima.2010.07.089 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Laser Interferometer Gravitational Wave Observatory (LIGO) is a network
of three detectors built to detect local perturbations in the space-time metric
from astrophysical sources. These detectors, two in Hanford, WA and one in
Livingston, LA, are power-recycled Fabry-Perot Michelson interferometers. In
their fifth science run (S5), between November 2005 and October 2007, these
detectors accumulated one year of triple coincident data while operating at
their designed sensitivity. In this paper, we describe the calibration of the
instruments in the S5 data set, including measurement techniques and
uncertainty estimation.
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""
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"de la Jordana",
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""
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[
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[
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[
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"B. J. J.",
""
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"J.",
""
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[
"Smith",
"J. R.",
""
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[
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"M. R.",
""
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[
"Smith",
"N. D.",
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[
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"K.",
""
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[
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"B.",
""
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[
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"F. C.",
""
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[
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"A. J.",
""
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[
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[
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[
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"S. P.",
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[
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"P.",
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""
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[
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[
"Broeck",
"C. Van Den",
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"M. V.",
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"L.",
""
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[
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"B.",
""
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"L.",
""
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[
"Winkler",
"W.",
""
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[
"Wipf",
"C. C.",
""
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[
"Wiseman",
"A. G.",
""
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[
"Woan",
"G.",
""
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[
"Wooley",
"R.",
""
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[
"Worden",
"J.",
""
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[
"Yakushin",
"I.",
""
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[
"Yamamoto",
"H.",
""
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[
"Yamamoto",
"K.",
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[
"Yeaton-Massey",
"D.",
""
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[
"Yoshida",
"S.",
""
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[
"Yu",
"P. P.",
""
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[
"Zanolin",
"M.",
""
],
[
"Zhang",
"L.",
""
],
[
"Zhang",
"Z.",
""
],
[
"Zhao",
"C.",
""
],
[
"Zotov",
"N.",
""
],
[
"Zucker",
"M. E.",
""
],
[
"Zweizig",
"J.",
""
]
] | The Laser Interferometer Gravitational Wave Observatory (LIGO) is a network of three detectors built to detect local perturbations in the space-time metric from astrophysical sources. These detectors, two in Hanford, WA and one in Livingston, LA, are power-recycled Fabry-Perot Michelson interferometers. In their fifth science run (S5), between November 2005 and October 2007, these detectors accumulated one year of triple coincident data while operating at their designed sensitivity. In this paper, we describe the calibration of the instruments in the S5 data set, including measurement techniques and uncertainty estimation. |
gr-qc/0608096 | Michel Leclerc | M. Leclerc | Noether's theorem, the stress-energy tensor and Hamiltonian constraints | references updated | null | null | null | gr-qc | null | Noether's theorem is reviewed with a particular focus on an intermediate step
between global and local gauge and coordinate transformations, namely linear
transformations. We rederive the well known result that global symmetry leads
to charge conservation (Noether's first theorem), and show that linear symmetry
allows for the current to be expressed as a four divergence. Local symmetry
leads to identical conservation of the current and allows for the expression of
the charge as two dimensional surface integral (Noether's second theorem). In
the context of coordinate transformations, an additional step (Poincare
symmetry) is of physical interest and leads to the definition of the symmetric
Belinfante stress-energy tensor, which is then shown to be identically zero in
generally covariant first order theories. The intermediate step of linear
symmetry turns out to be important in general relativity when the customary
first order Lagrangian is used, which is covariant only under affine
transformations. In addition, we derive explicitely the canonical stress-energy
tensor in second order theories in its identically conserved form. Finally, we
analyze the relations between the generators of local transformations, the
corresponding currents and the Hamiltonian constraints.
| [
{
"created": "Sun, 20 Aug 2006 10:36:27 GMT",
"version": "v1"
},
{
"created": "Wed, 23 Aug 2006 13:32:33 GMT",
"version": "v2"
},
{
"created": "Sun, 10 Sep 2006 16:31:04 GMT",
"version": "v3"
},
{
"created": "Tue, 12 Sep 2006 16:19:54 GMT",
"version": "v4"
}
] | 2007-05-23 | [
[
"Leclerc",
"M.",
""
]
] | Noether's theorem is reviewed with a particular focus on an intermediate step between global and local gauge and coordinate transformations, namely linear transformations. We rederive the well known result that global symmetry leads to charge conservation (Noether's first theorem), and show that linear symmetry allows for the current to be expressed as a four divergence. Local symmetry leads to identical conservation of the current and allows for the expression of the charge as two dimensional surface integral (Noether's second theorem). In the context of coordinate transformations, an additional step (Poincare symmetry) is of physical interest and leads to the definition of the symmetric Belinfante stress-energy tensor, which is then shown to be identically zero in generally covariant first order theories. The intermediate step of linear symmetry turns out to be important in general relativity when the customary first order Lagrangian is used, which is covariant only under affine transformations. In addition, we derive explicitely the canonical stress-energy tensor in second order theories in its identically conserved form. Finally, we analyze the relations between the generators of local transformations, the corresponding currents and the Hamiltonian constraints. |
gr-qc/0609007 | Michael Pfenning | Christopher J. Fewster, Ken D. Olum, Michael J. Pfenning | Averaged null energy condition in spacetimes with boundaries | 12 pages, 1 figure, revTex4 with pstricks figure. Revised to address
concerns of referee. Two theorems added to summarize results. v3: add grant
acknowledgment | Phys.Rev.D75:025007,2007 | 10.1103/PhysRevD.75.025007 | null | gr-qc math-ph math.MP | null | The Averaged Null Energy Condition (ANEC) requires that the average along a
complete null geodesic of the projection of the stress-energy tensor onto the
geodesic tangent vector can never be negative. It is sufficient to rule out
many exotic phenomena in general relativity. Subject to certain conditions, we
show that the ANEC can never be violated by a quantized minimally coupled free
scalar field along a complete null geodesic surrounded by a tubular
neighborhood in which the geometry is flat and whose intrinsic causal structure
coincides with that induced from the full spacetime. In particular, the ANEC
holds in flat space with boundaries, as in the Casimir effect, for geodesics
which stay a finite distance away from the boundary
| [
{
"created": "Fri, 1 Sep 2006 15:52:23 GMT",
"version": "v1"
},
{
"created": "Mon, 11 Dec 2006 18:45:21 GMT",
"version": "v2"
},
{
"created": "Mon, 10 Sep 2007 19:29:46 GMT",
"version": "v3"
}
] | 2008-11-26 | [
[
"Fewster",
"Christopher J.",
""
],
[
"Olum",
"Ken D.",
""
],
[
"Pfenning",
"Michael J.",
""
]
] | The Averaged Null Energy Condition (ANEC) requires that the average along a complete null geodesic of the projection of the stress-energy tensor onto the geodesic tangent vector can never be negative. It is sufficient to rule out many exotic phenomena in general relativity. Subject to certain conditions, we show that the ANEC can never be violated by a quantized minimally coupled free scalar field along a complete null geodesic surrounded by a tubular neighborhood in which the geometry is flat and whose intrinsic causal structure coincides with that induced from the full spacetime. In particular, the ANEC holds in flat space with boundaries, as in the Casimir effect, for geodesics which stay a finite distance away from the boundary |
gr-qc/0407018 | Martin Bojowald | Martin Bojowald and Rafal Swiderski | The Volume Operator in Spherically Symmetric Quantum Geometry | 25 pages, 2 figures | Class.Quant.Grav. 21 (2004) 4881-4900 | 10.1088/0264-9381/21/21/009 | AEI-2004-049 | gr-qc | null | The spherically symmetric volume operator is discussed and all its
eigenstates and eigenvalues are computed. Even though the operator is more
complicated than its homogeneous analog, the spectra are related in the sense
that the larger spherically symmetric volume spectrum adds fine structure to
the homogeneous spectrum. The formulas of this paper complete the derivation of
an explicit calculus for spherically symmetric models which is needed for
future physical investigations.
| [
{
"created": "Mon, 5 Jul 2004 13:38:02 GMT",
"version": "v1"
},
{
"created": "Thu, 8 Jul 2004 14:19:00 GMT",
"version": "v2"
}
] | 2007-05-23 | [
[
"Bojowald",
"Martin",
""
],
[
"Swiderski",
"Rafal",
""
]
] | The spherically symmetric volume operator is discussed and all its eigenstates and eigenvalues are computed. Even though the operator is more complicated than its homogeneous analog, the spectra are related in the sense that the larger spherically symmetric volume spectrum adds fine structure to the homogeneous spectrum. The formulas of this paper complete the derivation of an explicit calculus for spherically symmetric models which is needed for future physical investigations. |
2211.01766 | Hector O. Silva | Daniela D. Doneva, Fethi M. Ramazano\u{g}lu, Hector O. Silva, Thomas
P. Sotiriou, Stoytcho S. Yazadjiev | Scalarization | 50 pages, 24 figures. Review commissioned by Reviews of Modern
Physics, submitted version, comments welcome | null | null | null | gr-qc astro-ph.HE hep-th | http://creativecommons.org/licenses/by/4.0/ | Scalarization is a mechanism that endows strongly self-gravitating bodies,
such as neutron stars and black holes, with a scalar field configuration. It
resembles a phase transition in that the scalar configuration only appears when
a certain quantity that characterizes the compact object, e.g., its compactness
or spin, is beyond a threshold. We provide a critical and comprehensive review
of scalarization, including the mechanism itself, theories that exhibit it, its
manifestation in neutron stars, black holes, and their binaries, potential
extension to other fields, and a thorough discussion of future perspectives.
| [
{
"created": "Thu, 3 Nov 2022 12:45:58 GMT",
"version": "v1"
}
] | 2022-11-04 | [
[
"Doneva",
"Daniela D.",
""
],
[
"Ramazanoğlu",
"Fethi M.",
""
],
[
"Silva",
"Hector O.",
""
],
[
"Sotiriou",
"Thomas P.",
""
],
[
"Yazadjiev",
"Stoytcho S.",
""
]
] | Scalarization is a mechanism that endows strongly self-gravitating bodies, such as neutron stars and black holes, with a scalar field configuration. It resembles a phase transition in that the scalar configuration only appears when a certain quantity that characterizes the compact object, e.g., its compactness or spin, is beyond a threshold. We provide a critical and comprehensive review of scalarization, including the mechanism itself, theories that exhibit it, its manifestation in neutron stars, black holes, and their binaries, potential extension to other fields, and a thorough discussion of future perspectives. |
0811.3481 | Babak Vakili | Babak Vakili | Cosmology with minimal length uncertainty relations | 11 pages, 4 figures, to appear in IJMPD | Int.J.Mod.Phys.D18:1059-1071,2009 | 10.1142/S0218271809014935 | null | gr-qc astro-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the effects of the existence of a minimal observable length in the
phase space of classical and quantum de Sitter (dS) and Anti de Sitter (AdS)
cosmology. Since this length has been suggested in quantum gravity and string
theory, its effects in the early universe might be expected. Adopting the
existence of such a minimum length results in the Generalized Uncertainty
Principle (GUP), which is a deformed Heisenberg algebra between minisuperspace
variables and their momenta operators. We extend these deformed commutating
relations to the corresponding deformed Poisson algebra in the classical limit.
Using the resulting Poisson and Heisenberg relations, we then construct the
classical and quantum cosmology of dS and Ads models in a canonical framework.
We show that in classical dS cosmology this effect yields an inflationary
universe in which the rate of expansion is larger than the usual dS universe.
Also, for the AdS model it is shown that GUP might change the oscillatory
nature of the corresponding cosmology. We also study the effects of GUP in
quantized models through approximate analytical solutions of the Wheeler-DeWitt
(WD) equation, in the limit of small scale factor for the universe, and compare
the results with the ordinary quantum cosmology in each case.
| [
{
"created": "Fri, 21 Nov 2008 07:09:55 GMT",
"version": "v1"
}
] | 2009-08-25 | [
[
"Vakili",
"Babak",
""
]
] | We study the effects of the existence of a minimal observable length in the phase space of classical and quantum de Sitter (dS) and Anti de Sitter (AdS) cosmology. Since this length has been suggested in quantum gravity and string theory, its effects in the early universe might be expected. Adopting the existence of such a minimum length results in the Generalized Uncertainty Principle (GUP), which is a deformed Heisenberg algebra between minisuperspace variables and their momenta operators. We extend these deformed commutating relations to the corresponding deformed Poisson algebra in the classical limit. Using the resulting Poisson and Heisenberg relations, we then construct the classical and quantum cosmology of dS and Ads models in a canonical framework. We show that in classical dS cosmology this effect yields an inflationary universe in which the rate of expansion is larger than the usual dS universe. Also, for the AdS model it is shown that GUP might change the oscillatory nature of the corresponding cosmology. We also study the effects of GUP in quantized models through approximate analytical solutions of the Wheeler-DeWitt (WD) equation, in the limit of small scale factor for the universe, and compare the results with the ordinary quantum cosmology in each case. |
0804.3848 | Farook Rahaman | F.Rahaman, M.Kalam and K. A. Rahman | Can electro-magnetic field, anisotropic source and varying $\Lambda$ be
sufficient to produce wormhole spacetime ? | Some changes have been made | Int.J.Theor.Phys.48:1637-1648,2009 | 10.1007/s10773-009-9936-x | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | It is well known that solutions of general relativity which allow for
traversable wormholes require the existence of exotic matter (matter that
violates weak or null energy conditions [WEC or NEC]). In this article, we
provide a class of exact solution for Einstein-Maxwell field equations
describing wormholes assuming the erstwhile cosmological term $\Lambda$ to be
space variable, viz., $\Lambda = \Lambda (r)$.
The source considered here not only a matter entirely but a sum of matters
i.e. anisotropic matter distribution, electromagnetic field and cosmological
constant whose effective parts obey all energy conditions out side the wormhole
throat. Here violation of energy conditions can be compensated by varying
cosmological constant. The important feature of this article is that one can
get wormhole structure, at least theoretically, comprising with physically
acceptable matters.
| [
{
"created": "Thu, 24 Apr 2008 06:39:11 GMT",
"version": "v1"
},
{
"created": "Mon, 10 Nov 2008 11:30:54 GMT",
"version": "v2"
},
{
"created": "Mon, 17 Nov 2008 10:23:07 GMT",
"version": "v3"
}
] | 2009-05-29 | [
[
"Rahaman",
"F.",
""
],
[
"Kalam",
"M.",
""
],
[
"Rahman",
"K. A.",
""
]
] | It is well known that solutions of general relativity which allow for traversable wormholes require the existence of exotic matter (matter that violates weak or null energy conditions [WEC or NEC]). In this article, we provide a class of exact solution for Einstein-Maxwell field equations describing wormholes assuming the erstwhile cosmological term $\Lambda$ to be space variable, viz., $\Lambda = \Lambda (r)$. The source considered here not only a matter entirely but a sum of matters i.e. anisotropic matter distribution, electromagnetic field and cosmological constant whose effective parts obey all energy conditions out side the wormhole throat. Here violation of energy conditions can be compensated by varying cosmological constant. The important feature of this article is that one can get wormhole structure, at least theoretically, comprising with physically acceptable matters. |
0804.3892 | Chao-Guang Huang | Zhe Chang, Cheng-Bo Guan, Chao-Guang Huang, and Xin Li | Gravitational collapse without a remnant | 9 pages, 9 figures, to appear in Int. J. Theor. Phys | Int.J.Theor.Phys.47:2479-2491,2008 | 10.1007/s10773-008-9681-6 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We investigate the gravitational collapse of a spherically symmetric,
inhomogeneous star, which is described by a perfect fluid with heat flow and
satisfies the equation of state $p=\rho/3$ or $p=C\rho^\ga$ at its center.
Different from the ordinary process of gravitational collapsing, the energy of
the whole star is emitted into space. And the remaining spacetime is a
Minkowski one at the end of the process.
| [
{
"created": "Thu, 24 Apr 2008 10:47:05 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Chang",
"Zhe",
""
],
[
"Guan",
"Cheng-Bo",
""
],
[
"Huang",
"Chao-Guang",
""
],
[
"Li",
"Xin",
""
]
] | We investigate the gravitational collapse of a spherically symmetric, inhomogeneous star, which is described by a perfect fluid with heat flow and satisfies the equation of state $p=\rho/3$ or $p=C\rho^\ga$ at its center. Different from the ordinary process of gravitational collapsing, the energy of the whole star is emitted into space. And the remaining spacetime is a Minkowski one at the end of the process. |
gr-qc/9303011 | Philip Tuckey | Philip Tuckey | The Construction of Sorkin Triangulations | 5 pages (plus one figure not included, available from author on
request), Plain Tex, no local preprint number (Only change: omitted
"\magnification" command now replaced) | Class.Quant.Grav.10:L109-L113,1993 | 10.1088/0264-9381/10/8/004 | null | gr-qc | null | Some time ago, Sorkin (1975) reported investigations of the time evolution
and initial value problems in Regge calculus, for one triangulation each of the
manifolds $R*S^3$ and $R^4$. Here we display the simple, local characteristic
of those triangulations which underlies the structure found by Sorkin, and
emphasise its general applicability, and therefore the general validity of
Sorkin's conclusions. We also make some elementary observations on the
resulting structure of the time evolution and initial value problems in Regge
calculus, and add some comments and speculations.
| [
{
"created": "Fri, 5 Mar 1993 17:01:24 GMT",
"version": "v1"
},
{
"created": "Mon, 8 Mar 1993 12:55:32 GMT",
"version": "v2"
}
] | 2010-04-06 | [
[
"Tuckey",
"Philip",
""
]
] | Some time ago, Sorkin (1975) reported investigations of the time evolution and initial value problems in Regge calculus, for one triangulation each of the manifolds $R*S^3$ and $R^4$. Here we display the simple, local characteristic of those triangulations which underlies the structure found by Sorkin, and emphasise its general applicability, and therefore the general validity of Sorkin's conclusions. We also make some elementary observations on the resulting structure of the time evolution and initial value problems in Regge calculus, and add some comments and speculations. |
0812.1286 | Abraao Capistrano | A. J. S. Capistrano, P.I. Odon | The Dark Universe Riddle | 39 pages, corrected typos, additional references, no figures | Apeiron (Montreal), v. 16, p. 229-304, 2009 | null | null | gr-qc astro-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work we review some of the theoretical efforts and experimental
evidences related to Dark matter and Dark energy problems in the universe.
These dilemmas show us how incomplete our knowledge of gravity is, and how our
concepts about the universe must at least be revised. Mainly, on the Wilkinson
Microwave Anisotropy Probe (WMAP) fifth year, the data indicates that more than
90% of the total energy density of the universe is dark. Here we discuss the
impact of these phenomena imprint on gravitational and quantum field theory's
standard history. Moreover, we point out some recent and upcoming projects on
Cosmology intended to shed light on these problems.
| [
{
"created": "Sat, 6 Dec 2008 13:24:53 GMT",
"version": "v1"
},
{
"created": "Thu, 16 Apr 2009 00:27:22 GMT",
"version": "v2"
}
] | 2016-05-25 | [
[
"Capistrano",
"A. J. S.",
""
],
[
"Odon",
"P. I.",
""
]
] | In this work we review some of the theoretical efforts and experimental evidences related to Dark matter and Dark energy problems in the universe. These dilemmas show us how incomplete our knowledge of gravity is, and how our concepts about the universe must at least be revised. Mainly, on the Wilkinson Microwave Anisotropy Probe (WMAP) fifth year, the data indicates that more than 90% of the total energy density of the universe is dark. Here we discuss the impact of these phenomena imprint on gravitational and quantum field theory's standard history. Moreover, we point out some recent and upcoming projects on Cosmology intended to shed light on these problems. |
1508.04614 | Edward Glass | J.P. Krisch and E.N. Glass | Generalized Inheritance | null | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Generalized inheritance is used with the almost-conformal Killing equation.
Examples are the flat FRW, Kasner, and deSitter metrics. The volume changes in
FRW while transitioning to a stiff fluid are discussed. An inheritance current
is implicit in the generalized condition
| [
{
"created": "Wed, 19 Aug 2015 12:32:45 GMT",
"version": "v1"
}
] | 2015-08-20 | [
[
"Krisch",
"J. P.",
""
],
[
"Glass",
"E. N.",
""
]
] | Generalized inheritance is used with the almost-conformal Killing equation. Examples are the flat FRW, Kasner, and deSitter metrics. The volume changes in FRW while transitioning to a stiff fluid are discussed. An inheritance current is implicit in the generalized condition |
2103.07408 | Shunichiro Kinoshita | Shunichiro Kinoshita | Extension of Kodama vector and quasilocal quantities in
three-dimensional axisymmetric spacetimes | 5 pages; v2: minor changes, reference added; v3: published in PRD | Phys. Rev. D 103, 124042 (2021) | 10.1103/PhysRevD.103.124042 | null | gr-qc hep-th | http://creativecommons.org/licenses/by/4.0/ | Spherically symmetric spacetimes admit the so-called Kodama vector, which
provides a locally conserved current and a preferred time even for dynamical
spacetime without any time translation symmetry. A charge associated with this
conserved current leads to a quasilocal mass which agrees with the Misner-Sharp
mass. In three dimensions, spherically symmetric spacetimes correspond to
axisymmetric ones, while axisymmetry allows spacetimes to be rotating with
angular momentum. We extend the notion of the Kodama vector to axisymmetric
rotating spacetimes in three dimensions. We also define a quasilocal mass
taking into account angular momentum in three-dimensional axisymmetric
spacetimes.
| [
{
"created": "Fri, 12 Mar 2021 17:09:55 GMT",
"version": "v1"
},
{
"created": "Thu, 25 Mar 2021 11:39:42 GMT",
"version": "v2"
},
{
"created": "Fri, 16 Sep 2022 07:25:16 GMT",
"version": "v3"
}
] | 2022-09-19 | [
[
"Kinoshita",
"Shunichiro",
""
]
] | Spherically symmetric spacetimes admit the so-called Kodama vector, which provides a locally conserved current and a preferred time even for dynamical spacetime without any time translation symmetry. A charge associated with this conserved current leads to a quasilocal mass which agrees with the Misner-Sharp mass. In three dimensions, spherically symmetric spacetimes correspond to axisymmetric ones, while axisymmetry allows spacetimes to be rotating with angular momentum. We extend the notion of the Kodama vector to axisymmetric rotating spacetimes in three dimensions. We also define a quasilocal mass taking into account angular momentum in three-dimensional axisymmetric spacetimes. |
1206.3496 | Marcus Berg | Marcus Berg, Igor Buchberger, Jonas Enander, Edvard Mortsell, Stefan
Sjors | Growth Histories in Bimetric Massive Gravity | 28 pages + appendix, 11 figures | null | 10.1088/1475-7516/2012/12/021 | null | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We perform cosmological perturbation theory in Hassan-Rosen bimetric gravity
for general homogeneous and isotropic backgrounds. In the de Sitter
approximation, we obtain decoupled sets of massless and massive scalar
gravitational fluctuations. Matter perturbations then evolve like in Einstein
gravity. We perturb the future de Sitter regime by the ratio of matter to dark
energy, producing quasi-de Sitter space. In this more general setting the
massive and massless fluctuations mix. We argue that in the quasi-de Sitter
regime, the growth of structure in bimetric gravity differs from that of
Einstein gravity.
