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|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
1501.04956
|
Michele Levi
|
Michele Levi, Jan Steinhoff
|
Spinning gravitating objects in the effective field theory in the
post-Newtonian scheme
|
47 pages, 4 figures, published
|
JHEP 1509 (2015) 219
|
10.1007/JHEP09(2015)219
| null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We introduce a formulation for spinning gravitating objects in the effective
field theory in the post-Newtonian scheme in the context of the binary inspiral
problem. We aim at an effective action, where all field modes below the orbital
scale are integrated out. We spell out the relevant degrees of freedom, in
particular the rotational ones, and the associated symmetries. Building on
these symmetries, we introduce the minimal coupling part of the point particle
action in terms of gauge rotational variables, and construct the spin-induced
nonminimal couplings, where we obtain the leading order couplings to all orders
in spin. We specify the gauge for the rotational variables, where the
unphysical degrees of freedom are eliminated already from the Feynman rules,
and all the orbital field modes are integrated out. The equations of motion of
the spin can be directly obtained via a proper variation of the action, and
Hamiltonians may be straightforwardly derived. We implement this effective
field theory for spin to derive all spin dependent potentials up to
next-to-leading order to quadratic level in spin, namely up to the third
post-Newtonian order for rapidly rotating compact objects. In particular, the
proper next-to-leading order spin-squared potential and Hamiltonian for generic
compact objects are also derived. For the implementations we use the
nonrelativistic gravitational field decomposition, which is found here to
eliminate higher-loop Feynman diagrams also in spin dependent sectors, and
facilitates derivations. This formulation for spin is thus ideal for treatment
of higher order spin dependent sectors.
|
[
{
"created": "Tue, 20 Jan 2015 20:54:00 GMT",
"version": "v1"
},
{
"created": "Tue, 11 Aug 2015 08:24:30 GMT",
"version": "v2"
},
{
"created": "Mon, 5 Oct 2015 23:30:43 GMT",
"version": "v3"
}
] |
2015-10-07
|
[
[
"Levi",
"Michele",
""
],
[
"Steinhoff",
"Jan",
""
]
] |
We introduce a formulation for spinning gravitating objects in the effective field theory in the post-Newtonian scheme in the context of the binary inspiral problem. We aim at an effective action, where all field modes below the orbital scale are integrated out. We spell out the relevant degrees of freedom, in particular the rotational ones, and the associated symmetries. Building on these symmetries, we introduce the minimal coupling part of the point particle action in terms of gauge rotational variables, and construct the spin-induced nonminimal couplings, where we obtain the leading order couplings to all orders in spin. We specify the gauge for the rotational variables, where the unphysical degrees of freedom are eliminated already from the Feynman rules, and all the orbital field modes are integrated out. The equations of motion of the spin can be directly obtained via a proper variation of the action, and Hamiltonians may be straightforwardly derived. We implement this effective field theory for spin to derive all spin dependent potentials up to next-to-leading order to quadratic level in spin, namely up to the third post-Newtonian order for rapidly rotating compact objects. In particular, the proper next-to-leading order spin-squared potential and Hamiltonian for generic compact objects are also derived. For the implementations we use the nonrelativistic gravitational field decomposition, which is found here to eliminate higher-loop Feynman diagrams also in spin dependent sectors, and facilitates derivations. This formulation for spin is thus ideal for treatment of higher order spin dependent sectors.
|
2405.15883
|
Ghulam Mustafa
|
Puja Mukherjee, Ujjal Debnath, Himanshu Chaudhary and G. Mustafa
|
The estimation of parameters of generalized cosmic Chaplygin gas and
viscous modified Chaplygin gas and Accretions around Black Hole in the
background of Einstein-Aether gravity
|
20 pages, 5 figures
| null | null | null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this paper, we have investigated the phenomenon of accelerated cosmic
expansion in the late universe and the mass accretion process of a
4-dimensional Einstein-Aether black hole. Starting with the basics of
Einstein-Aether gravity theory, we have first considered the field equations
and two eminent models of Chaplygin gas, viz. generalized cosmic Chaplygin gas
model and viscous modified Chaplygin gas model. Then, we obtained the energy
density and Hubble parameters equations for these models in terms of some
dimensionless density parameters and some unknown parameters. After finding the
required parameters, we proceeded with the mass accretion process. For both
models, we obtained the equation of mass in terms of the redshift function and
represented the change of mass of the black hole graphically with redshift. At
the same time, we have made a graphical comparison between the above-mentioned
models and the $\Lambda$CDM model of the universe. Eventually, we have
concluded that the mass of a 4-dimensional black hole will increase along the
universe's evolution in the backdrop of Einstein-Aether gravity.
|
[
{
"created": "Fri, 24 May 2024 19:02:16 GMT",
"version": "v1"
}
] |
2024-05-28
|
[
[
"Mukherjee",
"Puja",
""
],
[
"Debnath",
"Ujjal",
""
],
[
"Chaudhary",
"Himanshu",
""
],
[
"Mustafa",
"G.",
""
]
] |
In this paper, we have investigated the phenomenon of accelerated cosmic expansion in the late universe and the mass accretion process of a 4-dimensional Einstein-Aether black hole. Starting with the basics of Einstein-Aether gravity theory, we have first considered the field equations and two eminent models of Chaplygin gas, viz. generalized cosmic Chaplygin gas model and viscous modified Chaplygin gas model. Then, we obtained the energy density and Hubble parameters equations for these models in terms of some dimensionless density parameters and some unknown parameters. After finding the required parameters, we proceeded with the mass accretion process. For both models, we obtained the equation of mass in terms of the redshift function and represented the change of mass of the black hole graphically with redshift. At the same time, we have made a graphical comparison between the above-mentioned models and the $\Lambda$CDM model of the universe. Eventually, we have concluded that the mass of a 4-dimensional black hole will increase along the universe's evolution in the backdrop of Einstein-Aether gravity.
|
2308.11049
|
Saeed Fakhry
|
Saeed Fakhry
|
Primordial Black Hole Merger Rate in $f(R)$ Gravity
|
17 pages, 11 figures, references added
|
The Astrophysical Journal (2024)
|
10.3847/1538-4357/ad0e66
| null |
gr-qc astro-ph.CO
|
http://creativecommons.org/licenses/by/4.0/
|
Primordial black holes (PBHs) are known as one of the potential candidates
for dark matter. They are expected to have formed due to the direct
gravitational collapse of density fluctuations in the early Universe.
Therefore, the study of the merger rate of PBHs in modified theories of gravity
can provide more detailed information about their abundance. In this work, we
delve into the calculation of the merger rate of PBHs within the theoretical
framework of $f(R)$ gravity. Our analysis reveals an enhancement in the merger
rate of PBHs compared to that obtained from general relativity (GR).