| [
{
"created": "Fri, 15 Jun 2012 15:09:13 GMT",
"version": "v1"
}
] | 2015-06-05 | [
[
"Berg",
"Marcus",
""
],
[
"Buchberger",
"Igor",
""
],
[
"Enander",
"Jonas",
""
],
[
"Mortsell",
"Edvard",
""
],
[
"Sjors",
"Stefan",
""
]
] | We perform cosmological perturbation theory in Hassan-Rosen bimetric gravity for general homogeneous and isotropic backgrounds. In the de Sitter approximation, we obtain decoupled sets of massless and massive scalar gravitational fluctuations. Matter perturbations then evolve like in Einstein gravity. We perturb the future de Sitter regime by the ratio of matter to dark energy, producing quasi-de Sitter space. In this more general setting the massive and massless fluctuations mix. We argue that in the quasi-de Sitter regime, the growth of structure in bimetric gravity differs from that of Einstein gravity. |
gr-qc/0307013 | Mihalis Dafermos | Mihalis Dafermos | The interior of charged black holes and the problem of uniqueness in
general relativity | 61 pages, 16 figures, revised version, minor corrections | Comm. Pure Appl. Math. 58 (2005), 0445--0504 | null | null | gr-qc math.AP | null | We consider a spherically symmetric characteristic initial value problem for
the Einstein-Maxwell-scalar field equations. On the initial outgoing
characteristic, the data is assumed to satisfy the Price law decay widely
believed to hold on an event horizon arising from the collapse of an
asymptotically flat Cauchy surface. We establish that the heuristic mass
inflation scenario put forth by Israel and Poisson is mathematically correct in
the context of this initial value problem. In particular, the maximal domain of
development has a future boundary, over which the spacetime is extendible as a
continuous metric, but along which the Hawking mass blows up identically; thus,
the spacetime is inextendible as a differentiable metric. In view of recent
results of the author in collaboration with I. Rodnianski (gr-qc/0309115),
which rigorously establish the validity of Price's law as an upper bound for
the decay of scalar field hair, the continuous extendibility result applies to
the collapse of complete asymptotically flat spacelike data where the scalar
field is compactly supported on the initial hypersurface. This shows that under
Christodoulou's C^0 formulation, the strong cosmic censorship conjecture is
false for this system.
| [
{
"created": "Thu, 3 Jul 2003 14:47:34 GMT",
"version": "v1"
},
{
"created": "Tue, 23 Sep 2003 21:24:20 GMT",
"version": "v2"
},
{
"created": "Sat, 6 Nov 2004 14:34:27 GMT",
"version": "v3"
}
] | 2011-10-13 | [
[
"Dafermos",
"Mihalis",
""
]
] | We consider a spherically symmetric characteristic initial value problem for the Einstein-Maxwell-scalar field equations. On the initial outgoing characteristic, the data is assumed to satisfy the Price law decay widely believed to hold on an event horizon arising from the collapse of an asymptotically flat Cauchy surface. We establish that the heuristic mass inflation scenario put forth by Israel and Poisson is mathematically correct in the context of this initial value problem. In particular, the maximal domain of development has a future boundary, over which the spacetime is extendible as a continuous metric, but along which the Hawking mass blows up identically; thus, the spacetime is inextendible as a differentiable metric. In view of recent results of the author in collaboration with I. Rodnianski (gr-qc/0309115), which rigorously establish the validity of Price's law as an upper bound for the decay of scalar field hair, the continuous extendibility result applies to the collapse of complete asymptotically flat spacelike data where the scalar field is compactly supported on the initial hypersurface. This shows that under Christodoulou's C^0 formulation, the strong cosmic censorship conjecture is false for this system. |
1010.1641 | Edward Porter | J\'er\^ome Carr\'e and Edward K. Porter | The Effect of Data Gaps on LISA Galactic Binary Parameter Estimation | Submitted to Classical Quantum Gravity, 11 pages, four figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In the last few years there has been an enormous effort in parameter
estimation studies for different sources with the space based gravitational
wave detector, LISA. While these studies have investigated sources of differing
complexity, the one thing they all have in common is they assume continuous
data streams. In reality, the LISA data stream will contain gaps from such
possible events such as repointing of the satellite antennae, to discharging
static charge build up on the satellites, to disruptions due to micro-meteor
strikes. In this work we conduct a large scale Monte Carlo parameter estimation
simulation for galactic binaries assuming data streams containing gaps. As the
expected duration and frequency of the gaps are currently unknown, we have
decided to focus on gaps of approximately one hour, occurring either once per
day or once per week. We also study the case where, as well as the expected
periodic gaps, we have a data drop-out of one continuous week. Our results show
that for for galactic binaries, a gap of once per week introduces a bias of
between 0.5% and 1% in the estimation of parameters, for the most important
parameters such as the sky position, amplitude and frequency. This number rises
to between 3% and 7% for the case of one gap a day, and to between 4% and 9%
when we have one gap a day and a spurious gap of a week. A future study will
investigate the effect of data gaps on supermassive black hole binaries and
extreme mass ratio inspirals.
| [
{
"created": "Fri, 8 Oct 2010 10:03:06 GMT",
"version": "v1"
}
] | 2010-10-11 | [
[
"Carré",
"Jérôme",
""
],
[
"Porter",
"Edward K.",
""
]
] | In the last few years there has been an enormous effort in parameter estimation studies for different sources with the space based gravitational wave detector, LISA. While these studies have investigated sources of differing complexity, the one thing they all have in common is they assume continuous data streams. In reality, the LISA data stream will contain gaps from such possible events such as repointing of the satellite antennae, to discharging static charge build up on the satellites, to disruptions due to micro-meteor strikes. In this work we conduct a large scale Monte Carlo parameter estimation simulation for galactic binaries assuming data streams containing gaps. As the expected duration and frequency of the gaps are currently unknown, we have decided to focus on gaps of approximately one hour, occurring either once per day or once per week. We also study the case where, as well as the expected periodic gaps, we have a data drop-out of one continuous week. Our results show that for for galactic binaries, a gap of once per week introduces a bias of between 0.5% and 1% in the estimation of parameters, for the most important parameters such as the sky position, amplitude and frequency. This number rises to between 3% and 7% for the case of one gap a day, and to between 4% and 9% when we have one gap a day and a spurious gap of a week. A future study will investigate the effect of data gaps on supermassive black hole binaries and extreme mass ratio inspirals. |
1904.04258 | Steven B. Giddings | Steven B. Giddings, Seth Koren, and Gabriel Trevi\~no | Exploring strong-field deviations from general relativity via
gravitational waves | 20 pages, 9 figures. v2: references and CERN preprint number added | Phys. Rev. D 100, 044005 (2019) | 10.1103/PhysRevD.100.044005 | CERN-TH-2019-075 | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Two new observational windows have been opened to strong gravitational
physics: gravitational waves, and very long baseline interferometry. This
suggests observational searches for new phenomena in this regime, and in
particular for those necessary to make black hole evolution consistent with
quantum mechanics. We describe possible features of "compact quantum objects"
that replace classical black holes in a consistent quantum theory, and
approaches to observational tests for these using gravitational waves. This is
an example of a more general problem of finding consistent descriptions of
deviations from general relativity, which can be tested via gravitational wave
detection. Simple models for compact modifications to classical black holes are
described via an effective stress tensor, possibly with an effective equation
of state. A general discussion is given of possible observational signatures,
and of their dependence on properties of the colliding objects. The possibility
that departures from classical behavior are restricted to the near-horizon
regime raises the question of whether these will be obscured in gravitational
wave signals, due to their mutual interaction in a binary coalescence being
deep in the mutual gravitational well. Numerical simulation with such simple
models will be useful to clarify the sensitivity of gravitational wave
observation to such highly compact departures from classical black holes.
| [
{
"created": "Mon, 8 Apr 2019 18:00:01 GMT",
"version": "v1"
},
{
"created": "Mon, 27 May 2019 18:10:36 GMT",
"version": "v2"
}
] | 2019-08-07 | [
[
"Giddings",
"Steven B.",
""
],
[
"Koren",
"Seth",
""
],
[
"Treviño",
"Gabriel",
""
]
] | Two new observational windows have been opened to strong gravitational physics: gravitational waves, and very long baseline interferometry. This suggests observational searches for new phenomena in this regime, and in particular for those necessary to make black hole evolution consistent with quantum mechanics. We describe possible features of "compact quantum objects" that replace classical black holes in a consistent quantum theory, and approaches to observational tests for these using gravitational waves. This is an example of a more general problem of finding consistent descriptions of deviations from general relativity, which can be tested via gravitational wave detection. Simple models for compact modifications to classical black holes are described via an effective stress tensor, possibly with an effective equation of state. A general discussion is given of possible observational signatures, and of their dependence on properties of the colliding objects. The possibility that departures from classical behavior are restricted to the near-horizon regime raises the question of whether these will be obscured in gravitational wave signals, due to their mutual interaction in a binary coalescence being deep in the mutual gravitational well. Numerical simulation with such simple models will be useful to clarify the sensitivity of gravitational wave observation to such highly compact departures from classical black holes. |
1503.02638 | Nathan Johnson-McDaniel | Nathan K. Johnson-McDaniel, Abhay G. Shah, Bernard F. Whiting | Experimental mathematics meets gravitational self-force | 25 pages, 3 figures; version accepted by PRD, including various small
additions and corrections | Phys. Rev. D 92, 044007 (2015) | 10.1103/PhysRevD.92.044007 | ICTS/2015/3 | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | It is now possible to compute linear in mass-ratio terms in the
post-Newtonian (PN) expansion for compact binaries to very high orders using
black hole perturbation theory applied to various invariants. For instance, a
computation of the redshift invariant of a point particle in a circular orbit
about a black hole in linear perturbation theory gives the linear-in-mass-ratio
portion of the binding energy of a circular binary with arbitrary mass ratio.
This binding energy, in turn, encodes the system's conservative dynamics. We
give a method for extracting the analytic forms of these PN coefficients from
high-accuracy numerical data using experimental mathematics techniques, notably
an integer relation algorithm. Such methods should be particularly important
when the calculations progress to the considerably more difficult case of
perturbations of the Kerr metric. As an example, we apply this method to the
redshift invariant in Schwarzschild. Here we obtain analytic coefficients to
12.5PN, and higher-order terms in mixed analytic-numerical form to 21.5PN,
including analytic forms for the complete 13.5PN coefficient, and all the
logarithmic terms at 13PN. At these high orders, an individual coefficient can
have over 30 terms, including a wide variety of transcendental numbers, when
written out in full. We are still able to obtain analytic forms for such
coefficients from the numerical data through a careful study of the structure
of the expansion. The structure we find also allows us to predict certain
"leading logarithm"-type contributions to all orders. The additional terms in
the expansion we obtain improve the accuracy of the PN series for the redshift
observable, even in the very strong-field regime inside the innermost stable
circular orbit, particularly when combined with exponential resummation.
| [
{
"created": "Mon, 9 Mar 2015 19:36:17 GMT",
"version": "v1"
},
{
"created": "Mon, 27 Jul 2015 18:04:21 GMT",
"version": "v2"
}
] | 2015-08-12 | [
[
"Johnson-McDaniel",
"Nathan K.",
""
],
[
"Shah",
"Abhay G.",
""
],
[
"Whiting",
"Bernard F.",
""
]
] | It is now possible to compute linear in mass-ratio terms in the post-Newtonian (PN) expansion for compact binaries to very high orders using black hole perturbation theory applied to various invariants. For instance, a computation of the redshift invariant of a point particle in a circular orbit about a black hole in linear perturbation theory gives the linear-in-mass-ratio portion of the binding energy of a circular binary with arbitrary mass ratio. This binding energy, in turn, encodes the system's conservative dynamics. We give a method for extracting the analytic forms of these PN coefficients from high-accuracy numerical data using experimental mathematics techniques, notably an integer relation algorithm. Such methods should be particularly important when the calculations progress to the considerably more difficult case of perturbations of the Kerr metric. As an example, we apply this method to the redshift invariant in Schwarzschild. Here we obtain analytic coefficients to 12.5PN, and higher-order terms in mixed analytic-numerical form to 21.5PN, including analytic forms for the complete 13.5PN coefficient, and all the logarithmic terms at 13PN. At these high orders, an individual coefficient can have over 30 terms, including a wide variety of transcendental numbers, when written out in full. We are still able to obtain analytic forms for such coefficients from the numerical data through a careful study of the structure of the expansion. The structure we find also allows us to predict certain "leading logarithm"-type contributions to all orders. The additional terms in the expansion we obtain improve the accuracy of the PN series for the redshift observable, even in the very strong-field regime inside the innermost stable circular orbit, particularly when combined with exponential resummation. |
gr-qc/9701043 | Kubotani Hiroto | H. Kubotani, T. Uesugi, M. Morikawa, A. Sugamoto (Ochanomizu
University, Tokyo, Japan) | Classicalization of Quantum Fluctuation in Inflationary Universe | 24 pages, Latex, 2 Postscript figures | Prog.Theor.Phys. 98 (1997) 1063-1080 | 10.1143/PTP.98.1063 | OCHA-PP-90 | gr-qc | null | We discuss the classicalization of a quantum state induced by an environment
in the inflationary stage of the universe. The classicalization is necessary
for the homogeneous ground sate to become classical non-homogeneous one
accompanied with the statistical fluctuation, which is a plausible candidate
for the seeds of structure formation. Using simple models, we show that i) the
two classicalization criteria, the classical correlation and quantum
decoherence, are simultaneously satisfied by the environment and that ii) the
power spectrum of the resultant statistical fluctuation depends upon the detail
of the classicalization process. Especially, the result ii) means that, taking
account of the classicalization process, the inflationary scenario does not
necessarily predict the unique spectrum which is usually believed.
| [
{
"created": "Mon, 20 Jan 1997 07:23:27 GMT",
"version": "v1"
}
] | 2009-10-30 | [
[
"Kubotani",
"H.",
"",
"Ochanomizu\n University, Tokyo, Japan"
],
[
"Uesugi",
"T.",
"",
"Ochanomizu\n University, Tokyo, Japan"
],
[
"Morikawa",
"M.",
"",
"Ochanomizu\n University, Tokyo, Japan"
],
[
"Sugamoto",
"A.",
"",
"Ochanomizu\n University, Tokyo, Japan"
]
] | We discuss the classicalization of a quantum state induced by an environment in the inflationary stage of the universe. The classicalization is necessary for the homogeneous ground sate to become classical non-homogeneous one accompanied with the statistical fluctuation, which is a plausible candidate for the seeds of structure formation. Using simple models, we show that i) the two classicalization criteria, the classical correlation and quantum decoherence, are simultaneously satisfied by the environment and that ii) the power spectrum of the resultant statistical fluctuation depends upon the detail of the classicalization process. Especially, the result ii) means that, taking account of the classicalization process, the inflationary scenario does not necessarily predict the unique spectrum which is usually believed. |
gr-qc/0208091 | Hiroshi Kozaki | Hiroshi Kozaki and Ken-ichi Nakao | Volume Expansion of Swiss-Cheese Universe | 22 pages, 7 figures, to be submitted to Phys. Rev. D | Phys.Rev. D66 (2002) 104008 | 10.1103/PhysRevD.66.104008 | null | gr-qc | null | In order to investigate the effect of inhomogeneities on the volume expansion
of the universe, we study modified Swiss-Cheese universe model. Since this
model is an exact solution of Einstein equations, we can get an insight into
non-linear dynamics of inhomogeneous universe from it. We find that
inhomogeneities make the volume expansion slower than that of the background
Einstein-de Sitter universe when those can be regarded as small fluctuations in
the background universe. This result is consistent with the previous studies
based on the second order perturbation analysis. On the other hand, if the
inhomogeneities can not be treated as small perturbations, the volume expansion
of the universe depends on the type of fluctuations. Although the volume
expansion rate approaches to the background value asymptotically, the volume
itself can be finally arbitrarily smaller than the background one and can be
larger than that of the background but there is an upper bound on it.
| [
{
"created": "Fri, 30 Aug 2002 13:04:23 GMT",
"version": "v1"
},
{
"created": "Sat, 31 Aug 2002 04:52:41 GMT",
"version": "v2"
}
] | 2009-11-07 | [
[
"Kozaki",
"Hiroshi",
""
],
[
"Nakao",
"Ken-ichi",
""
]
] | In order to investigate the effect of inhomogeneities on the volume expansion of the universe, we study modified Swiss-Cheese universe model. Since this model is an exact solution of Einstein equations, we can get an insight into non-linear dynamics of inhomogeneous universe from it. We find that inhomogeneities make the volume expansion slower than that of the background Einstein-de Sitter universe when those can be regarded as small fluctuations in the background universe. This result is consistent with the previous studies based on the second order perturbation analysis. On the other hand, if the inhomogeneities can not be treated as small perturbations, the volume expansion of the universe depends on the type of fluctuations. Although the volume expansion rate approaches to the background value asymptotically, the volume itself can be finally arbitrarily smaller than the background one and can be larger than that of the background but there is an upper bound on it. |
gr-qc/0308085 | Julien Sylvestre | Julien Sylvestre and Massimo Tinto | Noise characterization for LISA | 9 figures | Phys.Rev. D68 (2003) 102002 | 10.1103/PhysRevD.68.102002 | null | gr-qc | null | We consider the general problem of estimating the inflight LISA noise power
spectra and cross-spectra, which are needed for detecting and estimating the
gravitational wave signals present in the LISA data. For the LISA baseline
design and in the long wavelength limit, we bound the error on all spectrum
estimators that rely on the use of the fully symmetric Sagnac combination
($\zeta$). This procedure avoids biases in the estimation that would otherwise
be introduced by the presence of a strong galactic background in the LISA data.
We specialize our discussion to the detection and study of the galactic white
dwarf-white dwarf binary stochastic signal.
| [
{
"created": "Tue, 26 Aug 2003 18:05:31 GMT",
"version": "v1"
}
] | 2009-11-10 | [
[
"Sylvestre",
"Julien",
""
],
[
"Tinto",
"Massimo",
""
]
] | We consider the general problem of estimating the inflight LISA noise power spectra and cross-spectra, which are needed for detecting and estimating the gravitational wave signals present in the LISA data. For the LISA baseline design and in the long wavelength limit, we bound the error on all spectrum estimators that rely on the use of the fully symmetric Sagnac combination ($\zeta$). This procedure avoids biases in the estimation that would otherwise be introduced by the presence of a strong galactic background in the LISA data. We specialize our discussion to the detection and study of the galactic white dwarf-white dwarf binary stochastic signal. |
2407.15804 | Supriya Pan | Sudip Halder, Supriya Pan, Paulo M. S\'a, Tapan Saha | Coupled phantom cosmological model motivated by the warm inflationary
paradigm | 12 pages including references, 3 tables and 4 captioned figures;
comments are welcome! | null | null | null | gr-qc astro-ph.CO | http://creativecommons.org/licenses/by/4.0/ | In this article, we investigate a coupled phantom dark-energy cosmological
model in which the coupling term between a phantom scalar field with an
exponential potential and a pressureless dark-matter fluid is motivated by the
warm inflationary paradigm. Using methods of qualitative analysis of dynamical
systems, complemented by numerical solutions of the evolution equations, we
study the late-time behavior of our model. We show that contrary to the
uncoupled scenario, the coupled phantom model admits accelerated scaling
solutions. However, they do not correspond to a final state of the universe's
evolution and, therefore, cannot be used to solve the cosmological coincidence
problem. Furthermore, we show that, for certain coupling parameter values, the
total equation-of-state parameter's asymptotic behavior is significantly
changed when compared to the uncoupled scenario, allowing for solutions less
phantom even for steeper potentials of the phantom scalar field.
| [
{
"created": "Mon, 22 Jul 2024 17:16:03 GMT",
"version": "v1"
}
] | 2024-07-23 | [
[
"Halder",
"Sudip",
""
],
[
"Pan",
"Supriya",
""
],
[
"Sá",
"Paulo M.",
""
],
[
"Saha",
"Tapan",
""
]
] | In this article, we investigate a coupled phantom dark-energy cosmological model in which the coupling term between a phantom scalar field with an exponential potential and a pressureless dark-matter fluid is motivated by the warm inflationary paradigm. Using methods of qualitative analysis of dynamical systems, complemented by numerical solutions of the evolution equations, we study the late-time behavior of our model. We show that contrary to the uncoupled scenario, the coupled phantom model admits accelerated scaling solutions. However, they do not correspond to a final state of the universe's evolution and, therefore, cannot be used to solve the cosmological coincidence problem. Furthermore, we show that, for certain coupling parameter values, the total equation-of-state parameter's asymptotic behavior is significantly changed when compared to the uncoupled scenario, allowing for solutions less phantom even for steeper potentials of the phantom scalar field. |
2303.04119 | Ernesto Contreras | R. Avalos, P. Bargue\~no and E. Contreras | A static and spherically symmetric hairy black hole in the framework of
the Gravitational Decoupling | null | Fortschr. Phys.2023, 2200171 | 10.1002/prop.202200171 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this work we construct a static and spherically symmetric black hole
geometry supported by a family of generic mono-parametric sources thorough the
Gravitational Decoupling. The parameter characterizing the matter sector can be
interpreted as hair which cannot be associated to any global charge. Although
the solution is constructed by demanding the weak energy condition, we find
that the resulting matter sector satisfies all the energy conditions at and
outside the horizon. We study the effect of the hair on the periastron advance
and the gravitational lensing of the black hole. We estimate the best WKB order
to compute the quasinormal frequencies for scalar, vector and tensor
perturbation fields.
| [
{
"created": "Tue, 7 Mar 2023 18:30:45 GMT",
"version": "v1"
}
] | 2023-03-08 | [
[
"Avalos",
"R.",
""
],
[
"Bargueño",
"P.",
""
],
[
"Contreras",
"E.",
""
]
] | In this work we construct a static and spherically symmetric black hole geometry supported by a family of generic mono-parametric sources thorough the Gravitational Decoupling. The parameter characterizing the matter sector can be interpreted as hair which cannot be associated to any global charge. Although the solution is constructed by demanding the weak energy condition, we find that the resulting matter sector satisfies all the energy conditions at and outside the horizon. We study the effect of the hair on the periastron advance and the gravitational lensing of the black hole. We estimate the best WKB order to compute the quasinormal frequencies for scalar, vector and tensor perturbation fields. |
1408.4956 | Andrea Geralico | Donato Bini, Andrea Geralico, Robert T. Jantzen, Oldrich Semer\'ak | Effect of radiation flux on test particle motion in the Vaidya spacetime | 21 pages, 8 figures; published version | Class. Quantum Grav. 28, 245019 (2011) | 10.1088/0264-9381/28/24/245019 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Motion of massive test particles in the nonvacuum spherically symmetric
radiating Vaidya spacetime is investigated, allowing for physical interaction
of the particles with the radiation field in terms of which the source
energy-momentum tensor is interpreted. This "Poynting-Robertson-like effect" is
modeled by the usual effective term describing a Thomson-type radiation drag
force. The equations of motion are studied for simple types of motion including
free motion (without interaction), purely radial and purely azimuthal
(circular) motion, and for the particular case of "static" equilibrium;
appropriate solutions are given where possible. The results---mainly those on
the possible existence of equilibrium positions---are compared with their
counterparts obtained previously for a test spherically symmetric radiation
field in a vacuum Schwarzschild background.
| [
{
"created": "Thu, 21 Aug 2014 11:03:03 GMT",
"version": "v1"
}
] | 2015-06-22 | [
[
"Bini",
"Donato",
""
],
[
"Geralico",
"Andrea",
""
],
[
"Jantzen",
"Robert T.",
""
],
[
"Semerák",
"Oldrich",
""
]
] | Motion of massive test particles in the nonvacuum spherically symmetric radiating Vaidya spacetime is investigated, allowing for physical interaction of the particles with the radiation field in terms of which the source energy-momentum tensor is interpreted. This "Poynting-Robertson-like effect" is modeled by the usual effective term describing a Thomson-type radiation drag force. The equations of motion are studied for simple types of motion including free motion (without interaction), purely radial and purely azimuthal (circular) motion, and for the particular case of "static" equilibrium; appropriate solutions are given where possible. The results---mainly those on the possible existence of equilibrium positions---are compared with their counterparts obtained previously for a test spherically symmetric radiation field in a vacuum Schwarzschild background. |
gr-qc/9501032 | Hans-Juergen Schmidt | Sabine Kluske | The de Sitter space-time as attractor solution in higher order gravity | 8 pages, LaTeX under using AMS-Symbols, no figures, e-mail via
hjschmi@rz.uni-potsdam.de, to appear in R. Santilli, G. Sardanashvili (Eds.)
"New frontiers in gravitation" Hadronic Press | null | null | Uni Potsdam Math 95/1 | gr-qc | null | For arbitrary high order of the field equation one can always find examples
where the de Sitter space-time is an attractor solution in the set of the
spatially flat Friedmann-Robertson-Walker models.
| [
{
"created": "Wed, 25 Jan 1995 17:26:26 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Kluske",
"Sabine",
""
]
] | For arbitrary high order of the field equation one can always find examples where the de Sitter space-time is an attractor solution in the set of the spatially flat Friedmann-Robertson-Walker models. |
2307.05879 | Carlos A. S. Almeida | C. A. S. Almeida and F. C. E. Lima | Effects of quantum fluctuations of the metric on a braneworld | 20 pages, 5 captioned figures. Updated version to match one to appear
in EPJP | null | null | null | gr-qc hep-th | http://creativecommons.org/licenses/by/4.0/ | Adopting the premise that the expected value of the quantum fluctuating
metric is linear, i.e., $\langle g^{\mu\nu}\rangle=\alpha g^{\mu\nu}$, we
analyze the modified gravity theory induced by the Einstein-Hilbert action
coupled to a matter field. This approach engenders the $f(R,T)$ gravity used to
investigate the braneworld. In this scenario, considering a thick brane, the
influence of metric fluctuations on brane dynamics is investigated.