Additionally, modulating the field strength $f_{R0}$ induces shifts in the PBH
merger rate, presenting a potential observational signature of modified
gravity. We also find that the total merger rate of PBHs will be consistent
with the merger rate of black holes estimated by the Laser Interferometer
Gravitational-Wave Observatory (LIGO)-Virgo-KAGRA detectors if $f_{PBH}\gtrsim
0.1$. While further improvements might be required, relative enhancement of the
merger rate of PBHs in the framework of $f(R)$ gravity and its consistency with
gravitational wave data underscore the importance of employing modified
theories of gravity to examine diverse scenarios related to the formation of
black holes.
|
[
{
"created": "Mon, 21 Aug 2023 21:20:30 GMT",
"version": "v1"
}
] |
2024-01-11
|
[
[
"Fakhry",
"Saeed",
""
]
] |
Primordial black holes (PBHs) are known as one of the potential candidates for dark matter. They are expected to have formed due to the direct gravitational collapse of density fluctuations in the early Universe. Therefore, the study of the merger rate of PBHs in modified theories of gravity can provide more detailed information about their abundance. In this work, we delve into the calculation of the merger rate of PBHs within the theoretical framework of $f(R)$ gravity. Our analysis reveals an enhancement in the merger rate of PBHs compared to that obtained from general relativity (GR). Additionally, modulating the field strength $f_{R0}$ induces shifts in the PBH merger rate, presenting a potential observational signature of modified gravity. We also find that the total merger rate of PBHs will be consistent with the merger rate of black holes estimated by the Laser Interferometer Gravitational-Wave Observatory (LIGO)-Virgo-KAGRA detectors if $f_{PBH}\gtrsim 0.1$. While further improvements might be required, relative enhancement of the merger rate of PBHs in the framework of $f(R)$ gravity and its consistency with gravitational wave data underscore the importance of employing modified theories of gravity to examine diverse scenarios related to the formation of black holes.
|
2011.09304
|
Muhammad Sharif
|
M. Sharif and Faisal Javed
|
Stable Bounded Excursion Gravastars with Regular Black Holes
|
29 pages, 19 figures, to appear in ASTR
|
Astrophys. Space Sci. 366(2021)103
|
10.1007/s10509-021-04010-9
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
This paper explores the possible existence of stable regions of bounded
excursion gravastars in the background of regular black holes (Bardeen and
Bardeen-de Sitter black holes). For this purpose, we match internal de Sitter
geometry with an external regular black hole through an intermediate shell with
an equation of state. The matter surface located at the shell greatly affects
the dynamical configuration of the shell. We consider stiff and dust fluids to
discuss the outcomes of the developed structures. We then determine the
critical values of physical parameters at which the shell neither collapses nor
expands for both cases with different choices of external and internal
geometries. It is found that there does not exist any possible region of stable
bounded excursion gravastar for the interior flat and exterior regular
geometries. However, the stable bounded excursion gravastar is obtained for the
interior de Sitter and exterior regular black holes with a suitable choice of
physical parameters for both stiff and dust shells. We conclude that the
possibility of the existence of both bounded excursion gravastars as well as
black holes cannot be excluded in the dynamical model.
|
[
{
"created": "Tue, 17 Nov 2020 13:43:33 GMT",
"version": "v1"
},
{
"created": "Wed, 27 Oct 2021 13:42:21 GMT",
"version": "v2"
}
] |
2021-11-17
|
[
[
"Sharif",
"M.",
""
],
[
"Javed",
"Faisal",
""
]
] |
This paper explores the possible existence of stable regions of bounded excursion gravastars in the background of regular black holes (Bardeen and Bardeen-de Sitter black holes). For this purpose, we match internal de Sitter geometry with an external regular black hole through an intermediate shell with an equation of state. The matter surface located at the shell greatly affects the dynamical configuration of the shell. We consider stiff and dust fluids to discuss the outcomes of the developed structures. We then determine the critical values of physical parameters at which the shell neither collapses nor expands for both cases with different choices of external and internal geometries. It is found that there does not exist any possible region of stable bounded excursion gravastar for the interior flat and exterior regular geometries. However, the stable bounded excursion gravastar is obtained for the interior de Sitter and exterior regular black holes with a suitable choice of physical parameters for both stiff and dust shells. We conclude that the possibility of the existence of both bounded excursion gravastars as well as black holes cannot be excluded in the dynamical model.
|
gr-qc/9802068
|
Don Marolf
|
Jorma Louko and Donald Marolf
|
Inextendible Schwarzschild black hole with a single exterior: How
thermal is the Hawking radiation?
|
53 pages, REVTex v3.1 with amsfonts and epsf, includes 5 eps figures.
(v2: Title and abstract expanded, minor comments added. v3: Minor typos
corrected.)
|
Phys.Rev.D58:024007,1998
|
10.1103/PhysRevD.58.024007
|
PPG98-79, SU-GP-98/2-1
|
gr-qc hep-th
| null |
Several approaches to Hawking radiation on Schwarzschild spacetime rely in
some way or another on the fact that the Kruskal manifold has two causally
disconnected exterior regions. We investigate the Hawking(-Unruh) effect for a
real scalar field on the $\RPthree$ geon: an inextendible, globally hyperbolic,
space and time orientable eternal black hole spacetime that is locally
isometric to Kruskal but contains only one exterior region. The
Hartle-Hawking-like vacuum~$\hhvacgeon$, which can be characterized
alternatively by the positive frequency properties along the horizons or by the
complex analytic properties of the Feynman propagator, turns out to contain
exterior region Boulware modes in correlated pairs, and any operator in the
exterior that only couples to one member of each correlated Boulware pair has
thermal expectation values in the usual Hawking temperature. Generic operators
in the exterior do not have this special form; however, we use a Bogoliubov
transformation, a particle detector analysis, and a particle
emission-absorption analysis that invokes the analytic properties of the
Feynman propagator, to argue that $\hhvacgeon$ appears as a thermal bath with
the standard Hawking temperature to any exterior observer at asymptotically
early and late Schwarzschild times. A~(naive) saddle-point estimate for the
path-integral-approach partition function yields for the geon only half of the
Bekenstein-Hawking entropy of a Schwarzschild black hole with the same ADM
mass: possible implications of this result for the validity of path-integral
methods or for the statistical interpretation of black-hole entropy are
discussed. Analogous results hold for a Rindler observer in a flat spacetime
whose global properties mimic those of the geon.
|
[
{
"created": "Fri, 27 Feb 1998 14:49:47 GMT",
"version": "v1"
},
{
"created": "Tue, 14 Apr 1998 13:44:09 GMT",
"version": "v2"
},
{
"created": "Mon, 22 Jun 1998 08:59:42 GMT",
"version": "v3"
}
] |
2008-11-26
|
[
[
"Louko",
"Jorma",
""
],
[
"Marolf",
"Donald",
""
]
] |
Several approaches to Hawking radiation on Schwarzschild spacetime rely in some way or another on the fact that the Kruskal manifold has two causally disconnected exterior regions. We investigate the Hawking(-Unruh) effect for a real scalar field on the $\RPthree$ geon: an inextendible, globally hyperbolic, space and time orientable eternal black hole spacetime that is locally isometric to Kruskal but contains only one exterior region. The Hartle-Hawking-like vacuum~$\hhvacgeon$, which can be characterized alternatively by the positive frequency properties along the horizons or by the complex analytic properties of the Feynman propagator, turns out to contain exterior region Boulware modes in correlated pairs, and any operator in the exterior that only couples to one member of each correlated Boulware pair has thermal expectation values in the usual Hawking temperature. Generic operators in the exterior do not have this special form; however, we use a Bogoliubov transformation, a particle detector analysis, and a particle emission-absorption analysis that invokes the analytic properties of the Feynman propagator, to argue that $\hhvacgeon$ appears as a thermal bath with the standard Hawking temperature to any exterior observer at asymptotically early and late Schwarzschild times. A~(naive) saddle-point estimate for the path-integral-approach partition function yields for the geon only half of the Bekenstein-Hawking entropy of a Schwarzschild black hole with the same ADM mass: possible implications of this result for the validity of path-integral methods or for the statistical interpretation of black-hole entropy are discussed. Analogous results hold for a Rindler observer in a flat spacetime whose global properties mimic those of the geon.
|
gr-qc/0002056
|
Guillermo A. Mena Marugan
|
Maria E. Angulo (Univ. of Sussex, UK) and Guillermo A. Mena Marugan
(IMAFF, CSIC, Spain)
|
Large quantum gravity effects: Cylindrical waves in four dimensions
|
Version accepted for publication in Int. J. Mod. Phys. D
|
Int.J.Mod.Phys.D9:669-686,2000
|
10.1142/S0218271800000633
| null |
gr-qc
| null |
Linearly polarized cylindrical waves in four-dimensional vacuum gravity are
mathematically equivalent to rotationally symmetric gravity coupled to a
Maxwell (or Klein-Gordon) field in three dimensions. The quantization of this
latter system was performed by Ashtekar and Pierri in a recent work. Employing
that quantization, we obtain here a complete quantum theory which describes the
four-dimensional geometry of the Einstein-Rosen waves. In particular, we
construct regularized operators to represent the metric. It is shown that the
results achieved by Ashtekar about the existence of important quantum gravity
effects in the Einstein-Maxwell system at large distances from the symmetry
axis continue to be valid from a four-dimensional point of view. The only
significant difference is that, in order to admit an approximate classical
description in the asymptotic region, states that are coherent in the Maxwell
field need not contain a large number of photons anymore. We also analyze the
metric fluctuations on the symmetry axis and argue that they are generally
relevant for all of the coherent states.
|
[
{
"created": "Wed, 16 Feb 2000 09:40:33 GMT",
"version": "v1"
},
{
"created": "Tue, 27 Jun 2000 08:03:31 GMT",
"version": "v2"
}
] |
2010-11-19
|
[
[
"Angulo",
"Maria E.",
"",
"Univ. of Sussex, UK"
],
[
"Marugan",
"Guillermo A. Mena",
"",
"IMAFF, CSIC, Spain"
]
] |
Linearly polarized cylindrical waves in four-dimensional vacuum gravity are mathematically equivalent to rotationally symmetric gravity coupled to a Maxwell (or Klein-Gordon) field in three dimensions. The quantization of this latter system was performed by Ashtekar and Pierri in a recent work. Employing that quantization, we obtain here a complete quantum theory which describes the four-dimensional geometry of the Einstein-Rosen waves. In particular, we construct regularized operators to represent the metric. It is shown that the results achieved by Ashtekar about the existence of important quantum gravity effects in the Einstein-Maxwell system at large distances from the symmetry axis continue to be valid from a four-dimensional point of view. The only significant difference is that, in order to admit an approximate classical description in the asymptotic region, states that are coherent in the Maxwell field need not contain a large number of photons anymore. We also analyze the metric fluctuations on the symmetry axis and argue that they are generally relevant for all of the coherent states.
|
gr-qc/0005028
|
Felix Finster
|
Felix Finster, Joel Smoller, and Shing-Tung Yau
|
Absence of Static, Spherically Symmetric Black Hole Solutions for
Einstein-Dirac-Yang/Mills Equations with Complete Fermion Shells
|
27 pages, 1 figure (published version)
|
Adv.Theor.Math.Phys.4:1231-1257,2002
| null | null |
gr-qc math-ph math.AP math.MP
| null |
We study a static, spherically symmetric system of (2j+1) massive Dirac
particles, each having angular momentum j, j=1,2,..., in a classical
gravitational and SU(2) Yang-Mills field. We show that for any black hole
solution of the associated Einstein-Dirac-Yang/Mills equations, the spinors
must vanish identically outside of the event horizon.
|
[
{
"created": "Wed, 10 May 2000 11:58:36 GMT",
"version": "v1"
},
{
"created": "Sat, 7 Oct 2000 18:41:46 GMT",
"version": "v2"
},
{
"created": "Tue, 11 Jun 2002 16:05:14 GMT",
"version": "v3"
}
] |
2010-11-19
|
[
[
"Finster",
"Felix",
""
],
[
"Smoller",
"Joel",
""
],
[
"Yau",
"Shing-Tung",
""
]
] |
We study a static, spherically symmetric system of (2j+1) massive Dirac particles, each having angular momentum j, j=1,2,..., in a classical gravitational and SU(2) Yang-Mills field. We show that for any black hole solution of the associated Einstein-Dirac-Yang/Mills equations, the spinors must vanish identically outside of the event horizon.