Consequently, one shows how the metric fluctuations influence the vacuum
states. This influence has repercussions for modifying the brane energy and the
asymptotic profile of the matter field. After noticing these modifications, we
analyzed the most likely and stable structures from the matter field. One
performs this analysis considering the theoretical measure of differential
configurational entropy.
| [
{
"created": "Wed, 12 Jul 2023 02:52:15 GMT",
"version": "v1"
},
{
"created": "Mon, 17 Jun 2024 12:24:35 GMT",
"version": "v2"
}
] | 2024-06-18 | [
[
"Almeida",
"C. A. S.",
""
],
[
"Lima",
"F. C. E.",
""
]
] | Adopting the premise that the expected value of the quantum fluctuating metric is linear, i.e., $\langle g^{\mu\nu}\rangle=\alpha g^{\mu\nu}$, we analyze the modified gravity theory induced by the Einstein-Hilbert action coupled to a matter field. This approach engenders the $f(R,T)$ gravity used to investigate the braneworld. In this scenario, considering a thick brane, the influence of metric fluctuations on brane dynamics is investigated. Consequently, one shows how the metric fluctuations influence the vacuum states. This influence has repercussions for modifying the brane energy and the asymptotic profile of the matter field. After noticing these modifications, we analyzed the most likely and stable structures from the matter field. One performs this analysis considering the theoretical measure of differential configurational entropy. |
2002.02577 | Takafumi Kokubu | Takafumi Kokubu and Tomohiro Harada | Thin-shell wormholes in Einstein and Einstein-Gauss-Bonnet theories of
gravity | 52pages, 17figures, 6tables. This article belongs to the Special
Issue Recent Advances in Wormhole Physics (MDPI). This article is based on
arXiv:1411.5454 [gr-qc] and arXiv:1506.08550 [gr-qc] | Universe 2020, 6(11), 197 | null | RUP-20-4 | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We review recent works on the possibility for eternal existence of thin-shell
wormholes on Einstein and Einstein-Gauss-Bonnet gravity. We introduce
thin-shell wormholes that are categorized into a class of traversable wormhole
solutions. After that, we discuss stable thin-shell wormholes with
negative-tension branes in Reissner-Nordstr\"om-(anti) de Sitter spacetimes in
$d$ dimensional Einstein gravity. Imposing $Z_2$ symmetry, we construct and
classify traversable static thin-shell wormholes in spherical, planar and
hyperbolic symmetries. It is found that the spherical wormholes are stable
against spherically symmetric perturbations. It is also found that some classes
of wormholes in planar and hyperbolic symmetries with a negative cosmological
constant are stable against perturbations preserving symmetries. In most cases,
stable wormholes are found with the appropriate combination of an electric
charge and a negative cosmological constant. However, as special cases, there
are stable wormholes even with a vanishing cosmological constant in spherical
symmetry and with a vanishing electric charge in hyperbolic symmetry.
Subsequently, the existence and dynamical stability of traversable thin-shell
wormholes with electrically neutral negative-tension branes is discussed in
Einstein-Gauss-Bonnet theory of gravitation. We consider radial perturbations
against the shell for the solutions, which have the $Z_2$ symmetry. The effect
of the Gauss-Bonnet term on the stability depends on the spacetime symmetry.
| [
{
"created": "Fri, 7 Feb 2020 01:18:27 GMT",
"version": "v1"
},
{
"created": "Wed, 28 Oct 2020 05:37:22 GMT",
"version": "v2"
},
{
"created": "Fri, 30 Oct 2020 00:15:53 GMT",
"version": "v3"
}
] | 2020-11-02 | [
[
"Kokubu",
"Takafumi",
""
],
[
"Harada",
"Tomohiro",
""
]
] | We review recent works on the possibility for eternal existence of thin-shell wormholes on Einstein and Einstein-Gauss-Bonnet gravity. We introduce thin-shell wormholes that are categorized into a class of traversable wormhole solutions. After that, we discuss stable thin-shell wormholes with negative-tension branes in Reissner-Nordstr\"om-(anti) de Sitter spacetimes in $d$ dimensional Einstein gravity. Imposing $Z_2$ symmetry, we construct and classify traversable static thin-shell wormholes in spherical, planar and hyperbolic symmetries. It is found that the spherical wormholes are stable against spherically symmetric perturbations. It is also found that some classes of wormholes in planar and hyperbolic symmetries with a negative cosmological constant are stable against perturbations preserving symmetries. In most cases, stable wormholes are found with the appropriate combination of an electric charge and a negative cosmological constant. However, as special cases, there are stable wormholes even with a vanishing cosmological constant in spherical symmetry and with a vanishing electric charge in hyperbolic symmetry. Subsequently, the existence and dynamical stability of traversable thin-shell wormholes with electrically neutral negative-tension branes is discussed in Einstein-Gauss-Bonnet theory of gravitation. We consider radial perturbations against the shell for the solutions, which have the $Z_2$ symmetry. The effect of the Gauss-Bonnet term on the stability depends on the spacetime symmetry. |
0705.4372 | Kjell Tangen | Kjell Tangen | Generating Minimally Coupled Einstein-Scalar Field Solutions from Vacuum
Solutions with Arbitrary Cosmological Constant | 23 pages, 4 figures. v2: Replaced figures, more details on the
example solution in section VII.B | null | null | null | gr-qc | null | This paper generalizes two previously known techniques for generating
minimally coupled Einstein-scalar field solutions in 4 dimensions; the Buchdahl
and Fonarev transformations. By applying this solution generation technique,
minimally coupled Einstein-scalar field solutions can be generated from vacuum
solutions with arbitrary cosmological constant in arbitrary dimension. The only
requirement to a seed solution is that it posesses a hypersurface-orthogonal
Killing vector field. The generalization that allows us to use seed solutions
with arbitrary cosmological constant uncovers a new class of Einstein-scalar
field solutions that has previously not been studied. We apply the new solution
transformation to the (A)dS4 vacuum solution. Transforming the resulting
Einstein-scalar field solution to the conformal frame, a two-parameter family
of spatially finite, expanding and accelerating cosmological solutions are
found that are conformally isometric to the Einstein static universe RxS^3. We
study null geodesics and find that for any observer, the solution has a
cosmological horizon at an angular distance of pi/2 away from the observer. We
find that a subset of these solutions can be naturally interpreted as expanding
cosmologies in which a scalar black hole is formed at late times. The
conformally coupled scalar field satisfies the weak energy condition as long as
the energy density is positive, while the strong energy condition is generally
violated.
| [
{
"created": "Wed, 30 May 2007 15:45:49 GMT",
"version": "v1"
},
{
"created": "Mon, 4 Jun 2007 11:22:27 GMT",
"version": "v2"
}
] | 2007-06-13 | [
[
"Tangen",
"Kjell",
""
]
] | This paper generalizes two previously known techniques for generating minimally coupled Einstein-scalar field solutions in 4 dimensions; the Buchdahl and Fonarev transformations. By applying this solution generation technique, minimally coupled Einstein-scalar field solutions can be generated from vacuum solutions with arbitrary cosmological constant in arbitrary dimension. The only requirement to a seed solution is that it posesses a hypersurface-orthogonal Killing vector field. The generalization that allows us to use seed solutions with arbitrary cosmological constant uncovers a new class of Einstein-scalar field solutions that has previously not been studied. We apply the new solution transformation to the (A)dS4 vacuum solution. Transforming the resulting Einstein-scalar field solution to the conformal frame, a two-parameter family of spatially finite, expanding and accelerating cosmological solutions are found that are conformally isometric to the Einstein static universe RxS^3. We study null geodesics and find that for any observer, the solution has a cosmological horizon at an angular distance of pi/2 away from the observer. We find that a subset of these solutions can be naturally interpreted as expanding cosmologies in which a scalar black hole is formed at late times. The conformally coupled scalar field satisfies the weak energy condition as long as the energy density is positive, while the strong energy condition is generally violated. |
gr-qc/0305038 | Niall O. Murchadha | Niall O Murchadha | General Relativity from the three dimensional linear group | 4 pages, Revtex 4 | null | null | null | gr-qc | null | This letter describes a novel derivation of general relativity by considering
the (non)self-consistency of theories whose Hamiltonians are constraints. The
constraints, from Hamilton's equations, generate the evolution, while the
evolution, in turn, must preserve the constraints. This closure requirement can
be used as a selection mechanism for general relativity starting from a very
simple set of assumptions. The configuration space is chosen to be a family of
$3 \times 3$ positive definite symmetric matrices on some bare 3-manifold. A
general Hamiltonian is constructed on this space of matrices which consists of
a single constraint per space point. It is assumed that this constraint looks
like an energy balance relationship. It will be the sum of a `kinetic' term
which is quadratic and undifferentiated in the momenta, and a `potential' term,
which is any function of the configuration variables. Further, the constraint
must be a scalar under the linear group, the natural symmetry group of the
configuration space. This inexorably leads to the ADM Hamiltonian for general
relativity. Both the space of Riemannian geometries (Wheeler's superspace), and
spacetime are emergent quantities in this analysis.
| [
{
"created": "Sat, 10 May 2003 00:28:21 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Murchadha",
"Niall O",
""
]
] | This letter describes a novel derivation of general relativity by considering the (non)self-consistency of theories whose Hamiltonians are constraints. The constraints, from Hamilton's equations, generate the evolution, while the evolution, in turn, must preserve the constraints. This closure requirement can be used as a selection mechanism for general relativity starting from a very simple set of assumptions. The configuration space is chosen to be a family of $3 \times 3$ positive definite symmetric matrices on some bare 3-manifold. A general Hamiltonian is constructed on this space of matrices which consists of a single constraint per space point. It is assumed that this constraint looks like an energy balance relationship. It will be the sum of a `kinetic' term which is quadratic and undifferentiated in the momenta, and a `potential' term, which is any function of the configuration variables. Further, the constraint must be a scalar under the linear group, the natural symmetry group of the configuration space. This inexorably leads to the ADM Hamiltonian for general relativity. Both the space of Riemannian geometries (Wheeler's superspace), and spacetime are emergent quantities in this analysis. |
1409.6816 | Yoshimune Tomikawa | Yoshimune Tomikawa, Tetsuya Shiromizu, Keisuke Izumi | Wormhole on DGP brane | 7 pages, minor corrections, version to appear in PRD | null | 10.1103/PhysRevD.90.126001 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We analyze a spacetime structure on a new brane configuration constructed
recently in the Dvali-Gabadadze-Porrati braneworld context. The brane, embedded
on a five-dimensional bubble of nothing, has a wormhole structure. It is an
exact solution without any matter fields, and thus the energy conditions for
matter fields are trivially satisfied. We see that, under the traversability
condition, the size of the bubble should be larger than 10^{10}cm or so.
| [
{
"created": "Wed, 24 Sep 2014 04:11:20 GMT",
"version": "v1"
},
{
"created": "Mon, 17 Nov 2014 07:15:05 GMT",
"version": "v2"
}
] | 2015-06-23 | [
[
"Tomikawa",
"Yoshimune",
""
],
[
"Shiromizu",
"Tetsuya",
""
],
[
"Izumi",
"Keisuke",
""
]
] | We analyze a spacetime structure on a new brane configuration constructed recently in the Dvali-Gabadadze-Porrati braneworld context. The brane, embedded on a five-dimensional bubble of nothing, has a wormhole structure. It is an exact solution without any matter fields, and thus the energy conditions for matter fields are trivially satisfied. We see that, under the traversability condition, the size of the bubble should be larger than 10^{10}cm or so. |
1108.0078 | Miguel Vazquez-Mozo | Luis Alvarez-Gaume, Ehsan Hatefi | Critical Collapse in the Axion-Dilaton System in Diverse Dimensions | LaTeX, 10 pages, no figures | Class. Quantum Grav. 29 (2012) 025006 | 10.1088/0264-9381/29/2/025006 | CERN-PH-TH/2011-167 | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the gravitational collapse of the axion-dilaton system suggested by
type IIB string theory in dimensions ranging from four to ten. We extend
previous analysis concerning the role played by the global SL(2,R) symmetry and
we evaluate the Choptuik exponents in the elliptic case.
| [
{
"created": "Sat, 30 Jul 2011 15:17:50 GMT",
"version": "v1"
}
] | 2011-12-30 | [
[
"Alvarez-Gaume",
"Luis",
""
],
[
"Hatefi",
"Ehsan",
""
]
] | We study the gravitational collapse of the axion-dilaton system suggested by type IIB string theory in dimensions ranging from four to ten. We extend previous analysis concerning the role played by the global SL(2,R) symmetry and we evaluate the Choptuik exponents in the elliptic case. |
2009.01088 | Jorge Bellorin | J. Bellorin, C. Borquez and B. Droguett | Asymptotic flatness and nonflat solutions in the critical 2+1 Horava
theory | This version matches the version published in journal. arXiv admin
note: substantial text overlap with arXiv:2006.08693 | Gen. Rel. Grav. 53 (2021) 2, 19 | 10.1007/s10714-021-02793-4 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Horava theory in 2+1 dimensions can be formulated at a critical point in
the space of coupling constants where it has no local degrees of freedom. This
suggests that this critical case could share many features with 2+1 general
relativity, in particular its large-distance effective action that is of second
order in derivatives. To deepen on this relationship, we study the
asymptotically flat solutions of the effective action. We take the general
definition of asymptotic flatness from 2+1 general relativity, where an
asymptotically flat region with a nonfixed conical angle is approached. We show
that a class of regular asymptotically flat solutions are totally flat. The
class is characterized by having nonnegative energy (when the coupling constant
of the Ricci scalar is positive). We present a detailed canonical analysis on
the effective action showing that the dynamics of the theory forbids local
degrees of freedom. Another similarity with 2+1 general relativity is the
absence of a Newtonian force. In contrast to these results, we find evidence
against the similarity with 2+1 general relativity: we find an exact nonflat
solution of the same effective theory. This solution is out of the set of
asymptotically flat solutions.
| [
{
"created": "Tue, 1 Sep 2020 12:03:57 GMT",
"version": "v1"
},
{
"created": "Tue, 23 Mar 2021 16:25:54 GMT",
"version": "v2"
}
] | 2021-03-24 | [
[
"Bellorin",
"J.",
""
],
[
"Borquez",
"C.",
""
],
[
"Droguett",
"B.",
""
]
] | The Horava theory in 2+1 dimensions can be formulated at a critical point in the space of coupling constants where it has no local degrees of freedom. This suggests that this critical case could share many features with 2+1 general relativity, in particular its large-distance effective action that is of second order in derivatives. To deepen on this relationship, we study the asymptotically flat solutions of the effective action. We take the general definition of asymptotic flatness from 2+1 general relativity, where an asymptotically flat region with a nonfixed conical angle is approached. We show that a class of regular asymptotically flat solutions are totally flat. The class is characterized by having nonnegative energy (when the coupling constant of the Ricci scalar is positive). We present a detailed canonical analysis on the effective action showing that the dynamics of the theory forbids local degrees of freedom. Another similarity with 2+1 general relativity is the absence of a Newtonian force. In contrast to these results, we find evidence against the similarity with 2+1 general relativity: we find an exact nonflat solution of the same effective theory. This solution is out of the set of asymptotically flat solutions. |
gr-qc/9805091 | Valter Moretti | Valter Moretti (Math. Dept. Trento University) | Local $\zeta$-function techniques vs point-splitting procedure: a few
rigorous results | 40 pages, latex, no figures, shortened version, some previous
Comments and minor errors corrected, final version accepted for publication
in Commun. Math. Phys | Commun.Math.Phys. 201 (1999) 327-363 | 10.1007/s002200050558 | null | gr-qc hep-th math-ph math.MP | null | Some general properties of local $\zeta$-function procedures to renormalize
some quantities in $D$-dimensional (Euclidean) Quantum Field Theory in curved
background are rigorously discussed for positive scalar operators $-\Delta +
V(x)$ in general closed $D$-manifolds, and a few comments are given for
nonclosed manifolds too. A general comparison is carried out with respect to
the more known point-splitting procedure concerning the effective Lagrangian
and the field fluctuations. It is proven that, for $D>1$, the local
$\zeta$-function and point-splitting approaches lead essentially to the same
results apart from some differences in the subtraction procedure of the
Hadamard divergences. It is found that the $\zeta$ function procedure picks out
a particular term $w_0(x,y)$ in the Hadamard expansion. Also the presence of an
untrivial kernel of the operator $-\Delta +V(x)$ may produce some differences
between the two analyzed approaches. Finally, a formal identity concerning the
field fluctuations, used by physicists, is discussed and proven within the
local $\zeta$-function approach. This is done also to reply to recent criticism
against $\zeta$-function techniques.
| [
{
"created": "Tue, 26 May 1998 12:31:12 GMT",
"version": "v1"
},
{
"created": "Fri, 5 Jun 1998 13:33:59 GMT",
"version": "v2"
},
{
"created": "Thu, 27 Aug 1998 14:43:30 GMT",
"version": "v3"
}
] | 2009-10-31 | [
[
"Moretti",
"Valter",
"",
"Math. Dept. Trento University"
]
] | Some general properties of local $\zeta$-function procedures to renormalize some quantities in $D$-dimensional (Euclidean) Quantum Field Theory in curved background are rigorously discussed for positive scalar operators $-\Delta + V(x)$ in general closed $D$-manifolds, and a few comments are given for nonclosed manifolds too. A general comparison is carried out with respect to the more known point-splitting procedure concerning the effective Lagrangian and the field fluctuations. It is proven that, for $D>1$, the local $\zeta$-function and point-splitting approaches lead essentially to the same results apart from some differences in the subtraction procedure of the Hadamard divergences. It is found that the $\zeta$ function procedure picks out a particular term $w_0(x,y)$ in the Hadamard expansion. Also the presence of an untrivial kernel of the operator $-\Delta +V(x)$ may produce some differences between the two analyzed approaches. Finally, a formal identity concerning the field fluctuations, used by physicists, is discussed and proven within the local $\zeta$-function approach. This is done also to reply to recent criticism against $\zeta$-function techniques. |
1303.0912 | Vladimir Dzhunushaliev | Ascar K. Aringazin and Vladimir Dzhunushaliev | Decomposed Finsler geometry: decomposed Finsler gravity and physical
applications | 8 pages | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Special class of Finsler metrics that can be decomposed to the product of two
Riemannian metrics is considered. Based on such decomposition a new kind of
Finsler gravity is suggested. Physical applications of Finsler decomposed
metric are considered.
| [
{
"created": "Tue, 5 Mar 2013 02:51:04 GMT",
"version": "v1"
}
] | 2013-03-06 | [
[
"Aringazin",
"Ascar K.",
""
],
[
"Dzhunushaliev",
"Vladimir",
""
]
] | Special class of Finsler metrics that can be decomposed to the product of two Riemannian metrics is considered. Based on such decomposition a new kind of Finsler gravity is suggested. Physical applications of Finsler decomposed metric are considered. |
0902.0190 | Reiner Hedrich | Reiner Hedrich | Quantum Gravity: Has Spacetime Quantum Properties? | 31 pages | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The incompatibility between GR and QM is generally seen as a sufficient
motivation for the development of a theory of Quantum Gravity. If - so a
typical argumentation - QM gives a universally valid basis for the description
of all natural systems, then the gravitational field should have quantum
properties. Together with the arguments against semi-classical theories of
gravity, this leads to a strategy which takes a quantization of GR as the
natural avenue to Quantum Gravity. And a quantization of the gravitational
field would in some sense correspond to a quantization of geometry. Spacetime
would have quantum properties. But, this strategy will only be successful, if
gravity is a fundamental interaction. - What, if gravity is instead an
intrinsically classical phenomenon? Then, if QM is nevertheless fundamentally
valid, gravity can not be a fundamental interaction. An intrinsically classical
gravity in a quantum world would have to be an emergent, induced or residual,
macroscopic effect, caused by other interactions. The gravitational field (as
well as spacetime) would not have any quantum properties. A quantization of GR
would lead to artifacts without any relation to nature. The serious problems of
all approaches to Quantum Gravity that start from a direct quantization of GR
or try to capture the quantum properties of gravity in form of a 'graviton'
dynamics - together with the, meanwhile, rich spectrum of approaches to an
emergent gravity and/or spacetime - make this latter option more and more
interesting for the development of a theory of Quantum Gravity. The most
advanced emergent gravity (and spacetime) scenarios are of an
information-theoretical, quantum-computational type.
| [
{
"created": "Mon, 2 Feb 2009 02:34:51 GMT",
"version": "v1"
}
] | 2009-02-03 | [
[
"Hedrich",
"Reiner",
""
]
] | The incompatibility between GR and QM is generally seen as a sufficient motivation for the development of a theory of Quantum Gravity. If - so a typical argumentation - QM gives a universally valid basis for the description of all natural systems, then the gravitational field should have quantum properties. Together with the arguments against semi-classical theories of gravity, this leads to a strategy which takes a quantization of GR as the natural avenue to Quantum Gravity. And a quantization of the gravitational field would in some sense correspond to a quantization of geometry. Spacetime would have quantum properties. But, this strategy will only be successful, if gravity is a fundamental interaction. - What, if gravity is instead an intrinsically classical phenomenon? Then, if QM is nevertheless fundamentally valid, gravity can not be a fundamental interaction. An intrinsically classical gravity in a quantum world would have to be an emergent, induced or residual, macroscopic effect, caused by other interactions. The gravitational field (as well as spacetime) would not have any quantum properties. A quantization of GR would lead to artifacts without any relation to nature. The serious problems of all approaches to Quantum Gravity that start from a direct quantization of GR or try to capture the quantum properties of gravity in form of a 'graviton' dynamics - together with the, meanwhile, rich spectrum of approaches to an emergent gravity and/or spacetime - make this latter option more and more interesting for the development of a theory of Quantum Gravity. The most advanced emergent gravity (and spacetime) scenarios are of an information-theoretical, quantum-computational type. |
1606.07889 | Maurizio Gasperini | M. Gasperini | Observable gravitational waves in pre-big bang cosmology: an update | 14 pages, 6 figures. Typos corrected, references updated, a few
comments added | JCAP 12 (2016) 010 | 10.1088/1475-7516/2016/12/010 | BA-TH/706-16 | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In the light of the recent results concerning CMB observations and GW
detection we address the question of whether it is possible, in a
self-consistent inflationary framework, to simultaneously generate a spectrum
of scalar metric perturbations in agreement with Planck data and a stochastic
background of primordial gravitational radiation compatible with the design
sensitivity of aLIGO/Virgo and/or eLISA. We suggest that this is possible in a
string cosmology context, for a wide region of the parameter space of the
so-called pre-big bang models. We also discuss the associated values of the
tensor-to-scalar ratio relevant to the CMB polarization experiments. We
conclude that future, cross-correlated results from CMB observations and GW
detectors will be able to confirm or disprove pre-big bang models and -- in any
case -- will impose new significant constraints on the basic string
theory/cosmology parameters.
| [
{
"created": "Sat, 25 Jun 2016 09:07:58 GMT",
"version": "v1"
},
{
"created": "Mon, 21 Nov 2016 22:50:37 GMT",
"version": "v2"
},
{
"created": "Wed, 23 Nov 2016 16:49:27 GMT",
"version": "v3"
}
] | 2016-12-08 | [
[
"Gasperini",
"M.",
""
]
] | In the light of the recent results concerning CMB observations and GW detection we address the question of whether it is possible, in a self-consistent inflationary framework, to simultaneously generate a spectrum of scalar metric perturbations in agreement with Planck data and a stochastic background of primordial gravitational radiation compatible with the design sensitivity of aLIGO/Virgo and/or eLISA. We suggest that this is possible in a string cosmology context, for a wide region of the parameter space of the so-called pre-big bang models. We also discuss the associated values of the tensor-to-scalar ratio relevant to the CMB polarization experiments. We conclude that future, cross-correlated results from CMB observations and GW detectors will be able to confirm or disprove pre-big bang models and -- in any case -- will impose new significant constraints on the basic string theory/cosmology parameters. |
2303.17767 | Maxime Van de Moortel | Federico Pasqualotto and Yakov Shlapentokh-Rothman and Maxime Van de
Moortel | The asymptotics of massive fields on stationary spherically symmetric
black holes for all angular momenta | Version 2, 41 pages. Minor modifications | null | null | null | gr-qc math-ph math.AP math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the massive scalar field equation $\Box_g \phi = m^2 \phi$ on a
stationary and spherically symmetric black hole $g$ (including in particular
the Schwarzschild and Reissner--Nordstr\"om black holes in the full
sub-extremal range) for solutions $\phi$ projected on a fixed spherical
harmonic. Our problem involves the scattering of an attractive long-range
potential (Coulomb-like) and thus cannot be treated perturbatively.