|
1406.1930
|
Vedad Pasic Dr
|
Vedad Pasic and Elvis Barakovic
|
PP-waves with Torsion - a Metric-affine Model for the Massless Neutrino
|
24 pages. Corrected two references. The final publication is
available at springerlink.com. arXiv admin note: text overlap with
arXiv:gr-qc/0505157; and text overlap with arXiv:gr-qc/0304028,
arXiv:gr-qc/9402012 by other authors
|
General Relativ Gravit (2014) 46:1787
|
10.1007/s10714-014-1787-y
| null |
gr-qc math.DG
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this paper we deal with quadratic metric-affine gravity, which we briefly
introduce, explain and give historical and physical reasons for using this
particular theory of gravity. Further, we introduce a generalisation of well
known spacetimes, namely pp-waves. A classical pp-wave is a 4-dimensional
Lorentzian spacetime, which admits a nonvanishing parallel spinor field; here
the connection is assumed to be Levi-Civita. This definition was generalised in
our previous work to metric compatible spacetimes with torsion and used to
construct new explicit vacuum solutions of quadratic metric-affine gravity,
namely generalised pp-waves of parallel Ricci curvature. The physical
interpretation of these solutions we propose in this article is that they
represent a conformally invariant metric-affine model for a massless elementary
particle. We give a comparison with the classical model describing the
interaction of gravitational and massless neutrino fields, namely Einstein-Weyl
theory and construct pp-wave type solutions of this theory. We point out that
generalised pp-waves of parallel Ricci curvature are very similar to pp-wave
type solutions of the Einstein-Weyl model and therefore propose that our
generalised pp-waves of parallel Ricci curvature represent a metric-affine
model for the massless neutrino.
|
[
{
"created": "Sat, 7 Jun 2014 21:10:33 GMT",
"version": "v1"
},
{
"created": "Sat, 9 Aug 2014 12:50:53 GMT",
"version": "v2"
},
{
"created": "Wed, 3 Sep 2014 12:47:40 GMT",
"version": "v3"
}
] |
2014-09-04
|
[
[
"Pasic",
"Vedad",
""
],
[
"Barakovic",
"Elvis",
""
]
] |
In this paper we deal with quadratic metric-affine gravity, which we briefly introduce, explain and give historical and physical reasons for using this particular theory of gravity. Further, we introduce a generalisation of well known spacetimes, namely pp-waves. A classical pp-wave is a 4-dimensional Lorentzian spacetime, which admits a nonvanishing parallel spinor field; here the connection is assumed to be Levi-Civita. This definition was generalised in our previous work to metric compatible spacetimes with torsion and used to construct new explicit vacuum solutions of quadratic metric-affine gravity, namely generalised pp-waves of parallel Ricci curvature. The physical interpretation of these solutions we propose in this article is that they represent a conformally invariant metric-affine model for a massless elementary particle. We give a comparison with the classical model describing the interaction of gravitational and massless neutrino fields, namely Einstein-Weyl theory and construct pp-wave type solutions of this theory. We point out that generalised pp-waves of parallel Ricci curvature are very similar to pp-wave type solutions of the Einstein-Weyl model and therefore propose that our generalised pp-waves of parallel Ricci curvature represent a metric-affine model for the massless neutrino.
|
1912.05315
|
Roman Konoplya
|
Kirill A. Bronnikov and Roman A. Konoplya
|
Echoes in brane worlds: ringing at a black hole--wormhole transition
|
9 pages, revtex, 6 figures
|
Phys. Rev. D 101, 064004 (2020)
|
10.1103/PhysRevD.101.064004
| null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Echoes are known as modifications of the usual quasinormal ringing of a black
hole at late times because of the deviation of space-time from the initial
black-hole geometry in a small region near its event horizon. We consider a
class of brane-world model solutions of the Shiromizu-Maeda-Sasaki equations,
which describe both black holes and wormholes and interpolate between them via
a continuous parameter. In this way the brane-world scenario provides a natural
model for wormholes mimicking the black hole behavior if the continuous
parameter is chosen near the threshold with a black-hole solution. We show that
in the vicinity of this threshold interpolating between black holes and
wormholes, quasinormal ringing of the wormholes at the initial stage is
indistinguishable from that of the black holes with nearby values of the above
parameter, but at later times the signal is modified by intensive echoes. We
notice that the black-hole mimickers that are wormholes near the threshold have
the largest quality factor and are therefore the best oscillators among the
considered examples.
|
[
{
"created": "Wed, 11 Dec 2019 13:56:52 GMT",
"version": "v1"
}
] |
2020-03-11
|
[
[
"Bronnikov",
"Kirill A.",
""
],
[
"Konoplya",
"Roman A.",
""
]
] |
Echoes are known as modifications of the usual quasinormal ringing of a black hole at late times because of the deviation of space-time from the initial black-hole geometry in a small region near its event horizon. We consider a class of brane-world model solutions of the Shiromizu-Maeda-Sasaki equations, which describe both black holes and wormholes and interpolate between them via a continuous parameter. In this way the brane-world scenario provides a natural model for wormholes mimicking the black hole behavior if the continuous parameter is chosen near the threshold with a black-hole solution. We show that in the vicinity of this threshold interpolating between black holes and wormholes, quasinormal ringing of the wormholes at the initial stage is indistinguishable from that of the black holes with nearby values of the above parameter, but at later times the signal is modified by intensive echoes. We notice that the black-hole mimickers that are wormholes near the threshold have the largest quality factor and are therefore the best oscillators among the considered examples.
|
0810.0916
|
Miodrag Krmar
|
Vladan Pankovic, Simo Ciganovic, Jovan Ivanovic
|
A Simple Determination of the (LOGARITHMIC) Corrections of Black Hole
Entropy "without Knowing the Details of Quantum Gravity"
|
6 pages, no figures
| null | null |
PMF/Ph-12/08
|
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this work, starting by simple, approximate (quasi-classical) methods
presented in our previous works, we suggest a simple determination of the
(logarithmic) corrections of (Schwarzschild) black hole entropy "without
knowing the details of quantum gravity"(Fursaev). Namely, in our previous works
we demonstrated that all well-known important thermodynamical characteristics
of the black hole (Bekenstein-Hawking entropy, Bekenstein entropy/surface
quantization and Hawking temperature) can be effectively reproduced starting by
simple supposition that black hole horizon circumference holds integer number
of reduced Compton wave lengths corresponding to mass (energy) spectrum of a
small quantum system. (Obviously it is conceptually analogous to Bohr
quantization postulate interpreted by de Broglie relation in Old,
Bohr-Sommerfeld, quantum theory.) Especially, black hole entropy can be
presented as the quotient of the black hole mass and the minimal mass of small
quantum system in ground mass (energy) state. Now, we suppose that black hole
mass correction is simply equivalent to negative classical potential energy of
the gravitational interaction between black hole and small quantum system in
ground mass (energy) state. As it is not hard to see absolute value of the
classical potential energy of gravitational interaction is identical to black
hole temperature. All this, according to first thermodynamical law, implies
that first order entropy correction holds form of the logarithm of the surface
with coefficient -0.5. Our result, obtained practically quasi-classically,
"without knowing the details of quantum gravity", is equivalent to result
obtained by loop quantum gravity and other quantum gravity methods for
macroscopic black holes.