We prove precise (point-wise) asymptotic tails of the form $t^{-5/6} f(t)+
O(t^{-1+\delta})$, where $f(t)$ is an explicit oscillating profile. Our
asymptotics appear to be the first rigorous decay result for a massive scalar
field on a black hole. Establishing these asymptotics is also an important step
in retrieving the assumptions used in work of the third author regarding the
interior of dynamical black holes and Strong Cosmic Censorship.
| [
{
"created": "Fri, 31 Mar 2023 02:09:53 GMT",
"version": "v1"
},
{
"created": "Fri, 5 Jan 2024 01:03:01 GMT",
"version": "v2"
}
] | 2024-01-08 | [
[
"Pasqualotto",
"Federico",
""
],
[
"Shlapentokh-Rothman",
"Yakov",
""
],
[
"Van de Moortel",
"Maxime",
""
]
] | We study the massive scalar field equation $\Box_g \phi = m^2 \phi$ on a stationary and spherically symmetric black hole $g$ (including in particular the Schwarzschild and Reissner--Nordstr\"om black holes in the full sub-extremal range) for solutions $\phi$ projected on a fixed spherical harmonic. Our problem involves the scattering of an attractive long-range potential (Coulomb-like) and thus cannot be treated perturbatively. We prove precise (point-wise) asymptotic tails of the form $t^{-5/6} f(t)+ O(t^{-1+\delta})$, where $f(t)$ is an explicit oscillating profile. Our asymptotics appear to be the first rigorous decay result for a massive scalar field on a black hole. Establishing these asymptotics is also an important step in retrieving the assumptions used in work of the third author regarding the interior of dynamical black holes and Strong Cosmic Censorship. |
1406.6891 | Edward Porter | Edward K. Porter | The Challenges in Gravitational Wave Astronomy for Space-Based Detectors | 12 pages. Plenary presentation to appear in the Proceedings of the
Sant Cugat Forum on Astrophysics, Sant Cugat, April 22-25, 2014 | null | 10.1007/978-3-319-10488-1_23 | null | gr-qc astro-ph.IM | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Gravitational Wave (GW) universe contains a wealth of sources which, with
the proper treatment, will open up the universe as never before. By observing
massive black hole binaries to high redshifts, we should begin to explore the
formation process of seed black holes and track galactic evolution to the
present day. Observations of extreme mass ratio inspirals will allow us to
explore galactic centers in the local universe, as well as providing tests of
General Relativity and constraining the value of Hubble's constant. The
detection of compact binaries in our own galaxy may allow us to model stellar
evolution in the Milky Way. Finally, the detection of cosmic (super)strings and
a stochastic background would help us to constrain cosmological models.
However, all of this depends on our ability to not only resolve sources and
carry out parameter estimation, but also on our ability to define an optimal
data analysis strategy. In this presentation, I will examine the challenges
that lie ahead in GW astronomy for the ESA L3 Cosmic Vision mission, eLISA.
| [
{
"created": "Thu, 26 Jun 2014 14:02:11 GMT",
"version": "v1"
}
] | 2015-06-22 | [
[
"Porter",
"Edward K.",
""
]
] | The Gravitational Wave (GW) universe contains a wealth of sources which, with the proper treatment, will open up the universe as never before. By observing massive black hole binaries to high redshifts, we should begin to explore the formation process of seed black holes and track galactic evolution to the present day. Observations of extreme mass ratio inspirals will allow us to explore galactic centers in the local universe, as well as providing tests of General Relativity and constraining the value of Hubble's constant. The detection of compact binaries in our own galaxy may allow us to model stellar evolution in the Milky Way. Finally, the detection of cosmic (super)strings and a stochastic background would help us to constrain cosmological models. However, all of this depends on our ability to not only resolve sources and carry out parameter estimation, but also on our ability to define an optimal data analysis strategy. In this presentation, I will examine the challenges that lie ahead in GW astronomy for the ESA L3 Cosmic Vision mission, eLISA. |
1509.06806 | Julio Cesar Fabris | J.C. Fabris, O.F. Piattella, D.C. Rodrigues, B. Chauvineau, M.H.
Daouda | Introducing quantum effects in classical theories | Latex file, 10 pages. To appear in the proceedings of the 9th
Friedmann Seminar, St. Petersburg, Russia, june 21-27, 2015 | null | 10.1142/S0217751X16410086 | null | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, we explore two different ways of implementing quantum effects
in a classical structure. The first one is through an external field. The other
one is modifying the classical conservation laws. In both cases, the
consequences for the description of the evolution of the universe are
discussed.
| [
{
"created": "Tue, 22 Sep 2015 23:11:30 GMT",
"version": "v1"
},
{
"created": "Thu, 24 Sep 2015 19:24:45 GMT",
"version": "v2"
},
{
"created": "Mon, 5 Oct 2015 12:58:22 GMT",
"version": "v3"
}
] | 2016-02-03 | [
[
"Fabris",
"J. C.",
""
],
[
"Piattella",
"O. F.",
""
],
[
"Rodrigues",
"D. C.",
""
],
[
"Chauvineau",
"B.",
""
],
[
"Daouda",
"M. H.",
""
]
] | In this paper, we explore two different ways of implementing quantum effects in a classical structure. The first one is through an external field. The other one is modifying the classical conservation laws. In both cases, the consequences for the description of the evolution of the universe are discussed. |
0911.2486 | Sergio Dain | Sergio Dain | Angular momentum-mass inequality for axisymmetric black holes | 7 pages, 1 figure | New Trends in Mathematical Physics, Selected contributions of the
XVth International Congress on Mathematical Physics. Sidoravicius, Vladas
(Ed.), Springer, 2009 | 10.1007/978-90-481-2810-5_12 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In these notes we describe recent results concerning the inequality $m\geq
\sqrt{|J|}$ for axially symmetric black holes.
| [
{
"created": "Thu, 12 Nov 2009 22:01:33 GMT",
"version": "v1"
}
] | 2009-11-16 | [
[
"Dain",
"Sergio",
""
]
] | In these notes we describe recent results concerning the inequality $m\geq \sqrt{|J|}$ for axially symmetric black holes. |
gr-qc/9508051 | Atsushi Higuchi | C.J. Fewster and A. Higuchi | Quantum Field Theory on Certain Non-Globally Hyperbolic Spacetimes | 14 pages, latex, one figure (incorporated in latex source) | Class.Quant.Grav.13:51-62,1996 | 10.1088/0264-9381/13/1/006 | BUTP-95/31 | gr-qc | null | We study real linear scalar field theory on two simple non-globally
hyperbolic spacetimes containing closed timelike curves within the framework
proposed by Kay for algebraic quantum field theory on non-globally hyperbolic
spacetimes. In this context, a spacetime (M,g) is said to be `F-quantum
compatible' with a field theory if it admits a *-algebra of local observables
for that theory which satisfies a locality condition known as `F-locality'.
Kay's proposal is that, in formulating algebraic quantum field theory on
$(M,g)$, F-locality should be imposed as a necessary condition on the *-algebra
of observables. The spacetimes studied are the 2- and 4-dimensional spacelike
cylinders (Minkowski space quotiented by a timelike translation). Kay has shown
that the 4-dimensional spacelike cylinder is F-quantum compatible with massless
fields. We prove that it is also F-quantum compatible with massive fields and
prove the F-quantum compatibility of the 2-dimensional spacelike cylinder with
both massive and massless fields. In each case, F-quantum compatibility is
proved by constructing a suitable F-local algebra.
| [
{
"created": "Thu, 24 Aug 1995 15:49:44 GMT",
"version": "v1"
}
] | 2008-11-26 | [
[
"Fewster",
"C. J.",
""
],
[
"Higuchi",
"A.",
""
]
] | We study real linear scalar field theory on two simple non-globally hyperbolic spacetimes containing closed timelike curves within the framework proposed by Kay for algebraic quantum field theory on non-globally hyperbolic spacetimes. In this context, a spacetime (M,g) is said to be `F-quantum compatible' with a field theory if it admits a *-algebra of local observables for that theory which satisfies a locality condition known as `F-locality'. Kay's proposal is that, in formulating algebraic quantum field theory on $(M,g)$, F-locality should be imposed as a necessary condition on the *-algebra of observables. The spacetimes studied are the 2- and 4-dimensional spacelike cylinders (Minkowski space quotiented by a timelike translation). Kay has shown that the 4-dimensional spacelike cylinder is F-quantum compatible with massless fields. We prove that it is also F-quantum compatible with massive fields and prove the F-quantum compatibility of the 2-dimensional spacelike cylinder with both massive and massless fields. In each case, F-quantum compatibility is proved by constructing a suitable F-local algebra. |
gr-qc/0111010 | Mustapha Ishak | Roberto A. Sussman, Mustapha Ishak | Adiabatic models of the cosmological radiative era | 19 pages revtex4, 10 figures. Final form to appear in Gen. Rel. Grav | Gen.Rel.Grav. 34 (2002) 1589-1616 | null | null | gr-qc | null | We consider a generalization of the Lemaitre-Tolman-Bondi (LTB) solutions by
keeping the LTB metric but replacing its dust matter source by an imperfect
fluid with anisotropic pressure $\Pi_{ab} $. Assuming that total matter-energy
density $\rho$ is the sum of a rest mass term, $\rhom$, plus a radiation
$\rhor=3p$ density where $p$ is the isotropic pressure, Einstein's equations
are fully integrated without having to place any previous assumption on the
form of $\Pi_{ab} $. Three particular cases of interest are contained: the
usual LTB dust solutions (the dust limit), a class of FLRW cosmologies (the
homogeneous limit) and of the Vaydia solution (the vacuum limit). Initial
conditions are provided in terms of suitable averages and contrast functions of
the initial densities of $\rhom, \rhor$ and the 3-dimensional Ricci scalar
along an arbitrary initial surface $t=t_i$. We consider the source of the
models as an interactive radiation-matter mixture in local thermal equilibrium
that must be consistent with causal Extended Irreversible Thermodynamics (hence
$\Pi_{ab} $ is shear viscosity). Assuming near equilibrium conditions
associated with small initial density and curvature contrasts, the evolution of
the models is qualitatively similar to that of adiabatic perturbations on a
matter plus radiation FLRW background. We show that initial conditions exist
that lead to thermodynamically consistent models, but only for the full
transport equation of Extended Irreversible Thermodynamics. These interactive
mixtures provide a reasonable approximation to a dissipative 'tight coupling'
characteristic of radiation-matter mixtures in the radiative pre-decoupling
era.
| [
{
"created": "Mon, 5 Nov 2001 04:50:08 GMT",
"version": "v1"
},
{
"created": "Tue, 16 Apr 2002 15:49:39 GMT",
"version": "v2"
}
] | 2007-05-23 | [
[
"Sussman",
"Roberto A.",
""
],
[
"Ishak",
"Mustapha",
""
]
] | We consider a generalization of the Lemaitre-Tolman-Bondi (LTB) solutions by keeping the LTB metric but replacing its dust matter source by an imperfect fluid with anisotropic pressure $\Pi_{ab} $. Assuming that total matter-energy density $\rho$ is the sum of a rest mass term, $\rhom$, plus a radiation $\rhor=3p$ density where $p$ is the isotropic pressure, Einstein's equations are fully integrated without having to place any previous assumption on the form of $\Pi_{ab} $. Three particular cases of interest are contained: the usual LTB dust solutions (the dust limit), a class of FLRW cosmologies (the homogeneous limit) and of the Vaydia solution (the vacuum limit). Initial conditions are provided in terms of suitable averages and contrast functions of the initial densities of $\rhom, \rhor$ and the 3-dimensional Ricci scalar along an arbitrary initial surface $t=t_i$. We consider the source of the models as an interactive radiation-matter mixture in local thermal equilibrium that must be consistent with causal Extended Irreversible Thermodynamics (hence $\Pi_{ab} $ is shear viscosity). Assuming near equilibrium conditions associated with small initial density and curvature contrasts, the evolution of the models is qualitatively similar to that of adiabatic perturbations on a matter plus radiation FLRW background. We show that initial conditions exist that lead to thermodynamically consistent models, but only for the full transport equation of Extended Irreversible Thermodynamics. These interactive mixtures provide a reasonable approximation to a dissipative 'tight coupling' characteristic of radiation-matter mixtures in the radiative pre-decoupling era. |
gr-qc/9412004 | null | S. R. Vatsya | Mechanics of a Particle in a Gauge Field | A new Gauge theoretical description of Quantum Mechanics. 30 pages,
LaTeX, To appear in Can. J. Phys. Corr: 80 Char. lines | Can.J.Phys. 73 (1995) 85-95 | 10.1139/p95-013 | null | gr-qc | null | The action principle is frequently used to derive the classical equations of
motion. The action may also be used to associate group elements with curves in
the space-time manifold, similar to the gauge transformations. The action
principle is shown here to be an equivalence relation between the infinitesimal
elements so defined for a collection of closed curves and the identity element.
The action principle is then extended by requiring the equivalence of global
elements with the identity and by considering all curves. The resulting
equation is generalized further to include the non-Abelian gauge fields. The
extended equation has an infinite number, but not all, trajectories as
solutions. The properties of these paths are shown to impart wave-like
properties to the particles in motion. These results provide an insight into
the wave-particle duality and lead to a modified path-integral formalism. The
motion of a particle is formulated within the resulting framework which yields
a generalized Schrodinger equation. This equation is shown to reduce to a set
of equations, one of them being the Klein-Gordon equation.
| [
{
"created": "Thu, 1 Dec 1994 18:53:26 GMT",
"version": "v1"
},
{
"created": "Sun, 4 Dec 1994 00:24:17 GMT",
"version": "v2"
}
] | 2015-06-25 | [
[
"Vatsya",
"S. R.",
""
]
] | The action principle is frequently used to derive the classical equations of motion. The action may also be used to associate group elements with curves in the space-time manifold, similar to the gauge transformations. The action principle is shown here to be an equivalence relation between the infinitesimal elements so defined for a collection of closed curves and the identity element. The action principle is then extended by requiring the equivalence of global elements with the identity and by considering all curves. The resulting equation is generalized further to include the non-Abelian gauge fields. The extended equation has an infinite number, but not all, trajectories as solutions. The properties of these paths are shown to impart wave-like properties to the particles in motion. These results provide an insight into the wave-particle duality and lead to a modified path-integral formalism. The motion of a particle is formulated within the resulting framework which yields a generalized Schrodinger equation. This equation is shown to reduce to a set of equations, one of them being the Klein-Gordon equation. |
gr-qc/9312038 | Sergey Tertychniy | S.Tertychniy | On the alternative description of complex holomorphic and Lorentz
geometries in four dimensions | 29 pages, uuencoded compressed PostScript, no local # | null | null | null | gr-qc | null | The equivalence of a conformal metric on 4-dimensional space-time and a local
field of 3-dimensional subspaces of the space of 2-forms over space-time is
discussed and the basic notion of transection is introduced. Corresponding
relation is spread to the metric case in terms of notion of normalized ordered
oriented transection field. As a result, one obtains a possibility to handle
the metric geometry without any references to the metric tensor itself on a
distinct base which nevertheless contains all the information on metricity.
Moreover, the notion of space-time curvature is provided with its natural
counterpart in the transection `language' in a form of curvature endomorphism
as well. To globalize the local constructions introduced, a certain fiber
bundle is defined whose sections are equivalent to normalized ordered oriented
transection fields and locally to the metric tensor on space-time. The
criterion distinguishing the Lorentz geometry is discussed. The resulting
alternative method of the description of space-time metricity, dealing with
exterior forms foliation alone, seems to be of a power compatible with one of
the standard concept based on the metric tensor.
| [
{
"created": "Wed, 29 Dec 1993 18:29:23 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Tertychniy",
"S.",
""
]
] | The equivalence of a conformal metric on 4-dimensional space-time and a local field of 3-dimensional subspaces of the space of 2-forms over space-time is discussed and the basic notion of transection is introduced. Corresponding relation is spread to the metric case in terms of notion of normalized ordered oriented transection field. As a result, one obtains a possibility to handle the metric geometry without any references to the metric tensor itself on a distinct base which nevertheless contains all the information on metricity. Moreover, the notion of space-time curvature is provided with its natural counterpart in the transection `language' in a form of curvature endomorphism as well. To globalize the local constructions introduced, a certain fiber bundle is defined whose sections are equivalent to normalized ordered oriented transection fields and locally to the metric tensor on space-time. The criterion distinguishing the Lorentz geometry is discussed. The resulting alternative method of the description of space-time metricity, dealing with exterior forms foliation alone, seems to be of a power compatible with one of the standard concept based on the metric tensor. |
1710.02185 | LVC Publications | The LIGO Scientific Collaboration and the Virgo Collaboration: B. P.
Abbott, R. Abbott, T. D. Abbott, M. R. Abernathy, F. Acernese, K. Ackley, C.
Adams, T. Adams, P. Addesso, R. X. Adhikari, V. B. Adya, C. Affeldt, M.
Agathos, K. Agatsuma, N. Aggarwal, O. D. Aguiar, L. Aiello, A. Ain, B. Allen,
A. Allocca, P. A. Altin, S. B. Anderson, W. G. Anderson, K. Arai, M. C.
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Bustillo, T. Callister, E. Calloni, J. B. Camp, K. C. Cannon, J. Cao, C. D.
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B. Cepeda, L. Cerboni Baiardi, G. Cerretani, E. Cesarini, S. J. Chamberlin,
M. Chan, S. Chao, P. Charlton, E. Chassande-Mottin, B. D. Cheeseboro, H. Y.
Chen, Y. Chen, C. Cheng, A. Chincarini, A. Chiummo, H. S. Cho, M. Cho, J. H.
Chow, N. Christensen, Q. Chu, S. Chua, S. Chung, G. Ciani, F. Clara, J. A.
Clark, F. Cleva, E. Coccia, P.-F. Cohadon, A. Colla, C. G. Collette, L.
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Cornish, A. Corsi, S. Cortese, C. A. Costa, M. W. Coughlin, S. B. Coughlin,
J.-P. Coulon, S. T. Countryman, P. Couvares, E. E. Cowan, D. M. Coward, M. J.
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Silva Costa, V. Dattilo, I. Dave, M. Davier, G. S. Davies, E. J. Daw, R. Day,
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W. Del Pozzo, T. Denker, T. Dent, V. Dergachev, R. De Rosa, R. T. DeRosa, R.
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Giovanni, T. Di Girolamo, A. Di Lieto, S. Di Pace, I. Di Palma, A. Di
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Geng, E. Genin, A. Gennai, J. George, L. Gergely, V. Germain, Abhirup Ghosh,
Archisman Ghosh, S. Ghosh, J. A. Giaime, K. D. Giardina, A. Giazotto, K.
Gill, A. Glaefke, E. Goetz, R. Goetz, L. Gondan, G. Gonz'alez, J. M. Gonzalez
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Gosselin, R. Gouaty, A. Grado, C. Graef, P. B. Graff, M. Granata, A. Grant,
S. Gras, C. Gray, G. Greco, A. C. Green, P. Groot, H. Grote, S. Grunewald, G.
M. Guidi, X. Guo, A. Gupta, M. K. Gupta, K. E. Gushwa, E. K. Gustafson, R.
Gustafson, J. J. Hacker, B. R. Hall, E. D. Hall, G. Hammond, M. Haney, M. M.
Hanke, J. Hanks, M. D. Hannam, J. Hanson, T. Hardwick, J. Harms, G. M. Harry,
I. W. Harry, M. J. Hart, M. T. Hartman, C.-J. Haster, K. Haughian, A.
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Heng, J. Hennig, J. Henry, A. W. Heptonstall, M. Heurs, S. Hild, D. Hoak, D.
Hofman, K. Holt, D. E. Holz, P. Hopkins, J. Hough, E. A. Houston, E. J.
Howell, Y. M. Hu, S. Huang, E. A. Huerta, D. Huet, B. Hughey, S. Husa, S. H.
Huttner, T. Huynh-Dinh, N. Indik, D. R. Ingram, R. Inta, H. N. Isa, J.-M.
Isac, M. Isi, T. Isogai, B. R. Iyer, K. Izumi, T. Jacqmin, H. Jang, K. Jani,
P. Jaranowski, S. Jawahar, L. Jian, F. Jim'enez-Forteza, W. W. Johnson, D. I.
Jones, R. Jones, R. J. G. Jonker, L. Ju, Haris K, C. V. Kalaghatgi, V.
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S. Karvinen, M. Kasprzack, E. Katsavounidis, W. Katzman, S. Kaufer, T. Kaur,
K. Kawabe, F. K'ef'elian, M. S. Kehl, D. Keitel, D. B. Kelley, W. Kells, R.
Kennedy, J. S. Key, F. Y. Khalili, I. Khan, S. Khan, Z. Khan, E. A. Khazanov,
N. Kijbunchoo, Chi-Woong Kim, Chunglee Kim, J. Kim, K. Kim, N. Kim, W. Kim,
Y.-M. Kim, S. J. Kimbrell, E. J. King, P. J. King, J. S. Kissel, B. Klein, L.
Kleybolte, S. Klimenko, S. M. Koehlenbeck, S. Koley, V. Kondrashov, A.
Kontos, M. Korobko, W. Z. Korth, I. Kowalska, D. B. Kozak, V. Kringel, B.
Krishnan, A. Kr'olak, C. Krueger, G. Kuehn, P. Kumar, R. Kumar, L. Kuo, A.
Kutynia, B. D. Lackey, M. Landry, J. Lange, B. Lantz, P. D. Lasky, M. Laxen,
A. Lazzarini, C. Lazzaro, P. Leaci, S. Leavey, E. O. Lebigot, C. H. Lee, H.
K. Lee, H. M. Lee, K. Lee, A. Lenon, M. Leonardi, J. R. Leong, N. Leroy, N.
Letendre, Y. Levin, J. B. Lewis, T. G. F. Li, A. Libson, T. B. Littenberg, N.
A. Lockerbie, A. L. Lombardi, L. T. London, J. E. Lord, M. Lorenzini, V.
Loriette, M. Lormand, G. Losurdo, J. D. Lough, H. L"uck, A. P. Lundgren, R.
Lynch, Y. Ma, B. Machenschalk, M. MacInnis, D. M. Macleod, F.
Maga\~na-Sandoval, L. Maga\~na Zertuche, R. M. Magee, E. Majorana, I.
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S. Mastrogiovanni, F. Matichard, L. Matone, N. Mavalvala, N. Mazumder, R.