|
[
{
"created": "Mon, 6 Oct 2008 09:21:19 GMT",
"version": "v1"
}
] |
2008-10-07
|
[
[
"Pankovic",
"Vladan",
""
],
[
"Ciganovic",
"Simo",
""
],
[
"Ivanovic",
"Jovan",
""
]
] |
In this work, starting by simple, approximate (quasi-classical) methods presented in our previous works, we suggest a simple determination of the (logarithmic) corrections of (Schwarzschild) black hole entropy "without knowing the details of quantum gravity"(Fursaev). Namely, in our previous works we demonstrated that all well-known important thermodynamical characteristics of the black hole (Bekenstein-Hawking entropy, Bekenstein entropy/surface quantization and Hawking temperature) can be effectively reproduced starting by simple supposition that black hole horizon circumference holds integer number of reduced Compton wave lengths corresponding to mass (energy) spectrum of a small quantum system. (Obviously it is conceptually analogous to Bohr quantization postulate interpreted by de Broglie relation in Old, Bohr-Sommerfeld, quantum theory.) Especially, black hole entropy can be presented as the quotient of the black hole mass and the minimal mass of small quantum system in ground mass (energy) state. Now, we suppose that black hole mass correction is simply equivalent to negative classical potential energy of the gravitational interaction between black hole and small quantum system in ground mass (energy) state. As it is not hard to see absolute value of the classical potential energy of gravitational interaction is identical to black hole temperature. All this, according to first thermodynamical law, implies that first order entropy correction holds form of the logarithm of the surface with coefficient -0.5. Our result, obtained practically quasi-classically, "without knowing the details of quantum gravity", is equivalent to result obtained by loop quantum gravity and other quantum gravity methods for macroscopic black holes.
|
gr-qc/9811009
|
Thomas B. Bahder
|
Thomas B. Bahder
|
Fermi Coordinates of an Observer Moving in a Circle in Minkowski Space:
Apparent Behavior of Clocks
| null | null | null | null |
gr-qc
| null |
Coordinate transformations are derived from global Minkowski coordinates to
the Fermi coordinates of an observer moving in a circle in Minkowski
space-time. The metric for the Fermi coordinates is calculated directly from
the tensor transformation rule. The behavior of ideal clocks is examined from
the observer's reference frame using the Fermi coordinates. A complicated
relation exists between Fermi coordinate time and proper time on stationary
clocks (in the Fermi frame) and between proper time on satellite clocks that
orbit the observer. An orbital Sagnac-like effect exists for portable clocks
that orbit the Fermi coordinate origin. The coordinate speed of light is
isotropic but varies with Fermi coordinate position and time. The magnitudes of
these kinematic effects are computed for parameters that are relevant to the
Global Positioning System (GPS) and are found to be small; however, for future
high-accuracy time transfer systems, these effects may be of significant
magnitude.
|
[
{
"created": "Tue, 3 Nov 1998 16:00:40 GMT",
"version": "v1"
}
] |
2007-05-23
|
[
[
"Bahder",
"Thomas B.",
""
]
] |
Coordinate transformations are derived from global Minkowski coordinates to the Fermi coordinates of an observer moving in a circle in Minkowski space-time. The metric for the Fermi coordinates is calculated directly from the tensor transformation rule. The behavior of ideal clocks is examined from the observer's reference frame using the Fermi coordinates. A complicated relation exists between Fermi coordinate time and proper time on stationary clocks (in the Fermi frame) and between proper time on satellite clocks that orbit the observer. An orbital Sagnac-like effect exists for portable clocks that orbit the Fermi coordinate origin. The coordinate speed of light is isotropic but varies with Fermi coordinate position and time. The magnitudes of these kinematic effects are computed for parameters that are relevant to the Global Positioning System (GPS) and are found to be small; however, for future high-accuracy time transfer systems, these effects may be of significant magnitude.
|
1504.00306
|
Mikhail Gorbatenko
|
M.V. Gorbatenko, V.P. Neznamov, E.Yu. Popov
|
Some Aspects of Quantum Mechanics of Particle Motion in Static Centrally
Symmetric Gravitational Fields
|
21 pages, 2 figures
| null | null | null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The domain of wave functions and effective potentials of the Dirac and
Klein-Gordon equations for quantum-mechanical particles in static centrally
symmetric gravitational fields are analyzed by taking into account the Hilbert
causality condition. For all the explored metrics, assuming existence of event
horizons, the conditions of a "fall" of a particle to the appropriate event
horizons are implemented. The exclusion is one of the solutions for the
Reissner-Nordstroem extreme field with the single event horizon. In this case,
while fulfilling the condition found by V.I.Dokuchaev, Yu.N.Yeroshenko, the
normalization integral is convergent and the wave functions become zero on the
event horizon. This corresponds to the Hilbert causality condition. In our
paper, due to the analysis of the effective potential for the
Reissner-Nordstroem extreme field with real radial wave functions of the Dirac
equation, the impossibility is demonstrated for the bound stationary state
existence of quantum-mechanical particles, with positive energy, off the event
horizon. The analysis of the effective potential of the Dirac equation for the
case of the naked singularity of the Reissner-Nordstroem field shown the
possible existence of stationary bound states of quantum-mechanical half-spin
particles.
|
[
{
"created": "Wed, 1 Apr 2015 17:25:20 GMT",
"version": "v1"
}
] |
2015-04-02
|
[
[
"Gorbatenko",
"M. V.",
""
],
[
"Neznamov",
"V. P.",
""
],
[
"Popov",
"E. Yu.",
""
]
] |
The domain of wave functions and effective potentials of the Dirac and Klein-Gordon equations for quantum-mechanical particles in static centrally symmetric gravitational fields are analyzed by taking into account the Hilbert causality condition. For all the explored metrics, assuming existence of event horizons, the conditions of a "fall" of a particle to the appropriate event horizons are implemented. The exclusion is one of the solutions for the Reissner-Nordstroem extreme field with the single event horizon. In this case, while fulfilling the condition found by V.I.Dokuchaev, Yu.N.Yeroshenko, the normalization integral is convergent and the wave functions become zero on the event horizon. This corresponds to the Hilbert causality condition. In our paper, due to the analysis of the effective potential for the Reissner-Nordstroem extreme field with real radial wave functions of the Dirac equation, the impossibility is demonstrated for the bound stationary state existence of quantum-mechanical particles, with positive energy, off the event horizon. The analysis of the effective potential of the Dirac equation for the case of the naked singularity of the Reissner-Nordstroem field shown the possible existence of stationary bound states of quantum-mechanical half-spin particles.