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McIver, D. J. McManus, T. McRae, S. T. McWilliams, D. Meacher, G. D. Meadors,
J. Meidam, A. Melatos, G. Mendell, R. A. Mercer, E. L. Merilh, M. Merzougui,
S. Meshkov, C. Messenger, C. Messick, R. Metzdorff, P. M. Meyers, F. Mezzani,
H. Miao, C. Michel, H. Middleton, E. E. Mikhailov, L. Milano, A. L. Miller,
A. Miller, B. B. Miller, J. Miller, M. Millhouse, Y. Minenkov, J. Ming, S.
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S. M. Scott, D. Sellers, A. S. Sengupta, D. Sentenac, V. Sequino, A. Sergeev,
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Vardaro, S. Vass, M. Vas'uth, R. Vaulin, A. Vecchio, G. Vedovato, J. Veitch,
P. J. Veitch, K. Venkateswara, D. Verkindt, F. Vetrano, A. Vicer'e, S.
Vinciguerra, D. J. Vine, J.-Y. Vinet, S. Vitale, T. Vo, H. Vocca, C. Vorvick,
D. V. Voss, W. D. Vousden, S. P. Vyatchanin, A. R. Wade, L. E. Wade, M. Wade,
M. Walker, L. Wallace, S. Walsh, G. Wang, H. Wang, M. Wang, X. Wang, Y. Wang,
R. L. Ward, J. Warner, M. Was, B. Weaver, L.-W. Wei, M. Weinert, A. J.
Weinstein, R. Weiss, L. Wen, P. Wessels, T. Westphal, K. Wette, J. T. Whelan,
B. F. Whiting, 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. Worden,
J. L. Wright, D. S. Wu, G. Wu, J. Yablon, W. Yam, H. Yamamoto, C. C. Yancey,
H. Yu, M. Yvert, A. Zadro.zny, L. Zangrando, M. Zanolin, J.-P. Zendri, M.
Zevin, L. Zhang, M. Zhang, Y. Zhang, C. Zhao, M. Zhou, Z. Zhou, X. J. Zhu, M.
E. Zucker, S. E. Zuraw, J. Zweizig | Effects of Data Quality Vetoes on a Search for Compact Binary
Coalescences in Advanced LIGO's First Observing Run | 27 pages, 13 figures, published version | Class. Quantum Grav. 35 065010 (2018) | 10.1088/1361-6382/aaaafa | null | gr-qc astro-ph.IM | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The first observing run of Advanced LIGO spanned 4 months, from September 12,
2015 to January 19, 2016, during which gravitational waves were directly
detected from two binary black hole systems, namely GW150914 and GW151226.
Confident detection of gravitational waves requires an understanding of
instrumental transients and artifacts that can reduce the sensitivity of a
search. Studies of the quality of the detector data yield insights into the
cause of instrumental artifacts and data quality vetoes specific to a search
are produced to mitigate the effects of problematic data. In this paper, the
systematic removal of noisy data from analysis time is shown to improve the
sensitivity of searches for compact binary coalescences. The output of the
PyCBC pipeline, which is a python-based code package used to search for
gravitational wave signals from compact binary coalescences, is used as a
metric for improvement. GW150914 was a loud enough signal that removing noisy
data did not improve its significance. However, the removal of data with excess
noise decreased the false alarm rate of GW151226 by more than two orders of
magnitude, from 1 in 770 years to less than 1 in 186000 years.
| [
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"Thomas",
"M.",
""
],
[
"Thomas",
"P.",
""
],
[
"Thorne",
"K. A.",
""
],
[
"Thrane",
"E.",
""
],
[
"Tiwari",
"S.",
""
],
[
"Tiwari",
"V.",
""
],
[
"Tokmakov",
"K. V.",
""
],
[
"Toland",
"K.",
""
],
[
"Tomlinson",
"C.",
""
],
[
"Tonelli",
"M.",
""
],
[
"Tornasi",
"Z.",
""
],
[
"Torres",
"C. V.",
""
],
[
"Torrie",
"C. I.",
""
],
[
"T\"oyr\"a",
"D.",
""
],
[
"Travasso",
"F.",
""
],
[
"Traylor",
"G.",
""
],
[
"Trifir`o",
"D.",
""
],
[
"Tringali",
"M. C.",
""
],
[
"Trozzo",
"L.",
""
],
[
"Tse",
"M.",
""
],
[
"Turconi",
"M.",
""
],
[
"Tuyenbayev",
"D.",
""
],
[
"Ugolini",
"D.",
""
],
[
"Unnikrishnan",
"C. S.",
""
],
[
"Urban",
"A. L.",
""
],
[
"Usman",
"S. A.",
""
],
[
"Vahlbruch",
"H.",
""
],
[
"Vajente",
"G.",
""
],
[
"Valdes",
"G.",
""
],
[
"van Bakel",
"N.",
""
],
[
"van Beuzekom",
"M.",
""
],
[
"Brand",
"J. F. J. van den",
""
],
[
"Broeck",
"C. Van Den",
""
],
[
"Vander-Hyde",
"D. C.",
""
],
[
"van der Schaaf",
"L.",
""
],
[
"van Heijningen",
"J. V.",
""
],
[
"van Veggel",
"A. A.",
""
],
[
"Vardaro",
"M.",
""
],
[
"Vass",
"S.",
""
],
[
"Vas'uth",
"M.",
""
],
[
"Vaulin",
"R.",
""
],
[
"Vecchio",
"A.",
""
],
[
"Vedovato",
"G.",
""
],
[
"Veitch",
"J.",
""
],
[
"Veitch",
"P. J.",
""
],
[
"Venkateswara",
"K.",
""
],
[
"Verkindt",
"D.",
""
],
[
"Vetrano",
"F.",
""
],
[
"Vicer'e",
"A.",
""
],
[
"Vinciguerra",
"S.",
""
],
[
"Vine",
"D. J.",
""
],
[
"Vinet",
"J. -Y.",
""
],
[
"Vitale",
"S.",
""
],
[
"Vo",
"T.",
""
],
[
"Vocca",
"H.",
""
],
[
"Vorvick",
"C.",
""
],
[
"Voss",
"D. V.",
""
],
[
"Vousden",
"W. D.",
""
],
[
"Vyatchanin",
"S. P.",
""
],
[
"Wade",
"A. R.",
""
],
[
"Wade",
"L. E.",
""
],
[
"Wade",
"M.",
""
],
[
"Walker",
"M.",
""
],
[
"Wallace",
"L.",
""
],
[
"Walsh",
"S.",
""
],
[
"Wang",
"G.",
""
],
[
"Wang",
"H.",
""
],
[
"Wang",
"M.",
""
],
[
"Wang",
"X.",
""
],
[
"Wang",
"Y.",
""
],
[
"Ward",
"R. L.",
""
],
[
"Warner",
"J.",
""
],
[
"Was",
"M.",
""
],
[
"Weaver",
"B.",
""
],
[
"Wei",
"L. -W.",
""
],
[
"Weinert",
"M.",
""
],
[
"Weinstein",
"A. J.",
""
],
[
"Weiss",
"R.",
""
],
[
"Wen",
"L.",
""
],
[
"Wessels",
"P.",
""
],
[
"Westphal",
"T.",
""
],
[
"Wette",
"K.",
""
],
[
"Whelan",
"J. T.",
""
],
[
"Whiting",
"B. F.",
""
],
[
"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.",
""
],
[
"Worden",
"J.",
""
],
[
"Wright",
"J. L.",
""
],
[
"Wu",
"D. S.",
""
],
[
"Wu",
"G.",
""
],
[
"Yablon",
"J.",
""
],
[
"Yam",
"W.",
""
],
[
"Yamamoto",
"H.",
""
],
[
"Yancey",
"C. C.",
""
],
[
"Yu",
"H.",
""
],
[
"Yvert",
"M.",
""
],
[
"zny",
"A. Zadro.",
""
],
[
"Zangrando",
"L.",
""
],
[
"Zanolin",
"M.",
""
],
[
"Zendri",
"J. -P.",
""
],
[
"Zevin",
"M.",
""
],
[
"Zhang",
"L.",
""
],
[
"Zhang",
"M.",
""
],
[
"Zhang",
"Y.",
""
],
[
"Zhao",
"C.",
""
],
[
"Zhou",
"M.",
""
],
[
"Zhou",
"Z.",
""
],
[
"Zhu",
"X. J.",
""
],
[
"Zucker",
"M. E.",
""
],
[
"Zuraw",
"S. E.",
""
],
[
"Zweizig",
"J.",
""
]
] | The first observing run of Advanced LIGO spanned 4 months, from September 12, 2015 to January 19, 2016, during which gravitational waves were directly detected from two binary black hole systems, namely GW150914 and GW151226. Confident detection of gravitational waves requires an understanding of instrumental transients and artifacts that can reduce the sensitivity of a search. Studies of the quality of the detector data yield insights into the cause of instrumental artifacts and data quality vetoes specific to a search are produced to mitigate the effects of problematic data. In this paper, the systematic removal of noisy data from analysis time is shown to improve the sensitivity of searches for compact binary coalescences. The output of the PyCBC pipeline, which is a python-based code package used to search for gravitational wave signals from compact binary coalescences, is used as a metric for improvement. GW150914 was a loud enough signal that removing noisy data did not improve its significance. However, the removal of data with excess noise decreased the false alarm rate of GW151226 by more than two orders of magnitude, from 1 in 770 years to less than 1 in 186000 years. |
2212.10491 | Bernardo Araneda | Bernardo Araneda | Twistor quadrics and black holes | 7 pages | null | null | null | gr-qc hep-th | http://creativecommons.org/licenses/by/4.0/ | A simple procedure is given to construct curved, non-self-dual (complexified)
Kaehler metrics on space-time in terms of deformations of holomorphic quadric
surfaces in flat twistor space. Imposing Lorentzian reality conditions, the
Schwarzschild, Kerr, and Plebanski-Demianski space-times (among others) are
derived as examples of the construction.
| [
{
"created": "Tue, 20 Dec 2022 18:06:31 GMT",
"version": "v1"
}
] | 2022-12-21 | [
[
"Araneda",
"Bernardo",
""
]
] | A simple procedure is given to construct curved, non-self-dual (complexified) Kaehler metrics on space-time in terms of deformations of holomorphic quadric surfaces in flat twistor space. Imposing Lorentzian reality conditions, the Schwarzschild, Kerr, and Plebanski-Demianski space-times (among others) are derived as examples of the construction. |
2002.00042 | Mert Mangut | O. Gurtug, M. Mangut and M. Halilsoy | Gravitational Lensing in Rotating and Twisting Universes | null | Astroparticle Physics, Volume 128, March 2021, 102558 | 10.1016/j.astropartphys.2021.102558 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Gravitational lensing caused by the gravitational field of massive objects
has been studied and acknowledged for a long period of time. In this paper,
however, we propose a different mechanism where the bending of light stems from
the non-linear interaction of gravitational, electromagnetic and axion waves
that creates the high curvature zone in the space-time fabric. The striking
distinction in the present study is that in contrast to the convex lensing in
the gravitational field of a massive object, hyperbolic nature of the high
curvature zone of the background space-time may give rise to concave lensing.
Expectedly detection of this kind of lensing becomes possible through satellite
detectors.
| [
{
"created": "Fri, 31 Jan 2020 20:04:54 GMT",
"version": "v1"
},
{
"created": "Mon, 24 Aug 2020 18:21:26 GMT",
"version": "v2"
}
] | 2021-01-21 | [
[
"Gurtug",
"O.",
""
],
[
"Mangut",
"M.",
""
],
[
"Halilsoy",
"M.",
""
]
] | Gravitational lensing caused by the gravitational field of massive objects has been studied and acknowledged for a long period of time. In this paper, however, we propose a different mechanism where the bending of light stems from the non-linear interaction of gravitational, electromagnetic and axion waves that creates the high curvature zone in the space-time fabric. The striking distinction in the present study is that in contrast to the convex lensing in the gravitational field of a massive object, hyperbolic nature of the high curvature zone of the background space-time may give rise to concave lensing. Expectedly detection of this kind of lensing becomes possible through satellite detectors. |
2012.00549 | Ayyesha Ahmed | Ayyesha K. Ahmed and Azad A. Siddiqui | Weak Cosmic Censorship by Overspinning the Kerr-Newman-Kasuya Black Hole
with Test Particle | 4 pages | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We check the weak cosmic censorship conjecture by attempting to overspin the
Kerr-Newman-Kasuya black hole with test particle. The study suggests that the
Kerr-Newman-Kasuya black hole can be over-spun showing the violation of cosmic
censorship conjecture.
| [
{
"created": "Wed, 25 Nov 2020 08:30:14 GMT",
"version": "v1"
}
] | 2020-12-02 | [
[
"Ahmed",
"Ayyesha K.",
""
],
[
"Siddiqui",
"Azad A.",
""
]
] | We check the weak cosmic censorship conjecture by attempting to overspin the Kerr-Newman-Kasuya black hole with test particle. The study suggests that the Kerr-Newman-Kasuya black hole can be over-spun showing the violation of cosmic censorship conjecture. |
1707.02399 | Claudio Cremaschini | Claudio Cremaschini and Massimo Tessarotto | Quantum-wave equation and Heisenberg inequalities of covariant quantum
gravity | Entropy Journal Special Issue: Advances in Relativistic Statistical
Mechanics | Entropy 19, 339 (2017) | 10.3390/e19070339 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Key aspects of the manifestly-covariant theory of quantum gravity
(Cremaschini and Tessarotto 2015-2017) are investigated. These refer, first, to
the establishment of the 4-scalar, manifestly-covariant evolution quantum wave
equation, denoted as covariant quantum gravity (CQG) wave equation, which
advances the quantum state $\psi $ associated with a prescribed background
space-time. In this paper, the CQG-wave equation is proved to follow at once by
means of a Hamilton-Jacobi quantization of the classical variational tensor
field $g\equiv \left\{ g_{\mu \nu }\right\} $ and its conjugate momentum,
referred to as (canonical) $g-$quantization. The same equation is also shown to
be variational and to follow from a synchronous variational principle
identified here with the quantum Hamilton variational principle. The
corresponding quantum hydrodynamic equations are then obtained upon introducing
the Madelung representation for $\psi $, which provide an equivalent
statistical interpretation of the CQG-wave equation. Finally, the quantum state
$\psi $ is proved to fulfill generalized Heisenberg inequalities, relating the
statistical measurement errors of quantum observables. These are shown to be
represented in terms of the standard deviations of the matric tensor $g\equiv
\left\{ g_{\mu \nu }\right\} $ and its quantum conjugate momentum operator.
| [
{
"created": "Sat, 8 Jul 2017 05:58:28 GMT",
"version": "v1"
}
] | 2017-07-11 | [
[
"Cremaschini",
"Claudio",
""
],
[
"Tessarotto",
"Massimo",
""
]
] | Key aspects of the manifestly-covariant theory of quantum gravity (Cremaschini and Tessarotto 2015-2017) are investigated. These refer, first, to the establishment of the 4-scalar, manifestly-covariant evolution quantum wave equation, denoted as covariant quantum gravity (CQG) wave equation, which advances the quantum state $\psi $ associated with a prescribed background space-time. In this paper, the CQG-wave equation is proved to follow at once by means of a Hamilton-Jacobi quantization of the classical variational tensor field $g\equiv \left\{ g_{\mu \nu }\right\} $ and its conjugate momentum, referred to as (canonical) $g-$quantization. The same equation is also shown to be variational and to follow from a synchronous variational principle identified here with the quantum Hamilton variational principle. The corresponding quantum hydrodynamic equations are then obtained upon introducing the Madelung representation for $\psi $, which provide an equivalent statistical interpretation of the CQG-wave equation. Finally, the quantum state $\psi $ is proved to fulfill generalized Heisenberg inequalities, relating the statistical measurement errors of quantum observables. These are shown to be represented in terms of the standard deviations of the matric tensor $g\equiv \left\{ g_{\mu \nu }\right\} $ and its quantum conjugate momentum operator. |
1412.0005 | Pierre-Henri Chavanis | Pierre-Henri Chavanis | Relativistic self-gravitating Bose-Einstein condensates and cold baryons
with a stiff equation of state | null | Eur. Phys. J. Plus 130, 181 (2015) | 10.1140/epjp/i2015-15181-6 | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Because of their superfluid properties, some compact astrophysical objects
such as neutron stars may contain a significant part of their matter in the
form of a Bose-Einstein condensate (BEC). We consider a partially-relativistic
model of self-gravitating BECs where the relation between the pressure and the
rest-mass density is assumed to be quadratic (as in the case of classical BECs)
but pressure effects are taken into account in the relation between the energy
density and the rest-mass density. At high densities, we get a stiff equation
of state similar to the one considered by Zel'dovich (1961) in the context of
baryon stars in which the baryons interact through a vector meson field. We
determine the maximum mass of general relativistic BEC stars described by this
equation of state by using the formalism of Tooper (1965). This maximum mass is
slightly larger than the maximum mass obtained by Chavanis and Harko (2012)
using a fully-relativistic model. We also consider the possibility that dark
matter is made of BECs and apply the partially-relativistic model of BECs to
cosmology. In this model, we show that the universe experiences a stiff matter
phase, followed by a dust matter phase, and finally by a dark energy phase
(equivalent to a cosmological constant). The same evolution is obtained in
Zel'dovich (1972) model which assumes that initially, near the cosmological
singularity, the universe is filled with cold baryons. Interestingly, the
Friedmann equations can be solved analytically in that case and provide a
simple generalization of the $\Lambda$CDM model. We point out, however, the
limitations of the partially-relativistic model for BECs and show the need for
a fully-relativistic one.
| [
{
"created": "Thu, 27 Nov 2014 16:14:37 GMT",
"version": "v1"
}
] | 2016-07-12 | [
[
"Chavanis",
"Pierre-Henri",
""
]
] | Because of their superfluid properties, some compact astrophysical objects such as neutron stars may contain a significant part of their matter in the form of a Bose-Einstein condensate (BEC). We consider a partially-relativistic model of self-gravitating BECs where the relation between the pressure and the rest-mass density is assumed to be quadratic (as in the case of classical BECs) but pressure effects are taken into account in the relation between the energy density and the rest-mass density. At high densities, we get a stiff equation of state similar to the one considered by Zel'dovich (1961) in the context of baryon stars in which the baryons interact through a vector meson field. We determine the maximum mass of general relativistic BEC stars described by this equation of state by using the formalism of Tooper (1965). This maximum mass is slightly larger than the maximum mass obtained by Chavanis and Harko (2012) using a fully-relativistic model. We also consider the possibility that dark matter is made of BECs and apply the partially-relativistic model of BECs to cosmology. In this model, we show that the universe experiences a stiff matter phase, followed by a dust matter phase, and finally by a dark energy phase (equivalent to a cosmological constant). The same evolution is obtained in Zel'dovich (1972) model which assumes that initially, near the cosmological singularity, the universe is filled with cold baryons. Interestingly, the Friedmann equations can be solved analytically in that case and provide a simple generalization of the $\Lambda$CDM model. We point out, however, the limitations of the partially-relativistic model for BECs and show the need for a fully-relativistic one. |
2101.08617 | Jan Ambjorn | J. Ambjorn, Z. Drogosz, J. Gizbert-Studnicki, A. G\"orlich, J.
Jurkiewicz and D. N\'emeth | Cosmic voids and filaments from quantum gravity | 4 pages, 2 figures | null | 10.1140/epjc/s10052-021-09468-z | null | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Using computer simulations we study the geometry of a typical quantum
universe, i.e. the geometry one might expect before a possible period of
inflation. We display it using coordinates defined by means of four classical
scalar fields satisfying the Laplace equation with non-trivial boundary
conditions. The field configurations reveal cosmic web structures surprisingly
similar to the ones observed in the present-day Universe. Inflation might make
these structures relevant for our Universe.
| [
{
"created": "Thu, 21 Jan 2021 14:00:06 GMT",
"version": "v1"
}
] | 2021-09-01 | [
[
"Ambjorn",
"J.",
""
],
[
"Drogosz",
"Z.",
""
],
[
"Gizbert-Studnicki",
"J.",
""
],
[
"Görlich",
"A.",
""
],
[
"Jurkiewicz",
"J.",
""
],
[
"Németh",
"D.",
""
]
] | Using computer simulations we study the geometry of a typical quantum universe, i.e. the geometry one might expect before a possible period of inflation. We display it using coordinates defined by means of four classical scalar fields satisfying the Laplace equation with non-trivial boundary conditions. The field configurations reveal cosmic web structures surprisingly similar to the ones observed in the present-day Universe. Inflation might make these structures relevant for our Universe. |
1112.1341 | Felipe Falciano | F. T. Falciano and E. Goulart | A new symmetry of the relativistic wave equation | 4 pages | Class.Quant.Grav. 29 (2012) 085011 | 10.1088/0264-9381/29/8/085011 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper we show that there exists a new symmetry in the relativistic
wave equation for a scalar field in arbitrary dimensions. This symmetry is
related to redefinitions of the metric tensor which implement a map between
non-equivalent manifolds. It is possible to interpret these transformations as
a generalization of the conformal transformations. In addition, one can show
that this set of manifolds together with the transformation connecting its
metrics forms a group. As long as the scalar field dynamics is invariant under
these transformations, there immediately appears an ambiguity concerning the
definition of the underlying background geometry.
| [
{
"created": "Tue, 6 Dec 2011 16:38:41 GMT",
"version": "v1"
}
] | 2012-08-29 | [
[
"Falciano",
"F. T.",
""
],
[
"Goulart",
"E.",
""
]
] | In this paper we show that there exists a new symmetry in the relativistic wave equation for a scalar field in arbitrary dimensions. This symmetry is related to redefinitions of the metric tensor which implement a map between non-equivalent manifolds. It is possible to interpret these transformations as a generalization of the conformal transformations. In addition, one can show that this set of manifolds together with the transformation connecting its metrics forms a group. As long as the scalar field dynamics is invariant under these transformations, there immediately appears an ambiguity concerning the definition of the underlying background geometry. |
1909.12607 | Bibhas Majhi Ranjan | Avijit Bera, Subir Ghosh, Bibhas Ranjan Majhi | Hawking radiation in a non-covariant frame: the Jacobi metric approach | Typos corrected, to appear in Eur. Phys. J. Plus | Eur. Phys. J. Plus 135 (2020) 670 | 10.1140/epjp/s13360-020-00693-1 | null | gr-qc hep-th quant-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The present paper deals with a reformulation of the derivation of Hawking
temperature for static and stationary black holes. In contrast to the
conventional approach, where the covariant form of the metrics are used, we use
the manifestly non-covariant Jacobi metric for the black holes in question. In
the latter, a restricted form of Hamilton-Jacobi variational principle is
exploited where the energy of the particle (pertaining to Hawking radiation)
appears explicitly in the metric as a constant parameter. Our analysis shows
that, as far as computation of Hawking temperature (for stationary black holes)
is concerned, the Jacobi metric framework is more streamlined and yields the
result with less amount of complications, (as for example, considerations of
positive and negative energy modes and signature change of the metric across
horizon do not play any direct role in the present analysis).
| [
{
"created": "Fri, 27 Sep 2019 10:37:35 GMT",
"version": "v1"
},
{
"created": "Thu, 13 Aug 2020 06:58:16 GMT",
"version": "v2"
}
] | 2020-08-24 | [
[
"Bera",
"Avijit",
""
],
[
"Ghosh",
"Subir",
""
],
[
"Majhi",
"Bibhas Ranjan",
""
]
] | The present paper deals with a reformulation of the derivation of Hawking temperature for static and stationary black holes. In contrast to the conventional approach, where the covariant form of the metrics are used, we use the manifestly non-covariant Jacobi metric for the black holes in question. In the latter, a restricted form of Hamilton-Jacobi variational principle is exploited where the energy of the particle (pertaining to Hawking radiation) appears explicitly in the metric as a constant parameter. Our analysis shows that, as far as computation of Hawking temperature (for stationary black holes) is concerned, the Jacobi metric framework is more streamlined and yields the result with less amount of complications, (as for example, considerations of positive and negative energy modes and signature change of the metric across horizon do not play any direct role in the present analysis). |
gr-qc/0405138 | Chengmin Zhang | C.M. Zhang | Dirac Spin Precession in Kerr Spacetime by the parallelism description | 6 pages | Commun.Theor.Phys. 44 (2005) 279-286 | null | null | gr-qc | null | In the framework of parallelism general relativity (PGR), the Dirac particle
spin precession in the rotational gravitational field is studied. In terms of
the equivalent tetrad of Kerr frame, we investigate the torsion axial-vector
spin coupling in PGR. In the case of the weak field and slow rotation
approximation, we obtain that the torsion axial-vector has the dipole-like
structure, but different from the gravitomagnetic field, which indicates that
the choice of the Kerr tetrad will influence on the physics interpretation of
the axial-vector spin coupling.