|
1305.4461
|
Jianwei Mei
|
Jianwei Mei
|
Fluctuating Black Hole Horizons
|
References added, nature of boundary stress tensor clarified,
discussion of statistics refined and a mistake with Hawking temperature
corrected, 16 pages; version to appear in journal
| null |
10.1007/JHEP10(2013)195
| null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this paper we treat the black hole horizon as a physical boundary to the
spacetime and study its dynamics following from the Gibbons-Hawking-York
boundary term. Using the Kerr black hole as an example we derive an effective
action that describes, in the large wave number limit, a massless Klein-Gordon
field living on the average location of the boundary. Complete solutions can be
found in the small rotation limit of the black hole. The formulation suggests
that the boundary can be treated in the same way as any other matter
contributions. In particular, the angular momentum of the boundary matches
exactly with that of the black hole, suggesting an interesting possibility that
all charges (including the entropy) of the black hole are carried by the
boundary. Using this as input, we derive predictions on the Planck scale
properties of the boundary.
|
[
{
"created": "Mon, 20 May 2013 08:32:58 GMT",
"version": "v1"
},
{
"created": "Tue, 21 May 2013 19:57:42 GMT",
"version": "v2"
},
{
"created": "Mon, 7 Oct 2013 11:22:18 GMT",
"version": "v3"
}
] |
2015-06-16
|
[
[
"Mei",
"Jianwei",
""
]
] |
In this paper we treat the black hole horizon as a physical boundary to the spacetime and study its dynamics following from the Gibbons-Hawking-York boundary term. Using the Kerr black hole as an example we derive an effective action that describes, in the large wave number limit, a massless Klein-Gordon field living on the average location of the boundary. Complete solutions can be found in the small rotation limit of the black hole. The formulation suggests that the boundary can be treated in the same way as any other matter contributions. In particular, the angular momentum of the boundary matches exactly with that of the black hole, suggesting an interesting possibility that all charges (including the entropy) of the black hole are carried by the boundary. Using this as input, we derive predictions on the Planck scale properties of the boundary.
|
2109.00754
|
Tousif Islam
|
Tousif Islam, Scott E. Field, Gaurav Khanna, Niels Warburton
|
Survey of gravitational wave memory in intermediate mass ratio binaries
|
18 pages, 17 figures, matches the version published in PRD
|
Phys. Rev. D 108, 024046 (2023)
|
10.1103/PhysRevD.108.024046
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The non-linear gravitational wave (GW) memory effect is a distinct prediction
in general relativity. While the effect has been well studied for comparable
mass binaries, it has mostly been overlooked for intermediate mass ratio
inspirals (IMRIs). We offer a comprehensive analysis of the phenomenology and
detectability of memory effects, including contributions from subdominant
harmonic modes, in heavy IMRIs consisting of a stellar mass black hole and an
intermediate mass black hole. When formed through hierarchical mergers, for
example when a GW190521-like remnant captures a stellar mass black hole, IMRI
systems have a large total mass, large spin on the primary, and possibly
residual eccentricity; features that potentially raise the prospect for memory
detection. We compute both the displacement and spin non-linear GW memory from
the $m \neq 0$ gravitational waveforms computed within a black hole
perturbation theory framework that is partially calibrated to numerical
relativity waveforms. We probe the dependence of memory effects on mass ratio,
spin, and eccentricity and consider the detectability of a memory signal from
IMRIs using current and future GW detectors. We find that (i) while
eccentricity introduces additional features in both displacement and spin
memory, it does not appreciatively change the prospects of detectability, (ii)
including higher modes into the memory computation can increase singal-to-noise
(SNR) values by about 7\% in some cases, (iii) the SNR from displacement memory
dramatically increases as the spin approaches large, positive values, (iv) spin
memory from heavy IMRIs would, however, be difficult to detect with future
generation detectors even from highly spinning systems. Our results suggest
that hierarchical binary black hole mergers may be a promising source for
detecting memory and could favorably impact memory forecasts.
|
[
{
"created": "Thu, 2 Sep 2021 07:24:42 GMT",
"version": "v1"
},
{
"created": "Mon, 24 Jul 2023 22:06:05 GMT",
"version": "v2"
}
] |
2023-07-26
|
[
[
"Islam",
"Tousif",
""
],
[
"Field",
"Scott E.",
""
],
[
"Khanna",
"Gaurav",
""
],
[
"Warburton",
"Niels",
""
]
] |
The non-linear gravitational wave (GW) memory effect is a distinct prediction in general relativity. While the effect has been well studied for comparable mass binaries, it has mostly been overlooked for intermediate mass ratio inspirals (IMRIs). We offer a comprehensive analysis of the phenomenology and detectability of memory effects, including contributions from subdominant harmonic modes, in heavy IMRIs consisting of a stellar mass black hole and an intermediate mass black hole. When formed through hierarchical mergers, for example when a GW190521-like remnant captures a stellar mass black hole, IMRI systems have a large total mass, large spin on the primary, and possibly residual eccentricity; features that potentially raise the prospect for memory detection. We compute both the displacement and spin non-linear GW memory from the $m \neq 0$ gravitational waveforms computed within a black hole perturbation theory framework that is partially calibrated to numerical relativity waveforms. We probe the dependence of memory effects on mass ratio, spin, and eccentricity and consider the detectability of a memory signal from IMRIs using current and future GW detectors. We find that (i) while eccentricity introduces additional features in both displacement and spin memory, it does not appreciatively change the prospects of detectability, (ii) including higher modes into the memory computation can increase singal-to-noise (SNR) values by about 7\% in some cases, (iii) the SNR from displacement memory dramatically increases as the spin approaches large, positive values, (iv) spin memory from heavy IMRIs would, however, be difficult to detect with future generation detectors even from highly spinning systems. Our results suggest that hierarchical binary black hole mergers may be a promising source for detecting memory and could favorably impact memory forecasts.
|
1905.00524
|
Alexander Agathonov
|
Yu.G. Ignat'ev, A.A. Agathonov
|
Dynamics of cosmological models with nonlinear classical phantom scalar
fields. II. Qualitative analysis and numerical modeling
|
10 pages, 16 figures
|
Phys J (2019) 61: 2092
|
10.1007/s11182-019-01642-x
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
A detailed qualitative analysis and numerical modeling of the evolution of
cosmological models based on nonlinear classical and phantom scalar fields with
self-action are performed. Complete phase portraits of the corresponding
dynamical systems and their projections onto the Poincar\'e sphere are
constructed. It is shown that the phase trajectories of the corresponding
dynamical systems can, depending on the parameters of the model of the scalar
field, split into bifurcation trajectories along 2, 4, or 6 different dynamical
flows. In the phase space of such systems, regions can appear which are
inaccessible for motion. Here phase trajectories of the phantom scalar field
wind around one of the symmetric foci (centers) while the phase trajectories of
the classical scalar field can have a limit cycle determined by the zero
effective energy corresponding to a Euclidean Universe.