| [
{
"created": "Fri, 28 May 2004 14:22:08 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Zhang",
"C. M.",
""
]
] | In the framework of parallelism general relativity (PGR), the Dirac particle spin precession in the rotational gravitational field is studied. In terms of the equivalent tetrad of Kerr frame, we investigate the torsion axial-vector spin coupling in PGR. In the case of the weak field and slow rotation approximation, we obtain that the torsion axial-vector has the dipole-like structure, but different from the gravitomagnetic field, which indicates that the choice of the Kerr tetrad will influence on the physics interpretation of the axial-vector spin coupling. |
1110.6794 | Gustav Holzegel | Gustav Holzegel and Jacques Smulevici | Decay properties of Klein-Gordon fields on Kerr-AdS spacetimes | 47 pages, 1 figure; typos corrected, minor improvement of the results | null | null | null | gr-qc hep-th math.AP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | This paper investigates the decay properties of solutions to the massive
linear wave equation $\Box_g \psi + \frac{{\alpha}}{l^2} \psi =0$ for $g$ the
metric of a Kerr-AdS spacetime satisfying $|a|l<r_+^2$ and $\alpha<9/4$
satisfying the Breitenlohner Freedman bound. We prove that the non-degenerate
energy of $\psi$ with respect to an appropriate foliation of spacelike slices
decays like $(\log t^\star)^{-2}$. Our estimates are expected to be sharp from
heuristic and numerical arguments in the physics literature suggesting that
general solutions will only decay logarithmically. The underlying reason for
the slow decay rate can be traced back to a stable trapping phenomenon for
asymptotically anti de Sitter black holes which is in turn a consequence of the
reflecting boundary conditions for $\psi$ at null-infinity.
| [
{
"created": "Mon, 31 Oct 2011 13:49:19 GMT",
"version": "v1"
},
{
"created": "Sat, 23 Mar 2013 13:21:28 GMT",
"version": "v2"
}
] | 2013-03-26 | [
[
"Holzegel",
"Gustav",
""
],
[
"Smulevici",
"Jacques",
""
]
] | This paper investigates the decay properties of solutions to the massive linear wave equation $\Box_g \psi + \frac{{\alpha}}{l^2} \psi =0$ for $g$ the metric of a Kerr-AdS spacetime satisfying $|a|l<r_+^2$ and $\alpha<9/4$ satisfying the Breitenlohner Freedman bound. We prove that the non-degenerate energy of $\psi$ with respect to an appropriate foliation of spacelike slices decays like $(\log t^\star)^{-2}$. Our estimates are expected to be sharp from heuristic and numerical arguments in the physics literature suggesting that general solutions will only decay logarithmically. The underlying reason for the slow decay rate can be traced back to a stable trapping phenomenon for asymptotically anti de Sitter black holes which is in turn a consequence of the reflecting boundary conditions for $\psi$ at null-infinity. |
2110.14452 | Maxime Jacquet | Maxime J Jacquet, Luca Giacomelli, Quentin Valnais, Malo Joly,
Ferdinand Claude, Elisabeth Giacobino, Quentin Glorieux, Iacopo Carusotto and
Alberto Bramati | Quantum vacuum excitation of a quasi-normal mode in an analog model of
black hole spacetime | Version accepted for publication | null | 10.1103/PhysRevLett.130.111501 | null | gr-qc quant-ph | http://creativecommons.org/licenses/by-nc-sa/4.0/ | Vacuum quantum fluctuations near horizons are known to yield correlated
emission by the Hawking effect. We use a driven-dissipative quantum fluid of
microcavity polaritons as an analog model of a quantum field theory on a
black-hole spacetime and numerically calculate correlated emission. We show
that, in addition to the Hawking effect at the sonic horizon, quantum
fluctuations may result in a sizeable stationary excitation of a quasi-normal
mode of the field theory. Observable signatures of the excitation of the
quasi-normal mode are found in the spatial density fluctuations as well as in
the spectrum of Hawking emission. This suggests an intrinsic fluctuation-driven
mechanism leading to the quantum excitation of quasi-normal modes on black hole
spacetimes.
| [
{
"created": "Wed, 27 Oct 2021 14:16:12 GMT",
"version": "v1"
},
{
"created": "Fri, 11 Mar 2022 10:40:49 GMT",
"version": "v2"
},
{
"created": "Tue, 28 Feb 2023 08:46:57 GMT",
"version": "v3"
}
] | 2023-03-17 | [
[
"Jacquet",
"Maxime J",
""
],
[
"Giacomelli",
"Luca",
""
],
[
"Valnais",
"Quentin",
""
],
[
"Joly",
"Malo",
""
],
[
"Claude",
"Ferdinand",
""
],
[
"Giacobino",
"Elisabeth",
""
],
[
"Glorieux",
"Quentin",
""
],
[
"Carusotto",
"Iacopo",
""
],
[
"Bramati",
"Alberto",
""
]
] | Vacuum quantum fluctuations near horizons are known to yield correlated emission by the Hawking effect. We use a driven-dissipative quantum fluid of microcavity polaritons as an analog model of a quantum field theory on a black-hole spacetime and numerically calculate correlated emission. We show that, in addition to the Hawking effect at the sonic horizon, quantum fluctuations may result in a sizeable stationary excitation of a quasi-normal mode of the field theory. Observable signatures of the excitation of the quasi-normal mode are found in the spatial density fluctuations as well as in the spectrum of Hawking emission. This suggests an intrinsic fluctuation-driven mechanism leading to the quantum excitation of quasi-normal modes on black hole spacetimes. |
1408.2589 | Juan Carlos Degollado | Juan Carlos Degollado and Carlos A. R. Herdeiro | Wiggly tails: a gravitational wave signature of massive fields around
black holes | 6 pages, 4 figures | Phys. Rev. D 90, 065019 (2014) | 10.1103/PhysRevD.90.065019 | null | gr-qc astro-ph.HE hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Massive fields can exist in long-lived configurations around black holes. We
examine how the gravitational wave signal of a perturbed black hole is affected
by such `dirtiness' within linear theory. As a concrete example, we consider
the gravitational radiation emitted by the infall of a massive scalar field
into a Schwarzschild black hole. Whereas part of the scalar field is
absorbed/scattered by the black hole and triggers gravitational wave emission,
another part lingers in long-lived quasi-bound states. Solving numerically the
Teukolsky master equation for gravitational perturbations coupled to the
massive Klein-Gordon equation, we find a characteristic gravitational wave
signal, composed by a quasi-normal ringing followed by a late time tail. In
contrast to `clean' black holes, however, the late time tail contains small
amplitude wiggles with the frequency of the dominating quasi-bound state.
Additionally, an observer dependent beating pattern may also be seen. These
features were already observed in fully non-linear studies; our analysis shows
they are present at linear level, and, since it reduces to a 1+1 dimensional
numerical problem, allows for cleaner numerical data. Moreover, we discuss the
power law of the tail and that it only becomes universal sufficiently far away
from the `dirty' black hole. The wiggly tails, by constrast, are a generic
feature that may be used as a smoking gun for the presence of massive fields
around black holes, either as a linear cloud or as fully non-linear hair.
| [
{
"created": "Tue, 12 Aug 2014 00:29:43 GMT",
"version": "v1"
}
] | 2014-09-24 | [
[
"Degollado",
"Juan Carlos",
""
],
[
"Herdeiro",
"Carlos A. R.",
""
]
] | Massive fields can exist in long-lived configurations around black holes. We examine how the gravitational wave signal of a perturbed black hole is affected by such `dirtiness' within linear theory. As a concrete example, we consider the gravitational radiation emitted by the infall of a massive scalar field into a Schwarzschild black hole. Whereas part of the scalar field is absorbed/scattered by the black hole and triggers gravitational wave emission, another part lingers in long-lived quasi-bound states. Solving numerically the Teukolsky master equation for gravitational perturbations coupled to the massive Klein-Gordon equation, we find a characteristic gravitational wave signal, composed by a quasi-normal ringing followed by a late time tail. In contrast to `clean' black holes, however, the late time tail contains small amplitude wiggles with the frequency of the dominating quasi-bound state. Additionally, an observer dependent beating pattern may also be seen. These features were already observed in fully non-linear studies; our analysis shows they are present at linear level, and, since it reduces to a 1+1 dimensional numerical problem, allows for cleaner numerical data. Moreover, we discuss the power law of the tail and that it only becomes universal sufficiently far away from the `dirty' black hole. The wiggly tails, by constrast, are a generic feature that may be used as a smoking gun for the presence of massive fields around black holes, either as a linear cloud or as fully non-linear hair. |
2006.06734 | Carolina Benone | Leandro A. Oliveira, Carolina L. Benone, Amanda L. Almeida, Lu\'is C.
B. Crispino | Analytical investigation of wave absorption by a rotating black hole
analogue | 13 pages, 3 figures, Contribution to Selected Papers of the Fifth
Amazonian Symposium on Physics, accepted in IJMPD | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Perturbations in a draining vortex can be described analytically in terms of
confluent Heun functions. In the context of analogue models of gravity in ideal
fluids, we investigate analytically the absorption length of waves in a
draining bathtub, a rotating black hole analogue, using confluent Heun
functions. We compare our analytical results with the corresponding numerical
ones, obtaining excellent agreement.
| [
{
"created": "Thu, 11 Jun 2020 18:49:41 GMT",
"version": "v1"
}
] | 2020-06-15 | [
[
"Oliveira",
"Leandro A.",
""
],
[
"Benone",
"Carolina L.",
""
],
[
"Almeida",
"Amanda L.",
""
],
[
"Crispino",
"Luís C. B.",
""
]
] | Perturbations in a draining vortex can be described analytically in terms of confluent Heun functions. In the context of analogue models of gravity in ideal fluids, we investigate analytically the absorption length of waves in a draining bathtub, a rotating black hole analogue, using confluent Heun functions. We compare our analytical results with the corresponding numerical ones, obtaining excellent agreement. |
1802.06135 | Florian Hopfm\"uller | Florian Hopfm\"uller and Laurent Freidel | Null Conservation Laws for Gravity | 26 pages + appendices, comments welcome | Phys. Rev. D 97, 124029 (2018) | 10.1103/PhysRevD.97.124029 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We give a full analysis of the conservation along null surfaces of
generalized energy and super-momenta, for gravitational systems enclosed by a
finite boundary. In particular we interpret the conservation equations in a
canonical manner, revealing a notion of symplectic potential and a boundary
current intrinsic to null surfaces. This generalizes similar analyses done at
asymptotic infinity or on horizons.
| [
{
"created": "Fri, 16 Feb 2018 21:50:09 GMT",
"version": "v1"
}
] | 2018-06-20 | [
[
"Hopfmüller",
"Florian",
""
],
[
"Freidel",
"Laurent",
""
]
] | We give a full analysis of the conservation along null surfaces of generalized energy and super-momenta, for gravitational systems enclosed by a finite boundary. In particular we interpret the conservation equations in a canonical manner, revealing a notion of symplectic potential and a boundary current intrinsic to null surfaces. This generalizes similar analyses done at asymptotic infinity or on horizons. |
2111.05507 | Huiquan Li | Huiquan Li | Hawking-like radiation of charged particles via tunneling across the
lightcylinder of a rotating magnetosphere | 7 pages, no figure | null | 10.1016/j.physletb.2021.136816 | null | gr-qc astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In rotating magnetospheres planted on compact objects, there usually exist
lightcylinders (LC), beyond which the rotation speed of the magnetic field
lines exceeds the speed of light. The LC is a close analog to the horizon in
gravity, and is a casual boundary for charged particles that are restricted to
move along the magnetic field lines. In this work, it is proposed that there
should be Hawking-like radiation of charged particles from the LC of a rotating
magnetosphere from the point of view of tunneling by using the field sheet
metric.
| [
{
"created": "Wed, 10 Nov 2021 03:13:50 GMT",
"version": "v1"
}
] | 2022-01-05 | [
[
"Li",
"Huiquan",
""
]
] | In rotating magnetospheres planted on compact objects, there usually exist lightcylinders (LC), beyond which the rotation speed of the magnetic field lines exceeds the speed of light. The LC is a close analog to the horizon in gravity, and is a casual boundary for charged particles that are restricted to move along the magnetic field lines. In this work, it is proposed that there should be Hawking-like radiation of charged particles from the LC of a rotating magnetosphere from the point of view of tunneling by using the field sheet metric. |
1801.08162 | Carlos O. Lousto | James Healy and Carlos O. Lousto | The hangup effect in unequal mass binary black hole mergers and further
studies of their gravitational radiation and remnant properties | 26 pages, 13 figures | Phys. Rev. D 97, 084002 (2018) | 10.1103/PhysRevD.97.084002 | null | gr-qc astro-ph.CO astro-ph.GA astro-ph.HE | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present the results of 74 new simulations of nonprecessing spinning black
hole binaries with mass ratios $q=m_1/m_2$ in the range $1/7\leq q\leq1$ and
individual spins covering the parameter space $-0.95\leq\alpha_{1,2}\leq0.95$
with one runs with spins of $\pm0.95$. We supplement those runs with 107
previous simulations to study the hangup effect in black hole mergers, i.e. the
delay or prompt merger of spinning holes with respect to non spinning binaries.
We perform the numerical evolution for typically the last ten orbits before the
merger and down to the formation of the final remnant black hole. This allows
us to study the hangup effect for unequal mass binaries leading us to identify
the spin variable that controls the number of orbits before merger as
$\vec{S}_{hu}\cdot{\hat{L}},$ where
$\vec{S}_{hu}=(1+\frac12\frac{m_2}{m_1})\vec{S}_1+(1+\frac12\frac{m_1}{m_2})\vec{S}_2$.
We also combine the total results of those 181 simulations to obtain improved
fitting formulae for the remnant final black hole mass, spin and recoil
velocity as well as for the peak luminosity and peak frequency of the
gravitational strain, and find new correlations among them. This accurate new
set of simulations enhances the number of available numerical relativity
waveforms available for parameter estimation of gravitational wave
observations.
| [
{
"created": "Wed, 24 Jan 2018 19:45:08 GMT",
"version": "v1"
}
] | 2018-04-11 | [
[
"Healy",
"James",
""
],
[
"Lousto",
"Carlos O.",
""
]
] | We present the results of 74 new simulations of nonprecessing spinning black hole binaries with mass ratios $q=m_1/m_2$ in the range $1/7\leq q\leq1$ and individual spins covering the parameter space $-0.95\leq\alpha_{1,2}\leq0.95$ with one runs with spins of $\pm0.95$. We supplement those runs with 107 previous simulations to study the hangup effect in black hole mergers, i.e. the delay or prompt merger of spinning holes with respect to non spinning binaries. We perform the numerical evolution for typically the last ten orbits before the merger and down to the formation of the final remnant black hole. This allows us to study the hangup effect for unequal mass binaries leading us to identify the spin variable that controls the number of orbits before merger as $\vec{S}_{hu}\cdot{\hat{L}},$ where $\vec{S}_{hu}=(1+\frac12\frac{m_2}{m_1})\vec{S}_1+(1+\frac12\frac{m_1}{m_2})\vec{S}_2$. We also combine the total results of those 181 simulations to obtain improved fitting formulae for the remnant final black hole mass, spin and recoil velocity as well as for the peak luminosity and peak frequency of the gravitational strain, and find new correlations among them. This accurate new set of simulations enhances the number of available numerical relativity waveforms available for parameter estimation of gravitational wave observations. |
2002.01663 | Hamid Reza Sepangi | A. Rahmani, M. Honardoost, H. R. Sepangi | Thermal phase transition in $F(R)$-charged $AdS_{4}$-scalar theory | 16 pages, 11 figures, to appear in PRD | Phys. Rev. D 101, 084036 (2020) | 10.1103/PhysRevD.101.084036 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We investigate instabilities of $F(R)$-charged $AdS_{4}$ black holes by a
massive charged scalar field in a linear perturbation regime. We study
tachyonic instabilities as the near horizon scalar condensation in a model of
$F(R)$ gravity with planar horizon and investigate properties of possible phase
transitions. The results show that such transitions are sensitive to the first
derivative of $F(R)$ with respect to $R$ in that the larger its value, the
higher the critical temperature, thus resulting in a new generation of
high-temperature superconductors. Also, for a certain range of parameters,
$F(R)$-charged $AdS_{4}$ black holes suffer from superradiant instability. We
consider the effects of the scalar mass and charge on such instabilities and
conclude that RN black holes decay into small hairy black holes that have a
charged scalar condensate floating near the horizon. It is shown that the
existence of phase transition at the critical temperature leading to a hairy
black hole solution emerges for $T<T_{c}$, while RN black holes exist for
$T>T_{c}$. The effect of $F(R)$ on the critical temperature is subsequently
investigated in the case of superradiant instability, showing that higher
critical temperatures would be possible in $F(R)$ gravity. We also check the
stability of hairy black holes and show that the resulting hairy solution can
be considered as a possible end point of superradiant instability of a small
charged black hole.
| [
{
"created": "Wed, 5 Feb 2020 06:56:27 GMT",
"version": "v1"
},
{
"created": "Sat, 4 Apr 2020 14:37:18 GMT",
"version": "v2"
}
] | 2020-04-22 | [
[
"Rahmani",
"A.",
""
],
[
"Honardoost",
"M.",
""
],
[
"Sepangi",
"H. R.",
""
]
] | We investigate instabilities of $F(R)$-charged $AdS_{4}$ black holes by a massive charged scalar field in a linear perturbation regime. We study tachyonic instabilities as the near horizon scalar condensation in a model of $F(R)$ gravity with planar horizon and investigate properties of possible phase transitions. The results show that such transitions are sensitive to the first derivative of $F(R)$ with respect to $R$ in that the larger its value, the higher the critical temperature, thus resulting in a new generation of high-temperature superconductors. Also, for a certain range of parameters, $F(R)$-charged $AdS_{4}$ black holes suffer from superradiant instability. We consider the effects of the scalar mass and charge on such instabilities and conclude that RN black holes decay into small hairy black holes that have a charged scalar condensate floating near the horizon. It is shown that the existence of phase transition at the critical temperature leading to a hairy black hole solution emerges for $T<T_{c}$, while RN black holes exist for $T>T_{c}$. The effect of $F(R)$ on the critical temperature is subsequently investigated in the case of superradiant instability, showing that higher critical temperatures would be possible in $F(R)$ gravity. We also check the stability of hairy black holes and show that the resulting hairy solution can be considered as a possible end point of superradiant instability of a small charged black hole. |
1203.4750 | Homer G. Ellis | Homer G. Ellis | Gravity Inside a Nonrotating, Homogeneous, Spherical Body | 6 pages, 1 figure, 5 references, REVTex 4.1; v2: final paragraph
changed to delete error, 3 references added | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Schwarzschild's 'interior solution' is a space-time metric that satisfies
Einstein's gravitational field equations with a source term that Einstein
created on the basis of an unjustified identification of the conceptually
distinct notions of the passive gravitational mass of matter and the active
gravitational mass of matter. Giving up that assumption allows deriving from a
variational principle new and better (because logically obtained) field
equations that more faithfully extend the Poisson equation for Newton's gravity
than do Einstein's, with an active gravitational mass density providing the
source term. Solving these equations for a nonrotating spherical ball of matter
with uniform mass density produces a new, improved interior metric matched at
the surface of the ball to Schwarzschild's 'exterior' solution metric. This new
metric can then be used to address questions about the flight times of photons
and neutrinos through such a ball of matter.
| [
{
"created": "Tue, 20 Mar 2012 19:27:04 GMT",
"version": "v1"
},
{
"created": "Tue, 16 Oct 2012 20:00:48 GMT",
"version": "v2"
}
] | 2012-10-18 | [
[
"Ellis",
"Homer G.",
""
]
] | Schwarzschild's 'interior solution' is a space-time metric that satisfies Einstein's gravitational field equations with a source term that Einstein created on the basis of an unjustified identification of the conceptually distinct notions of the passive gravitational mass of matter and the active gravitational mass of matter. Giving up that assumption allows deriving from a variational principle new and better (because logically obtained) field equations that more faithfully extend the Poisson equation for Newton's gravity than do Einstein's, with an active gravitational mass density providing the source term. Solving these equations for a nonrotating spherical ball of matter with uniform mass density produces a new, improved interior metric matched at the surface of the ball to Schwarzschild's 'exterior' solution metric. This new metric can then be used to address questions about the flight times of photons and neutrinos through such a ball of matter. |
2406.12015 | Adailton Ara\'ujo Filho | A. A. Ara\'ujo Filho, J. R. Nascimento, A. Yu. Petrov, P. J.
Porf\'irio, Ali \"Ovg\"un | Effects of non-commutative geometry on black hole properties | 26 pages, 13 figures and 4 tables | null | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this study, we investigate the signatures of a non-commutative black hole
solution. Initially, we calculate the thermodynamic properties of the system,
including entropy, heat capacity, and Hawking radiation. For the latter
quantity, we employ two distinct methods: surface gravity and the topological
approach. Additionally, we examine the emission rate and remnant mass within
this context. Remarkably, the lifetime of the black hole, after reaching its
final state due to the evaporation process, is expressed analytically up to a
grey-body factor. We estimate the lifetime for specific initial and final mass
configurations. Also, we analyze the tensorial quasinormal modes using the
6th-order WKB method. Finally, we study the deflection angle, i.e.,
gravitational lensing, in both the weak and strong deflection limits.
| [
{
"created": "Mon, 17 Jun 2024 18:32:52 GMT",
"version": "v1"
}
] | 2024-06-19 | [
[
"Filho",
"A. A. Araújo",
""
],
[
"Nascimento",
"J. R.",
""
],
[
"Petrov",
"A. Yu.",
""
],
[
"Porfírio",
"P. J.",
""
],
[
"Övgün",
"Ali",
""
]
] | In this study, we investigate the signatures of a non-commutative black hole solution. Initially, we calculate the thermodynamic properties of the system, including entropy, heat capacity, and Hawking radiation. For the latter quantity, we employ two distinct methods: surface gravity and the topological approach. Additionally, we examine the emission rate and remnant mass within this context. Remarkably, the lifetime of the black hole, after reaching its final state due to the evaporation process, is expressed analytically up to a grey-body factor. We estimate the lifetime for specific initial and final mass configurations. Also, we analyze the tensorial quasinormal modes using the 6th-order WKB method. Finally, we study the deflection angle, i.e., gravitational lensing, in both the weak and strong deflection limits. |
gr-qc/0701076 | Eanna E. Flanagan | Prakash Balachandran, Eanna E. Flanagan | Detectability of Mode Resonances in Coalescing Neutron Star Binaries | 3 pages, no figures | null | null | null | gr-qc | null | Inspirals of neutron star-neutron star binaries are a promising source of
gravitational waves for gravitational wave detectors like LIGO. During the
inspiral, the tidal gravitational field of one of the stars can resonantly
excite internal modes of the other star, resulting in a phase shift in the
gravitational wave signal. We compute using a Fisher-matrix analysis how large
the phase shift must be in order to be detectable. For a $1.4 M_\odot, 1.4
M_\odot$ binary the result is $\sim 8.1, 2.9$ and 1.8 radians, for resonant
frequencies of $16, 32$ and 64 Hz. The measurement accuracies of the other
binary parameters are degraded by inclusion of the mode resonance effect.
| [
{
"created": "Mon, 15 Jan 2007 02:32:34 GMT",
"version": "v1"
}
] | 2007-05-23 | [
[
"Balachandran",
"Prakash",
""
],
[
"Flanagan",
"Eanna E.",
""
]
] | Inspirals of neutron star-neutron star binaries are a promising source of gravitational waves for gravitational wave detectors like LIGO. During the inspiral, the tidal gravitational field of one of the stars can resonantly excite internal modes of the other star, resulting in a phase shift in the gravitational wave signal. We compute using a Fisher-matrix analysis how large the phase shift must be in order to be detectable. For a $1.4 M_\odot, 1.4 M_\odot$ binary the result is $\sim 8.1, 2.9$ and 1.8 radians, for resonant frequencies of $16, 32$ and 64 Hz. The measurement accuracies of the other binary parameters are degraded by inclusion of the mode resonance effect. |
0707.2825 | Yongli Ping | Yongli Ping, Lixin Xu, Chengwu Zhang, and Hongya Liu | Dark Energy in Global Brane Universe | 8 pages,4 figures | Int.J.Mod.Phys.D16:1633-1640,2007 | 10.1142/S0218271807011024 | null | gr-qc | null | We discuss the exact solutions of brane universes and the results indicate
the Friedmann equations on the branes are modified with a new density term.
Then, we assume the new term as the density of dark energy. Using Wetterich's
parametrization equation of state (EOS) of dark energy, we obtain the new term
varies with the red-shift z. Finally, the evolutions of the mass density
parameter $\Omega_2$, dark energy density parameter $\Omega_x$ and deceleration
parameter q_2 are studied.
| [
{
"created": "Thu, 19 Jul 2007 00:40:13 GMT",
"version": "v1"
},
{
"created": "Mon, 23 Jul 2007 01:29:54 GMT",
"version": "v2"
},
{
"created": "Thu, 20 Dec 2007 12:18:13 GMT",
"version": "v3"
}
] | 2008-11-26 | [
[
"Ping",
"Yongli",
""
],
[
"Xu",
"Lixin",
""
],
[
"Zhang",
"Chengwu",
""
],
[
"Liu",
"Hongya",
""
]
] | We discuss the exact solutions of brane universes and the results indicate the Friedmann equations on the branes are modified with a new density term. Then, we assume the new term as the density of dark energy. Using Wetterich's parametrization equation of state (EOS) of dark energy, we obtain the new term varies with the red-shift z. Finally, the evolutions of the mass density parameter $\Omega_2$, dark energy density parameter $\Omega_x$ and deceleration parameter q_2 are studied. |
1211.6114 | Ulrich Sperhake | Ulrich Sperhake, Emanuele Berti, Vitor Cardoso, Frans Pretorius | Universality, maximum radiation and absorption in high-energy collisions
of black holes with spin | added simulations with larger spins; to match published version | Phys.Rev.Lett.111:041101,2013 | 10.1103/PhysRevLett.111.041101 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We explore the impact of black hole spins on the dynamics of high-energy
black hole collisions. We report results from numerical simulations with
gamma-factors up to 2.49 and dimensionless spin parameter +0.85, +0.6, 0, -0.6,
-0.85. We find that the scattering threshold becomes independent of spin at
large center-of-mass energies, confirming previous conjectures that structure
does not matter in ultrarelativistic collisions. It has further been argued
that in this limit all of the kinetic energy of the system may be radiated by
fine tuning the impact parameter to threshold. On the contrary, we find that
only about 60% of the kinetic energy is radiated for gamma=2.49. By monitoring
apparent horizons before and after scattering events we show that the "missing
energy" is absorbed by the individual black holes in the encounter, and
moreover the individual black-hole spins change significantly. We support this
conclusion with perturbative calculations. An extrapolation of our results to
the limit gamma->infinity suggests that about half of the center-of-mass energy
of the system can be emitted in gravitational radiation, while the rest must be
converted into rest-mass and spin energy.
| [
{
"created": "Mon, 26 Nov 2012 21:00:03 GMT",
"version": "v1"
},
{
"created": "Wed, 7 Aug 2013 12:30:00 GMT",
"version": "v2"
}
] | 2013-11-13 | [
[
"Sperhake",
"Ulrich",
""
],
[
"Berti",
"Emanuele",
""
],
[
"Cardoso",
"Vitor",
""
],
[
"Pretorius",
"Frans",
""
]
] | We explore the impact of black hole spins on the dynamics of high-energy black hole collisions. We report results from numerical simulations with gamma-factors up to 2.49 and dimensionless spin parameter +0.85, +0.6, 0, -0.6, -0.85. We find that the scattering threshold becomes independent of spin at large center-of-mass energies, confirming previous conjectures that structure does not matter in ultrarelativistic collisions. It has further been argued that in this limit all of the kinetic energy of the system may be radiated by fine tuning the impact parameter to threshold. On the contrary, we find that only about 60% of the kinetic energy is radiated for gamma=2.49. By monitoring apparent horizons before and after scattering events we show that the "missing energy" is absorbed by the individual black holes in the encounter, and moreover the individual black-hole spins change significantly. We support this conclusion with perturbative calculations. An extrapolation of our results to the limit gamma->infinity suggests that about half of the center-of-mass energy of the system can be emitted in gravitational radiation, while the rest must be converted into rest-mass and spin energy. |
gr-qc/0504097 | Mikhail Golubev B | Mikhail B. Golubev, Stanislav R. Kelner | Point Charge Self-Energy in the General Relativity | VI Fridmann Seminar, France, Corsica, Corgeze, 2004, LaTeX, 6 pages,
2 figes | Int.J.Mod.Phys. A20 (2005) 2288-2294 | 10.1142/S0217751X05024511 | null | gr-qc hep-th | null | Singularities in the metric of the classical solutions to the Einstein
equations (Schwarzschild, Kerr, Reissner -- Nordstr\"om and Kerr -- Newman
solutions) lead to appearance of generalized functions in the Einstein tensor
that are not usually taken into consideration. The generalized functions can be
of a more complex nature than the Dirac $\d$-function. To study them, a
technique has been used based on a limiting solution sequence. The solutions
are shown to satisfy the Einstein equations everywhere, if the energy-momentum
tensor has a relevant singular addition of non-electromagnetic origin. When the
addition is included, the total energy proves finite and equal to $mc^2$, while
for the Kerr and Kerr--Newman solutions the angular momentum is $mc {\bf a}$.
As the Reissner--Nordstr\"om and Kerr--Newman solutions correspond to the point
charge in the classical electrodynamics, the result obtained allows us to view
the point charge self-energy divergence problem in a new fashion.
| [
{
"created": "Thu, 21 Apr 2005 00:26:48 GMT",
"version": "v1"
}
] | 2009-11-11 | [
[
"Golubev",
"Mikhail B.",
""
],
[
"Kelner",
"Stanislav R.",
""
]
] | Singularities in the metric of the classical solutions to the Einstein equations (Schwarzschild, Kerr, Reissner -- Nordstr\"om and Kerr -- Newman solutions) lead to appearance of generalized functions in the Einstein tensor that are not usually taken into consideration. The generalized functions can be of a more complex nature than the Dirac $\d$-function. To study them, a technique has been used based on a limiting solution sequence. The solutions are shown to satisfy the Einstein equations everywhere, if the energy-momentum tensor has a relevant singular addition of non-electromagnetic origin. When the addition is included, the total energy proves finite and equal to $mc^2$, while for the Kerr and Kerr--Newman solutions the angular momentum is $mc {\bf a}$. As the Reissner--Nordstr\"om and Kerr--Newman solutions correspond to the point charge in the classical electrodynamics, the result obtained allows us to view the point charge self-energy divergence problem in a new fashion. |
1506.06050 | Paolo Pani | Paolo Pani | I-Love-Q relations for a gravastar and the approach to the black-hole
limit | 10 pages, 2 figures, v2: various improvements, to appear in PRD, v3:
erratum available as an ancillary file and at
https://www.dropbox.com/s/0d1gsgy0idqtihi/erratum_1506.06050.pdf?dl=0
correcting the final result for the moment of inertia and for the tidal Love
number | Phys. Rev. D 92, 124030 (2015) | 10.1103/PhysRevD.92.124030 | null | gr-qc astro-ph.HE hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The multipole moments and the tidal Love numbers of neutron stars and quark
stars satisfy certain relations which are almost insensitive to the star's
internal structure. A natural question is whether the same relations hold for
different compact objects and how they possibly approach the black-hole limit.
Here we consider "gravastars", which are hypothetical compact objects sustained
by their internal vacuum energy. Such solutions have been proposed as exotic
alternatives to the black-hole paradigm because they can be as compact as black
holes and exist in any mass range. By constructing slowly-rotating, thin-shell
gravastars to quadratic order in the spin, we compute the moment of inertia
$I$, the mass quadrupole moment $Q$, and the tidal Love number $\lambda$ in
exact form. The $I$-$\lambda$-$Q$ relations of a gravastar are dramatically
different from those of an ordinary compact star, but the black-hole limit is
continuous, i.e. these quantities approach their Kerr counterparts when the
compactness is maximum. Therefore, such relations can be used to discern a
gravastar from an ordinary compact star, but not to break the degeneracy with
the black-hole case. Based on these results, we conjecture that the full
multipolar structure and the tidal deformability of a spinning, ultracompact
gravastar are identical to those of a Kerr black hole. The approach to the
black-hole limit is nonpolynomial, thus differing from the critical behavior
recently found for strongly anisotropic neutron stars.
| [
{
"created": "Fri, 19 Jun 2015 15:29:32 GMT",
"version": "v1"
},
{
"created": "Fri, 20 Nov 2015 14:45:47 GMT",
"version": "v2"
},
{
"created": "Sat, 21 Jan 2017 12:21:50 GMT",
"version": "v3"
}
] | 2017-01-24 | [
[
"Pani",
"Paolo",
""
]
] | The multipole moments and the tidal Love numbers of neutron stars and quark stars satisfy certain relations which are almost insensitive to the star's internal structure. A natural question is whether the same relations hold for different compact objects and how they possibly approach the black-hole limit. Here we consider "gravastars", which are hypothetical compact objects sustained by their internal vacuum energy. Such solutions have been proposed as exotic alternatives to the black-hole paradigm because they can be as compact as black holes and exist in any mass range. By constructing slowly-rotating, thin-shell gravastars to quadratic order in the spin, we compute the moment of inertia $I$, the mass quadrupole moment $Q$, and the tidal Love number $\lambda$ in exact form. The $I$-$\lambda$-$Q$ relations of a gravastar are dramatically different from those of an ordinary compact star, but the black-hole limit is continuous, i.e. these quantities approach their Kerr counterparts when the compactness is maximum. Therefore, such relations can be used to discern a gravastar from an ordinary compact star, but not to break the degeneracy with the black-hole case. Based on these results, we conjecture that the full multipolar structure and the tidal deformability of a spinning, ultracompact gravastar are identical to those of a Kerr black hole. The approach to the black-hole limit is nonpolynomial, thus differing from the critical behavior recently found for strongly anisotropic neutron stars. |
1805.05856 | Bekir Baytas | Bekir Bayta\c{s}, Eugenio Bianchi, Nelson Yokomizo | Gluing polyhedra with entanglement in loop quantum gravity | 42 pages, 10 figures | Phys. Rev. D 98, 026001 (2018) | 10.1103/PhysRevD.98.026001 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In a spin-network basis state, nodes of the graph describe un-entangled
quantum regions of space, quantum polyhedra. In this paper we show how
entanglement between intertwiner degrees of freedom enforces gluing conditions
for neighboring quantum polyhedra. In particular we introduce Bell-network
states, entangled states defined via squeezed vacuum techniques. We study
correlations of quantum polyhedra in a dipole, a pentagram and a generic graph.
We find that vector geometries, structures with neighboring polyhedra having
adjacent faces glued back-to-back, arise from Bell-network states. We also
discuss the relation to Regge geometries. The results presented show clearly
the role that entanglement plays in the gluing of neighboring quantum regions
of space.
| [
{
"created": "Tue, 15 May 2018 15:39:33 GMT",
"version": "v1"
},
{
"created": "Tue, 3 Jul 2018 17:37:41 GMT",
"version": "v2"
}
] | 2018-07-04 | [
[
"Baytaş",
"Bekir",
""
],
[
"Bianchi",
"Eugenio",
""
],
[
"Yokomizo",
"Nelson",
""
]
] | In a spin-network basis state, nodes of the graph describe un-entangled quantum regions of space, quantum polyhedra. In this paper we show how entanglement between intertwiner degrees of freedom enforces gluing conditions for neighboring quantum polyhedra. In particular we introduce Bell-network states, entangled states defined via squeezed vacuum techniques. We study correlations of quantum polyhedra in a dipole, a pentagram and a generic graph. We find that vector geometries, structures with neighboring polyhedra having adjacent faces glued back-to-back, arise from Bell-network states. We also discuss the relation to Regge geometries. The results presented show clearly the role that entanglement plays in the gluing of neighboring quantum regions of space. |
gr-qc/0612060 | Duncan Brown | Duncan A. Brown, Jeandrew Brink, Hua Fang, Jonathan R. Gair, Chao Li,
Geoffrey Lovelace, Ilya Mandel, Kip S. Thorne | Gravitational waves from intermediate-mass-ratio inspirals for
ground-based detectors | Accepted for publication in Physical Review Letters | Phys.Rev.Lett.99:201102,2007 | 10.1103/PhysRevLett.99.201102 | LIGO-P060054-00-Z | gr-qc astro-ph.CO astro-ph.HE | null | We explore the prospects for Advanced LIGO to detect gravitational waves from
neutron stars and stellar mass black holes spiraling into intermediate-mass
($M\sim 50 M_\odot$ to $350 M_\odot$) black holes. We estimate an event rate
for such \emph{intermediate-mass-ratio inspirals} (IMRIs) of up to $\sim
10$--$30 \mathrm{yr}^{-1}$. Our numerical simulations show that if the central
body is not a black hole but its metric is stationary, axisymmetric, reflection
symmetric and asymptotically flat then the waves will likely be tri-periodic,
as for a black hole. We report generalizations of a theorem due to Ryan (1995)
which suggest that the evolutions of the waves' three fundamental frequencies
and of the complex amplitudes of their spectral components encode (in
principle) a full map of the central body's metric, full details of the energy
and angular momentum exchange between the central body and the orbit, and the
time-evolving orbital elements. We estimate that Advanced LIGO can measure or
constrain deviations of the central body from a Kerr black hole with modest but
interesting accuracy.
| [
{
"created": "Mon, 11 Dec 2006 20:14:56 GMT",
"version": "v1"
},
{
"created": "Thu, 13 Mar 2008 00:43:19 GMT",
"version": "v2"
}
] | 2009-11-10 | [
[
"Brown",
"Duncan A.",
""
],
[
"Brink",
"Jeandrew",
""
],
[
"Fang",
"Hua",
""
],
[
"Gair",
"Jonathan R.",
""
],
[
"Li",
"Chao",
""
],
[
"Lovelace",
"Geoffrey",
""
],
[
"Mandel",
"Ilya",
""
],
[
"Thorne",
"Kip S.",
""
]
] | We explore the prospects for Advanced LIGO to detect gravitational waves from neutron stars and stellar mass black holes spiraling into intermediate-mass ($M\sim 50 M_\odot$ to $350 M_\odot$) black holes. We estimate an event rate for such \emph{intermediate-mass-ratio inspirals} (IMRIs) of up to $\sim 10$--$30 \mathrm{yr}^{-1}$. Our numerical simulations show that if the central body is not a black hole but its metric is stationary, axisymmetric, reflection symmetric and asymptotically flat then the waves will likely be tri-periodic, as for a black hole. We report generalizations of a theorem due to Ryan (1995) which suggest that the evolutions of the waves' three fundamental frequencies and of the complex amplitudes of their spectral components encode (in principle) a full map of the central body's metric, full details of the energy and angular momentum exchange between the central body and the orbit, and the time-evolving orbital elements. We estimate that Advanced LIGO can measure or constrain deviations of the central body from a Kerr black hole with modest but interesting accuracy. |
gr-qc/0501014 | T. R. Mongan | T. R. Mongan | Simple quantum cosmology: Vacuum energy and initial state | To be published in General Relativity and Gravitation, Vol. 37, May
2005. 5 pages, no figures | Gen.Rel.Grav. 37 (2005) 967-970 | 10.1007/s10714-005-0079-y | null | gr-qc astro-ph hep-ph | null | A static non-singular 10-dimensional closed Friedmann universe of Planck
size, filled with a perfect fluid with an equation of state with w = -2/3, can
arise spontaneously by a quantum fluctuation from nothing in 11-dimensional
spacetime. A quantum transition from this state can initiate the inflationary
quantum cosmology outlined in Ref. 2 [General Relativity and Gravitation 33,
1415, 2001 - gr-qc/0103021]. With no fine-tuning, that cosmology predicts about
60 e-folds of inflation and a vacuum energy density depending only on the
number of extra space dimensions (seven), G, h, c and the ratio between the
strength of gravity and the strength of the strong force. The fraction of the
total energy in the universe represented by this vacuum energy depends on the
Hubble constant. Hubble constant estimates from WMAP, SDSS, the Hubble Key
Project and Sunyaev-Zeldovich and X-ray flux measurements range from 60 to 72
km/(Mpc sec). With a mid-range Hubble constant of 65 km/(Mpc sec), the model in
Ref. 2 predicts Omega-sub-Lambda = 0.7
| [
{
"created": "Wed, 5 Jan 2005 21:20:42 GMT",
"version": "v1"
}
] | 2009-11-11 | [
[
"Mongan",
"T. R.",
""
]
] | A static non-singular 10-dimensional closed Friedmann universe of Planck size, filled with a perfect fluid with an equation of state with w = -2/3, can arise spontaneously by a quantum fluctuation from nothing in 11-dimensional spacetime. A quantum transition from this state can initiate the inflationary quantum cosmology outlined in Ref. 2 [General Relativity and Gravitation 33, 1415, 2001 - gr-qc/0103021]. With no fine-tuning, that cosmology predicts about 60 e-folds of inflation and a vacuum energy density depending only on the number of extra space dimensions (seven), G, h, c and the ratio between the strength of gravity and the strength of the strong force. The fraction of the total energy in the universe represented by this vacuum energy depends on the Hubble constant. Hubble constant estimates from WMAP, SDSS, the Hubble Key Project and Sunyaev-Zeldovich and X-ray flux measurements range from 60 to 72 km/(Mpc sec). With a mid-range Hubble constant of 65 km/(Mpc sec), the model in Ref. 2 predicts Omega-sub-Lambda = 0.7 |
2209.07543 | Dongjun Li | Dongjun Li, Vincent S. H. Lee, Yanbei Chen, Kathryn M. Zurek | Interferometer Response to Geontropic Fluctuations | 17 pages, 6 figures | null | 10.1103/PhysRevD.107.024002 | CALT-TH-2022-033 | gr-qc hep-ph hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We model vacuum fluctuations in quantum gravity with a scalar field,
characterized by a high occupation number, coupled to the metric. The
occupation number of the scalar is given by a thermal density matrix, whose
form is motivated by fluctuations in the vacuum energy, which have been shown
to be conformal near a light-sheet horizon. For the experimental measurement of
interest in an interferometer, the size of the energy fluctuations is fixed by
the area of a surface bounding the volume of spacetime being interrogated by an
interferometer. We compute the interferometer response to these "geontropic"
scalar-metric fluctuations, and apply our results to current and future
interferometer measurements, such as LIGO and the proposed GQuEST experiment.
| [
{
"created": "Thu, 15 Sep 2022 18:00:16 GMT",
"version": "v1"
}
] | 2023-01-18 | [
[
"Li",
"Dongjun",
""
],
[
"Lee",
"Vincent S. H.",
""
],
[
"Chen",
"Yanbei",
""
],
[
"Zurek",
"Kathryn M.",
""
]
] | We model vacuum fluctuations in quantum gravity with a scalar field, characterized by a high occupation number, coupled to the metric. The occupation number of the scalar is given by a thermal density matrix, whose form is motivated by fluctuations in the vacuum energy, which have been shown to be conformal near a light-sheet horizon. For the experimental measurement of interest in an interferometer, the size of the energy fluctuations is fixed by the area of a surface bounding the volume of spacetime being interrogated by an interferometer. We compute the interferometer response to these "geontropic" scalar-metric fluctuations, and apply our results to current and future interferometer measurements, such as LIGO and the proposed GQuEST experiment. |
gr-qc/9712055 | Marsha Weaver | Marsha Weaver, James Isenberg, Beverly K. Berger | Mixmaster Behavior in Inhomogeneous Cosmological Spacetimes | 4 pages plus 4 figures. A sentence has been deleted. Accepted for
publication in PRL | Phys.Rev.Lett. 80 (1998) 2984-2987 | 10.1103/PhysRevLett.80.2984 | null | gr-qc | null | Numerical investigation of a class of inhomogeneous cosmological spacetimes
shows evidence that at a generic point in space the evolution toward the
initial singularity is asymptotically that of a spatially homogeneous spacetime
with Mixmaster behavior. This supports a long-standing conjecture due to
Belinskii et al. on the nature of the generic singularity in Einstein's
equations.
| [
{
"created": "Fri, 12 Dec 1997 04:28:04 GMT",
"version": "v1"
},
{
"created": "Wed, 4 Feb 1998 04:59:48 GMT",
"version": "v2"
},
{
"created": "Wed, 11 Mar 1998 20:35:55 GMT",
"version": "v3"
}
] | 2009-10-30 | [
[
"Weaver",
"Marsha",
""
],
[
"Isenberg",
"James",
""
],
[
"Berger",
"Beverly K.",
""
]
] | Numerical investigation of a class of inhomogeneous cosmological spacetimes shows evidence that at a generic point in space the evolution toward the initial singularity is asymptotically that of a spatially homogeneous spacetime with Mixmaster behavior. This supports a long-standing conjecture due to Belinskii et al. on the nature of the generic singularity in Einstein's equations. |
1707.01261 | Marcus Werner | Frederic P. Schuller and Marcus C. Werner | Etherington's Distance Duality with Birefringence | Invited paper for special issue `Gravitational Lensing and
Astrometry' of Universe, accepted for publication | null | null | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We consider light propagation in a spacetime whose kinematics allow weak
birefringence, and whose dynamics have recently been derived by gravitational
closure. Revisiting the definitions of luminosity and angular diameter
distances in this setting, we present a modification of the Etherington
distance duality relation in a weak gravitational field around a point mass.
This provides the first concrete example of how the non-metricities implied by
gravitational closure of birefringent electrodynamics affect observationally
testable relations.
| [
{
"created": "Wed, 5 Jul 2017 08:41:46 GMT",
"version": "v1"
}
] | 2017-07-06 | [
[
"Schuller",
"Frederic P.",
""
],
[
"Werner",
"Marcus C.",
""
]
] | We consider light propagation in a spacetime whose kinematics allow weak birefringence, and whose dynamics have recently been derived by gravitational closure. Revisiting the definitions of luminosity and angular diameter distances in this setting, we present a modification of the Etherington distance duality relation in a weak gravitational field around a point mass. This provides the first concrete example of how the non-metricities implied by gravitational closure of birefringent electrodynamics affect observationally testable relations. |
1603.04159 | Shingo Takeuchi | Shingo Takeuchi | Hawking fluxes and Anomalies in Rotating Regular Black Holes with a
Time-Delay | 26 pages, 2 figures, accepted version in CQG | Class.Quant.Grav. 33 (2016) 225016 | 10.1088/0264-9381/33/22/225016 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Based on the anomaly cancellation method we are going to compute the Hawking
fluxes (the Hawking thermal flux and the total flux of energy-momentum tensor)
from a four-dimensional rotating regular black hole with a time-delay. To this
purpose, in the three metrics proposed in arXiv:1510.08828, we try to perform
the dimensional reduction in which the anomaly cancellation method is feasible
at the near-horizon region in a general scalar field theory. As a result we can
demonstrate that the dimensional reduction is possible in two of those metrics.
Hence we perform the anomaly cancellation method and compute the Hawking fluxes
in those two metrics. Our Hawking fluxes involve the three effects: 1) the
quantum gravity effect regularizing the core of the black holes, 2) rotation of
the black hole, 3) the time-delay. Further in this paper toward the metric in
which the dimensional could not be performed, we argue that it would be some
problematic metric, and mention its cause. The Hawking fluxes we compute in
this study could be considered to correspond to more realistic Hawking fluxes.