|
[
{
"created": "Wed, 1 May 2019 22:44:56 GMT",
"version": "v1"
}
] |
2019-05-03
|
[
[
"Ignat'ev",
"Yu. G.",
""
],
[
"Agathonov",
"A. A.",
""
]
] |
A detailed qualitative analysis and numerical modeling of the evolution of cosmological models based on nonlinear classical and phantom scalar fields with self-action are performed. Complete phase portraits of the corresponding dynamical systems and their projections onto the Poincar\'e sphere are constructed. It is shown that the phase trajectories of the corresponding dynamical systems can, depending on the parameters of the model of the scalar field, split into bifurcation trajectories along 2, 4, or 6 different dynamical flows. In the phase space of such systems, regions can appear which are inaccessible for motion. Here phase trajectories of the phantom scalar field wind around one of the symmetric foci (centers) while the phase trajectories of the classical scalar field can have a limit cycle determined by the zero effective energy corresponding to a Euclidean Universe.
|
gr-qc/0502021
|
Richard Shurtleff
|
Richard Shurtleff
|
Poincare Connections in Flat Spacetime
|
18 pages, 6 problems, no figures, latex. In version 1, the torsion
survived the arc length formula that in fact destroys it. Some torsion
statements, the abstract, and the introduction are revised and some
typographical errors are fixed in version 2. The torsion problem does not
affect the main results
| null | null | null |
gr-qc
| null |
In flat spacetime, as a simple 4-vector, a particle's 4-velocity cannot be
changed by translation. Parallel translation then produces constant velocity,
motion without force. Here we consider a richer, but less well-known,
representation of the Poincare group of symmetries of flat spacetime in which
translation adds a non-linear connection term to the 4-vector. Then 4-vectors
can be meaningfully parallel translated, curved geodesics can be developed, and
the curvature for the connection can be found. By adding an assumption, that
the arc length is calculated with a position dependent metric, it is shown that
a geodesic has a 4-acceleration which is the sum of a Christoffel connection
term and a term that is the scalar product of 4-velocity and an antisymmetric
tensor. This is just like the force law obeyed by a charged, massive particle
in general relativity. Thus the dynamical laws of electrodynamics and general
relativity can be deduced as geodesic equations from the way particle proper
time depends on position and the way 4-vectors can change upon translation in
flat spacetime.
|
[
{
"created": "Mon, 7 Feb 2005 20:33:49 GMT",
"version": "v1"
},
{
"created": "Sun, 13 Feb 2005 17:04:57 GMT",
"version": "v2"
}
] |
2007-05-23
|
[
[
"Shurtleff",
"Richard",
""
]
] |
In flat spacetime, as a simple 4-vector, a particle's 4-velocity cannot be changed by translation. Parallel translation then produces constant velocity, motion without force. Here we consider a richer, but less well-known, representation of the Poincare group of symmetries of flat spacetime in which translation adds a non-linear connection term to the 4-vector. Then 4-vectors can be meaningfully parallel translated, curved geodesics can be developed, and the curvature for the connection can be found. By adding an assumption, that the arc length is calculated with a position dependent metric, it is shown that a geodesic has a 4-acceleration which is the sum of a Christoffel connection term and a term that is the scalar product of 4-velocity and an antisymmetric tensor. This is just like the force law obeyed by a charged, massive particle in general relativity. Thus the dynamical laws of electrodynamics and general relativity can be deduced as geodesic equations from the way particle proper time depends on position and the way 4-vectors can change upon translation in flat spacetime.
|
0706.3890
|
M Hossain Ali
|
M. Hossain Ali
|
Hawking Radiation via Tunneling from Hot NUT-Kerr-Newman-Kasuya
Spacetime
|
To appear in Class. Quant. Grav
|
Class.Quant.Grav.24:5849-5860,2007
|
10.1088/0264-9381/24/23/008
| null |
gr-qc hep-th
| null |
We study the Hawking thermal spectrum in dragging coordinate system and the
tunneling radiation characteristics of hot NUT-Kerr-Newman-Kasuya spacetime.
The tunneling rates at the event and cosmological horizon are found to be
related to the change of Bekenstein-Hawking entropy. The radiation spectrum is
not pure thermal and thus there is a correction to the Hawking thermal
spectrum.
|
[
{
"created": "Tue, 26 Jun 2007 18:54:45 GMT",
"version": "v1"
},
{
"created": "Sun, 28 Oct 2007 05:33:31 GMT",
"version": "v2"
}
] |
2008-11-26
|
[
[
"Ali",
"M. Hossain",
""
]
] |
We study the Hawking thermal spectrum in dragging coordinate system and the tunneling radiation characteristics of hot NUT-Kerr-Newman-Kasuya spacetime. The tunneling rates at the event and cosmological horizon are found to be related to the change of Bekenstein-Hawking entropy. The radiation spectrum is not pure thermal and thus there is a correction to the Hawking thermal spectrum.
|
2102.03084
|
Ke Wang
|
Ke Wang and Qing-Guo Huang
|
Gravitational Waves from Preheating with Modified Gravitational-wave
Propagation
|
5 pages and 2 figures
| null | null | null |
gr-qc astro-ph.CO hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We investigate how the production of gravitational waves (GWs) is affected by
the GW velocity $(c_T)$ during preheating after inflation. For instance, we
simulate the production of GWs after $\lambda\phi^4$ chaotic inflation, and
find that GW spectrum is enhanced for $c_T<1$, but distorted (suppressed at low
frequency, but enhanced at high frequency) for $c_T>1$.
|
[
{
"created": "Fri, 5 Feb 2021 10:12:18 GMT",
"version": "v1"
},
{
"created": "Mon, 15 Feb 2021 07:44:56 GMT",
"version": "v2"
}
] |
2021-02-16
|
[
[
"Wang",
"Ke",
""
],
[
"Huang",
"Qing-Guo",
""
]
] |
We investigate how the production of gravitational waves (GWs) is affected by the GW velocity $(c_T)$ during preheating after inflation. For instance, we simulate the production of GWs after $\lambda\phi^4$ chaotic inflation, and find that GW spectrum is enhanced for $c_T<1$, but distorted (suppressed at low frequency, but enhanced at high frequency) for $c_T>1$.