Further what Hawking fluxes can be obtained from the anomaly cancellation
method would be interesting in terms of the relation between a consistency of
quantum field theories and black hole thermodynamics.
| [
{
"created": "Mon, 14 Mar 2016 08:05:29 GMT",
"version": "v1"
},
{
"created": "Tue, 3 May 2016 17:14:10 GMT",
"version": "v2"
},
{
"created": "Wed, 11 May 2016 15:19:13 GMT",
"version": "v3"
},
{
"created": "Mon, 16 May 2016 15:15:59 GMT",
"version": "v4"
},
{
"created": "Wed, 10 Aug 2016 16:21:40 GMT",
"version": "v5"
},
{
"created": "Wed, 12 Oct 2016 15:33:45 GMT",
"version": "v6"
}
] | 2016-10-31 | [
[
"Takeuchi",
"Shingo",
""
]
] | Based on the anomaly cancellation method we are going to compute the Hawking fluxes (the Hawking thermal flux and the total flux of energy-momentum tensor) from a four-dimensional rotating regular black hole with a time-delay. To this purpose, in the three metrics proposed in arXiv:1510.08828, we try to perform the dimensional reduction in which the anomaly cancellation method is feasible at the near-horizon region in a general scalar field theory. As a result we can demonstrate that the dimensional reduction is possible in two of those metrics. Hence we perform the anomaly cancellation method and compute the Hawking fluxes in those two metrics. Our Hawking fluxes involve the three effects: 1) the quantum gravity effect regularizing the core of the black holes, 2) rotation of the black hole, 3) the time-delay. Further in this paper toward the metric in which the dimensional could not be performed, we argue that it would be some problematic metric, and mention its cause. The Hawking fluxes we compute in this study could be considered to correspond to more realistic Hawking fluxes. Further what Hawking fluxes can be obtained from the anomaly cancellation method would be interesting in terms of the relation between a consistency of quantum field theories and black hole thermodynamics. |
gr-qc/0007074 | Kip S. Thorne | Lee Samuel Finn (1) and Kip S. Thorne (2) ((1) Department of Physics,
Astronomy & Astrophysics, The Pennsylvania State University, University Park,
PA, (2) Theoretical Astrophysics, California Institute of Technology,
Pasadena, CA) | Gravitational Waves from a Compact Star in a Circular, Inspiral Orbit,
in the Equatorial Plane of a Massive, Spinning Black Hole, as Observed by
LISA | Physical Review D, in press; 21 pages, 9 figures, 10 tables it is
present in the RevTeX file | Phys.Rev.D62:124021,2000 | 10.1103/PhysRevD.62.124021 | null | gr-qc | null | Results are presented from high-precision computations of the orbital
evolution and emitted gravitational waves for a stellar-mass object spiraling
into a massive black hole in a slowly shrinking, circular, equatorial orbit.
The focus of these computations is inspiral near the innermost stable circular
orbit (isco)---more particularly, on orbits for which the angular velocity
Omega is 0.03 < Omega/Omega_{isco} < 1. The computations are based on the
Teukolsky-Sasaki-Nakamura formalism, and the results are tabulated in a set of
functions that are of order unity and represent relativistic corrections to
low-orbital-velocity formulas. These tables can form a foundation for future
design studies for the LISA space-based gravitational-wave mission. A first
survey of applications to LISA is presented: Signal to noise ratios S/N are
computed and graphed as functions of the time-evolving gravitational-wave
frequency for representative values of the hole's mass M and spin a and the
inspiraling object's mass \mu, with the distance to Earth chosen to be r_o = 1
Gpc. These S/N's show a very strong dependence on the black-hole spin, as well
as on M and \mu. A comparison with predicted event rates shows strong promise
for detecting these waves, but not beyond about 1Gpc if the inspiraling object
is a white dwarf or neutron star. This argues for a modest lowering of LISA's
noise floor. A brief discussion is given of the prospects for extracting
information from the observed waves
| [
{
"created": "Fri, 28 Jul 2000 06:07:46 GMT",
"version": "v1"
}
] | 2014-11-17 | [
[
"Finn",
"Lee Samuel",
""
],
[
"Thorne",
"Kip S.",
""
]
] | Results are presented from high-precision computations of the orbital evolution and emitted gravitational waves for a stellar-mass object spiraling into a massive black hole in a slowly shrinking, circular, equatorial orbit. The focus of these computations is inspiral near the innermost stable circular orbit (isco)---more particularly, on orbits for which the angular velocity Omega is 0.03 < Omega/Omega_{isco} < 1. The computations are based on the Teukolsky-Sasaki-Nakamura formalism, and the results are tabulated in a set of functions that are of order unity and represent relativistic corrections to low-orbital-velocity formulas. These tables can form a foundation for future design studies for the LISA space-based gravitational-wave mission. A first survey of applications to LISA is presented: Signal to noise ratios S/N are computed and graphed as functions of the time-evolving gravitational-wave frequency for representative values of the hole's mass M and spin a and the inspiraling object's mass \mu, with the distance to Earth chosen to be r_o = 1 Gpc. These S/N's show a very strong dependence on the black-hole spin, as well as on M and \mu. A comparison with predicted event rates shows strong promise for detecting these waves, but not beyond about 1Gpc if the inspiraling object is a white dwarf or neutron star. This argues for a modest lowering of LISA's noise floor. A brief discussion is given of the prospects for extracting information from the observed waves |
gr-qc/0104016 | David Coule | D.H.Coule | Does brane cosmology have realistic principles? | extended version and title change | null | 10.1088/0264-9381/18/20/306 | null | gr-qc hep-th | null | The maximal symmetry, or Perfect Cosmological Principle(PCP), that prevents
AdS type spaces from degenerating into anti-inflationary collapse is argued to
be unphysical. For example, the simple requirement that brane-bulk models
should be the result of having evolved from even more energetic string
phenomena picks out a preferred time direction.
We question whether quantum cosmological reasoning can be applied in any
meaningful way to obtain, what are essentially, classical constructs . An
alternative scheme is to more readily accept the PCP and allow the branes to
also become eternal. A perpetually expanding and contracting brane model could
be driven by the presence of charged black holes in the AdS bulk, that
effectively violates the weak-energy condition as singularities are approached.
This can be contrasted with the so-called Ekpyrotic universe which also closely
accepts the PCP. This being broken only by occasional collisions between
branes, that can then simulate a big bang cosmology.
| [
{
"created": "Wed, 4 Apr 2001 17:22:08 GMT",
"version": "v1"
},
{
"created": "Thu, 26 Apr 2001 17:10:53 GMT",
"version": "v2"
}
] | 2016-08-31 | [
[
"Coule",
"D. H.",
""
]
] | The maximal symmetry, or Perfect Cosmological Principle(PCP), that prevents AdS type spaces from degenerating into anti-inflationary collapse is argued to be unphysical. For example, the simple requirement that brane-bulk models should be the result of having evolved from even more energetic string phenomena picks out a preferred time direction. We question whether quantum cosmological reasoning can be applied in any meaningful way to obtain, what are essentially, classical constructs . An alternative scheme is to more readily accept the PCP and allow the branes to also become eternal. A perpetually expanding and contracting brane model could be driven by the presence of charged black holes in the AdS bulk, that effectively violates the weak-energy condition as singularities are approached. This can be contrasted with the so-called Ekpyrotic universe which also closely accepts the PCP. This being broken only by occasional collisions between branes, that can then simulate a big bang cosmology. |
2312.17014 | Bogeun Gwak | Junbeom Ko, Bogeun Gwak | Universality on thermodynamic relation with corrections in de Sitter
black holes | 19 pages, published in JHEP | null | 10.1007/JHEP03(2024)072 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We herein investigate the universal relation proposed by Goon and Penco in de
Sitter black holes with electric charge or angular momentum. Our analysis
focuses on the cosmological horizon, which only exists in de Sitter and Nariai
spacetimes. Because the relation is given in a general case, the overall
relationship may be valid. However, we elucidate the details of the relation,
highlighting distinctions from those of (anti-)de Sitter black holes while
affirming the validity of the relation. Furthermore, based on our analysis of
Schwarzschild--de Sitter, Reissner--Nordstr\"om--de Sitter, and Kerr--de Sitter
black holes, we demonstrate the universality of the thermodynamic relation in
de Sitter black holes.
| [
{
"created": "Thu, 28 Dec 2023 13:31:15 GMT",
"version": "v1"
},
{
"created": "Thu, 14 Mar 2024 12:12:06 GMT",
"version": "v2"
}
] | 2024-03-15 | [
[
"Ko",
"Junbeom",
""
],
[
"Gwak",
"Bogeun",
""
]
] | We herein investigate the universal relation proposed by Goon and Penco in de Sitter black holes with electric charge or angular momentum. Our analysis focuses on the cosmological horizon, which only exists in de Sitter and Nariai spacetimes. Because the relation is given in a general case, the overall relationship may be valid. However, we elucidate the details of the relation, highlighting distinctions from those of (anti-)de Sitter black holes while affirming the validity of the relation. Furthermore, based on our analysis of Schwarzschild--de Sitter, Reissner--Nordstr\"om--de Sitter, and Kerr--de Sitter black holes, we demonstrate the universality of the thermodynamic relation in de Sitter black holes. |
2110.02340 | Mitja Fridman Mr. | Saurya Das, Mitja Fridman, Gaetano Lambiase, Antonio Stabile and Elias
C. Vagenas | Modified dispersion relations and a potential explanation of the EDGES
anomaly | 11 pages, 8 figures | Eur. Phys. J. C 82, no.8, 720 (2022) [erratum: Eur. Phys. J. C 82,
no.9, 816 (2022)] | 10.1140/epjc/s10052-022-10680-8 | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Experiment to Detect the Global Epoch of Reionisation Signature (EDGES)
collaboration has recently reported an important result related to the
absorption signal in the Cosmic Microwave Background radiation spectrum. This
signal corresponds to the red-shifted 21-cm line at $z \simeq 17.2$, whose
amplitude is about twice the expected value. This represents a deviation of
approximately $3.8\sigma$ from the predictions of the standard model of
cosmology, i.e. the $\Lambda$CDM model. This opens a window for testing new
physics beyond both the standard model of particle physics and the $\Lambda$CDM
model. In this work, we explore the possibility of explaining the EDGES anomaly
in terms of modified dispersion relations. The latter are typically induced in
unified theories and theories of quantum gravity, such as String/M-theories and
Loop Quantum Gravity. These modified dispersion relations affect the density of
states per unit volume and thus the thermal spectrum of the Cosmic Microwave
Background photons. The temperature of the 21-cm brightness temperature is
modified accordingly giving a potential explanation of the EDGES anomaly.
| [
{
"created": "Tue, 5 Oct 2021 20:15:31 GMT",
"version": "v1"
},
{
"created": "Mon, 15 Aug 2022 16:01:40 GMT",
"version": "v2"
}
] | 2023-06-30 | [
[
"Das",
"Saurya",
""
],
[
"Fridman",
"Mitja",
""
],
[
"Lambiase",
"Gaetano",
""
],
[
"Stabile",
"Antonio",
""
],
[
"Vagenas",
"Elias C.",
""
]
] | The Experiment to Detect the Global Epoch of Reionisation Signature (EDGES) collaboration has recently reported an important result related to the absorption signal in the Cosmic Microwave Background radiation spectrum. This signal corresponds to the red-shifted 21-cm line at $z \simeq 17.2$, whose amplitude is about twice the expected value. This represents a deviation of approximately $3.8\sigma$ from the predictions of the standard model of cosmology, i.e. the $\Lambda$CDM model. This opens a window for testing new physics beyond both the standard model of particle physics and the $\Lambda$CDM model. In this work, we explore the possibility of explaining the EDGES anomaly in terms of modified dispersion relations. The latter are typically induced in unified theories and theories of quantum gravity, such as String/M-theories and Loop Quantum Gravity. These modified dispersion relations affect the density of states per unit volume and thus the thermal spectrum of the Cosmic Microwave Background photons. The temperature of the 21-cm brightness temperature is modified accordingly giving a potential explanation of the EDGES anomaly. |
1908.04275 | Andreas Schmitt | Nils Andersson and Andreas Schmitt | Dissipation triggers dynamical two-stream instability | 20 pages, 4 figures, v2: minor changes in the text, references added,
version accepted for publication | null | null | null | gr-qc astro-ph.HE hep-ph physics.plasm-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Two coupled, interpenetrating fluids suffer instabilities beyond certain
critical counterflows. For ideal fluids, an energetic instability occurs at the
point where a sound mode inverts its direction due to the counterflow, while
dynamical instabilities only occur at larger relative velocities. Here we
discuss two relativistic fluids, one of which is dissipative. Using linearized
hydrodynamics, we show that in this case the energetic instability turns
dynamical, i.e., there is an exponentially growing mode, and this exponential
growth only occurs in the presence of dissipation. This result is general and
does not rely on an underlying microscopic theory. It can be applied to various
two-fluid systems for instance in the interior of neutron stars. We also point
out that under certain circumstances the two-fluid system exhibits a mode
analogous to the r-mode in neutron stars that can become unstable for
arbitrarily small values of the counterflow.
| [
{
"created": "Wed, 7 Aug 2019 10:02:21 GMT",
"version": "v1"
},
{
"created": "Fri, 1 Nov 2019 10:15:32 GMT",
"version": "v2"
}
] | 2019-11-04 | [
[
"Andersson",
"Nils",
""
],
[
"Schmitt",
"Andreas",
""
]
] | Two coupled, interpenetrating fluids suffer instabilities beyond certain critical counterflows. For ideal fluids, an energetic instability occurs at the point where a sound mode inverts its direction due to the counterflow, while dynamical instabilities only occur at larger relative velocities. Here we discuss two relativistic fluids, one of which is dissipative. Using linearized hydrodynamics, we show that in this case the energetic instability turns dynamical, i.e., there is an exponentially growing mode, and this exponential growth only occurs in the presence of dissipation. This result is general and does not rely on an underlying microscopic theory. It can be applied to various two-fluid systems for instance in the interior of neutron stars. We also point out that under certain circumstances the two-fluid system exhibits a mode analogous to the r-mode in neutron stars that can become unstable for arbitrarily small values of the counterflow. |
2309.07397 | Long-Gang Pang | Zhi-Han Li, Chen-Qi Li, Long-Gang Pang | Solving Einstein equations using deep learning | 18 pages, 4 figures | null | null | null | gr-qc nucl-th physics.comp-ph | http://creativecommons.org/licenses/by-nc-sa/4.0/ | Einstein field equations are notoriously challenging to solve due to their
complex mathematical form, with few analytical solutions available in the
absence of highly symmetric systems or ideal matter distribution. However,
accurate solutions are crucial, particularly in systems with strong
gravitational field such as black holes or neutron stars. In this work, we use
neural networks and auto differentiation to solve the Einstein field equations
numerically inspired by the idea of physics-informed neural networks (PINNs).
By utilizing these techniques, we successfully obtain the Schwarzschild metric
and the charged Schwarzschild metric given the energy-momentum tensor of
matter. This innovative method could open up a different way for solving
space-time coupled Einstein field equations and become an integral part of
numerical relativity.
| [
{
"created": "Thu, 14 Sep 2023 02:46:48 GMT",
"version": "v1"
}
] | 2023-09-15 | [
[
"Li",
"Zhi-Han",
""
],
[
"Li",
"Chen-Qi",
""
],
[
"Pang",
"Long-Gang",
""
]
] | Einstein field equations are notoriously challenging to solve due to their complex mathematical form, with few analytical solutions available in the absence of highly symmetric systems or ideal matter distribution. However, accurate solutions are crucial, particularly in systems with strong gravitational field such as black holes or neutron stars. In this work, we use neural networks and auto differentiation to solve the Einstein field equations numerically inspired by the idea of physics-informed neural networks (PINNs). By utilizing these techniques, we successfully obtain the Schwarzschild metric and the charged Schwarzschild metric given the energy-momentum tensor of matter. This innovative method could open up a different way for solving space-time coupled Einstein field equations and become an integral part of numerical relativity. |
2301.04967 | Hai Siong Tan | H. S. Tan | Shadows of Kerr-Vaidya-like black holes | 28 pages, 9 figures. [v4]: minor edits | Class. Quantum Grav. 40 195010, 2023 | 10.1088/1361-6382/acf180 | null | gr-qc astro-ph.HE hep-th | http://creativecommons.org/licenses/by/4.0/ | In this work, we study the shadow boundary curves of rotating time-dependent
black hole solutions which have well-defined Kerr and Vaidya limits. These
solutions are constructed by applying the Newman-Janis algorithm to a
spherically symmetric seed metric conformal to the Vaidya solution with a mass
function that is linear in Eddington-Finkelstein coordinates. Equipped with a
conformal Killing vector field, this class of solution exhibits separability of
null geodesics, thus allowing one to develop an analytic formula for the
boundary curve of its shadow. We find a simple power law describing the
dependence of the mean radius and asymmetry factor of the shadow on the
accretion rate. Applicability of our model to recent Event Horizon Telescope
observations of M87${}^*$ and Sgr A${}^*$ is also discussed.
| [
{
"created": "Thu, 12 Jan 2023 12:21:28 GMT",
"version": "v1"
},
{
"created": "Mon, 16 Jan 2023 11:29:42 GMT",
"version": "v2"
},
{
"created": "Sun, 20 Aug 2023 13:51:51 GMT",
"version": "v3"
},
{
"created": "Wed, 20 Sep 2023 23:29:14 GMT",
"version": "v4"
}
] | 2023-09-22 | [
[
"Tan",
"H. S.",
""
]
] | In this work, we study the shadow boundary curves of rotating time-dependent black hole solutions which have well-defined Kerr and Vaidya limits. These solutions are constructed by applying the Newman-Janis algorithm to a spherically symmetric seed metric conformal to the Vaidya solution with a mass function that is linear in Eddington-Finkelstein coordinates. Equipped with a conformal Killing vector field, this class of solution exhibits separability of null geodesics, thus allowing one to develop an analytic formula for the boundary curve of its shadow. We find a simple power law describing the dependence of the mean radius and asymmetry factor of the shadow on the accretion rate. Applicability of our model to recent Event Horizon Telescope observations of M87${}^*$ and Sgr A${}^*$ is also discussed. |
2310.07356 | Archie Cable | Archie Cable and Arttu Rajantie | Stochastic parameters for scalar fields in de Sitter spacetime | 53 pages, 4 figures | Phys. Rev. D 109, 045017 (2024) | null | null | gr-qc hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The stochastic effective theory approach, often called stochastic inflation,
is widely used in cosmology to describe scalar field dynamics during inflation.
The existing formulations are, however, more qualitative than quantitative
because the connection to the underlying quantum field theory (QFT) has not
been properly established. A concrete sign of this is that the QFT parameters
depend on the renormalisation scale, and therefore the relation between the QFT
and stochastic theory must have explicit scale dependence that cancels it. In
this paper we achieve that by determining the parameters of the second-order
stochastic effective theory of light scalar fields in de Sitter to linear order
in the self-coupling constant $\lambda$. This is done by computing equal-time
two-point correlators to one-loop order both in QFT using dimensional
regularisation and the $\overline{\rm MS}$ renormalisation scheme and the
equal-time four-point correlator to leading order in both theories, and
demanding that the results obtained in the two theories agree. With these
parameters, the effective theory is valid when $m\lesssim H$ and $\lambda^2\ll
m^4/H^4$, and therefore it is applicable in cases where neither perturbation
theory nor any previously proposed stochastic effective theories are.
| [
{
"created": "Wed, 11 Oct 2023 10:14:54 GMT",
"version": "v1"
},
{
"created": "Thu, 12 Oct 2023 08:59:07 GMT",
"version": "v2"
},
{
"created": "Wed, 28 Feb 2024 10:07:54 GMT",
"version": "v3"
}
] | 2024-02-29 | [
[
"Cable",
"Archie",
""
],
[
"Rajantie",
"Arttu",
""
]
] | The stochastic effective theory approach, often called stochastic inflation, is widely used in cosmology to describe scalar field dynamics during inflation. The existing formulations are, however, more qualitative than quantitative because the connection to the underlying quantum field theory (QFT) has not been properly established. A concrete sign of this is that the QFT parameters depend on the renormalisation scale, and therefore the relation between the QFT and stochastic theory must have explicit scale dependence that cancels it. In this paper we achieve that by determining the parameters of the second-order stochastic effective theory of light scalar fields in de Sitter to linear order in the self-coupling constant $\lambda$. This is done by computing equal-time two-point correlators to one-loop order both in QFT using dimensional regularisation and the $\overline{\rm MS}$ renormalisation scheme and the equal-time four-point correlator to leading order in both theories, and demanding that the results obtained in the two theories agree. With these parameters, the effective theory is valid when $m\lesssim H$ and $\lambda^2\ll m^4/H^4$, and therefore it is applicable in cases where neither perturbation theory nor any previously proposed stochastic effective theories are. |
1906.10363 | Yuki Sakakihara | Asuka Ito, Yuki Sakakihara, Jiro Soda | Accelerating Universe with a stable extra dimension in cuscuton gravity | 10 pages | Phys. Rev. D 100, 063531 (2019) | 10.1103/PhysRevD.100.063531 | KOBE-COSMO-09-11 | gr-qc astro-ph.CO hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study Kaluza-Klein cosmology in cuscuton gravity and find an exact
solution describing an accelerating 4-dimensional universe with a stable extra
dimension. A cuscuton which is a non-dynamical scalar field is responsible for
the accelerating expansion and a vector field makes the extra dimensional space
stable. Remarkably, the accelerating universe in our model is not exactly de
Sitter.
| [
{
"created": "Tue, 25 Jun 2019 07:41:43 GMT",
"version": "v1"
}
] | 2019-10-02 | [
[
"Ito",
"Asuka",
""
],
[
"Sakakihara",
"Yuki",
""
],
[
"Soda",
"Jiro",
""
]
] | We study Kaluza-Klein cosmology in cuscuton gravity and find an exact solution describing an accelerating 4-dimensional universe with a stable extra dimension. A cuscuton which is a non-dynamical scalar field is responsible for the accelerating expansion and a vector field makes the extra dimensional space stable. Remarkably, the accelerating universe in our model is not exactly de Sitter. |
2402.06413 | Tianshu Wu | Tianshu Wu and Yiqian Chen | Distinguishing the Observational Signatures of Hot Spots Orbiting
Reissner-Nordstr\"om Spacetime | 21 pages, 7 figures | null | null | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | This paper delves into observable signatures of hot spots orbiting
Reissner-Nordstr\"om (RN) black holes and naked singularities. In a RN black
hole case, we find two discernible lensing image tracks in time integrated
images capturing a complete orbit of hot spots, and a image shadow within the
critical curve where photons with a small impact parameter fall into the event
horizon. Conversely, in RN singularities, additional image tracks can be found
inner the critical curve, originating from photons reflected by the infinitely
high effective potential well. Moreover, we found incomplete and converge
tracks from the time integrated images of hot spot orbiting RN singularities
lacking of a photon sphere. The presence of these additional image tracks
exerts a significant influence on temporal magnitudes at their local maxima,
allowing us to differentiate between RN black holes and RN naked singularities.
| [
{
"created": "Fri, 9 Feb 2024 14:00:09 GMT",
"version": "v1"
}
] | 2024-02-12 | [
[
"Wu",
"Tianshu",
""
],
[
"Chen",
"Yiqian",
""
]
] | This paper delves into observable signatures of hot spots orbiting Reissner-Nordstr\"om (RN) black holes and naked singularities. In a RN black hole case, we find two discernible lensing image tracks in time integrated images capturing a complete orbit of hot spots, and a image shadow within the critical curve where photons with a small impact parameter fall into the event horizon. Conversely, in RN singularities, additional image tracks can be found inner the critical curve, originating from photons reflected by the infinitely high effective potential well. Moreover, we found incomplete and converge tracks from the time integrated images of hot spot orbiting RN singularities lacking of a photon sphere. The presence of these additional image tracks exerts a significant influence on temporal magnitudes at their local maxima, allowing us to differentiate between RN black holes and RN naked singularities. |
0708.0178 | Volker Perlick | Volker Perlick | Theoretical gravitational lensing. Beyond the weak-field small-angle
approximation | 20 pages, 9 figures; extended written version of rapporteur talk,
given at the workshop on ``Theoretical Gravitational Lensing'' at the 11th
Marcel Grossmann Meeting, Berlin, 2006 | null | 10.1142/9789812834300_0030 | null | gr-qc | null | An overview is given on those theoretical gravitational lensing results that
can be formulated in a spacetime setting, without assuming that the
gravitational fields are weak and that the bending angles are small. The first
part is devoted to analytical methods considering spacetimes in which the
equations for light rays (lightlike geodesics) is completely integrable. This
includes spherically symmetric static spacetimes, the Kerr spacetime and plane
gravitational waves. The second part is devoted to qualitative methods which
give some information on lensing properties without actually solving the
equation for lightlike geodesics. This includes Morse theory, methods from
differential topology and bifurcation theory.
| [
{
"created": "Wed, 1 Aug 2007 15:31:22 GMT",
"version": "v1"
}
] | 2016-11-15 | [
[
"Perlick",
"Volker",
""
]
] | An overview is given on those theoretical gravitational lensing results that can be formulated in a spacetime setting, without assuming that the gravitational fields are weak and that the bending angles are small. The first part is devoted to analytical methods considering spacetimes in which the equations for light rays (lightlike geodesics) is completely integrable. This includes spherically symmetric static spacetimes, the Kerr spacetime and plane gravitational waves. The second part is devoted to qualitative methods which give some information on lensing properties without actually solving the equation for lightlike geodesics. This includes Morse theory, methods from differential topology and bifurcation theory. |
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