|
2010.08837
|
Rosie Hayward
|
Rosie Hayward and Fabio Biancalana
|
New Insights into the Nature of Nonlinear Gravitational Waves
| null | null | null | null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We study the evolution equations for gravitational waves, which are derived
using the full metric to raise and lower indices. This method ensures full
consistency between the Ricci tensor and all gauge restrictions and
requirements, and allows a meaningful expansion of all tensors up to second
order, avoiding several inconsistencies and contradictions observed in previous
work. Taking the harmonic gauge to second order in the perturbation theory
results in a new nonlinear equation. We show that non-trivial solutions to this
equation are necessarily non-plane wave modes with a non-zero trace. These
solutions must contain both longitudinal and transverse components, as both are
permitted by the gauge restrictions.
|
[
{
"created": "Sat, 17 Oct 2020 18:04:13 GMT",
"version": "v1"
},
{
"created": "Mon, 26 Oct 2020 15:28:58 GMT",
"version": "v2"
},
{
"created": "Mon, 30 Nov 2020 12:10:34 GMT",
"version": "v3"
},
{
"created": "Mon, 8 Nov 2021 09:41:20 GMT",
"version": "v4"
}
] |
2021-11-09
|
[
[
"Hayward",
"Rosie",
""
],
[
"Biancalana",
"Fabio",
""
]
] |
We study the evolution equations for gravitational waves, which are derived using the full metric to raise and lower indices. This method ensures full consistency between the Ricci tensor and all gauge restrictions and requirements, and allows a meaningful expansion of all tensors up to second order, avoiding several inconsistencies and contradictions observed in previous work. Taking the harmonic gauge to second order in the perturbation theory results in a new nonlinear equation. We show that non-trivial solutions to this equation are necessarily non-plane wave modes with a non-zero trace. These solutions must contain both longitudinal and transverse components, as both are permitted by the gauge restrictions.
|
gr-qc/9304013
| null |
I. Hauser and F. J. Ernst
|
Gurses' Type (b) Transformations are Neighborhood-Isometries
|
10 pages, LATEX, FJE-93-003
|
Phys.Rev.Lett. 71 (1993) 316-319
|
10.1103/PhysRevLett.71.316
| null |
gr-qc
| null |
Following an idea close to one given by C. G. Torre (private communication),
we prove that Riemannian spaces (M,g) and (M,h) that are related by a Gurses
type (b) transformation [M. Gurses, Phys. Rev. Lett. 70, 367 (1993)] or,
equivalently, by a Torre-Anderson generalized diffeomorphism [C. G. Torre and
I. M. Anderson, Phys. Rev. Lett. xx, xxx (1993)] are neighborhood-isometric,
i.e., every point x in M has a corresponding diffeomorphism phi of a
neighborhood V of x onto a generally different neighborhood W of x such that
phi*(h|W) = g|V.
|
[
{
"created": "Fri, 9 Apr 1993 17:33:14 GMT",
"version": "v1"
}
] |
2009-10-22
|
[
[
"Hauser",
"I.",
""
],
[
"Ernst",
"F. J.",
""
]
] |
Following an idea close to one given by C. G. Torre (private communication), we prove that Riemannian spaces (M,g) and (M,h) that are related by a Gurses type (b) transformation [M. Gurses, Phys. Rev. Lett. 70, 367 (1993)] or, equivalently, by a Torre-Anderson generalized diffeomorphism [C. G. Torre and I. M. Anderson, Phys. Rev. Lett. xx, xxx (1993)] are neighborhood-isometric, i.e., every point x in M has a corresponding diffeomorphism phi of a neighborhood V of x onto a generally different neighborhood W of x such that phi*(h|W) = g|V.
|
1102.1170
|
Re Fiorentin Stefano
|
Stefano Re Fiorentin
|
A re-interpretation of the concept of mass and of the relativistic
mass-energy relation
| null |
Found.Phys.39:1394-1406,2009
|
10.1007/s10701-009-9359-9
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
For over a century the definitions of mass and derivations of its relation
with energy continue to be elaborated, demonstrating that the concept of mass
is still not satisfactorily understood. The aim of this study is to show that,
starting from the properties of Minkowski spacetime and from the principle of
least action, energy expresses the property of inertia of a body. This implies
that inertial mass can only be the object of a definition - the so called
mass-energy relation - aimed at measuring energy in different units, more
suitable to describe the huge amount of it enclosed in what we call the
"rest-energy" of a body. Likewise, the concept of gravitational mass becomes
unnecessary, being replaceable by energy, thus making the weak equivalence
principle intrinsically verified. In dealing with mass, a new unit of
measurement is foretold for it, which relies on the de Broglie frequency of
atoms, the value of which can today be measured with an accuracy of a few parts
in 10^9.
|
[
{
"created": "Sun, 6 Feb 2011 17:07:37 GMT",
"version": "v1"
}
] |
2011-03-10
|
[
[
"Fiorentin",
"Stefano Re",
""
]
] |
For over a century the definitions of mass and derivations of its relation with energy continue to be elaborated, demonstrating that the concept of mass is still not satisfactorily understood. The aim of this study is to show that, starting from the properties of Minkowski spacetime and from the principle of least action, energy expresses the property of inertia of a body. This implies that inertial mass can only be the object of a definition - the so called mass-energy relation - aimed at measuring energy in different units, more suitable to describe the huge amount of it enclosed in what we call the "rest-energy" of a body. Likewise, the concept of gravitational mass becomes unnecessary, being replaceable by energy, thus making the weak equivalence principle intrinsically verified. In dealing with mass, a new unit of measurement is foretold for it, which relies on the de Broglie frequency of atoms, the value of which can today be measured with an accuracy of a few parts in 10^9.
|
2406.15512
|
Otto Kong
|
Otto C.W. Kong (Nat'l Central U, Taiwan)
|
Quantum Mechanics in Curved Space(time) with a Noncommutative Geometric
Perspective
|
24 pages in RevTex, no figure
| null | null |
NCU-HEP-k102
|
gr-qc hep-th quant-ph
|
http://creativecommons.org/licenses/by/4.0/
|
We have previously presented a version of the Weak Equivalence Principle for
a quantum particle as an exact analog of the classical case, based on the
Heisenberg picture analysis of free particle motion. Here, we take that to a
full formalism of quantum mechanics in a generic curved space(time). Our basic
perspective is to take seriously the noncommutative symplectic geometry
corresponding to the quantum observable algebra. Particle position coordinate
transformations and a nontrivial metric assigning an invariant inner product to
vectors, and covectors, are implemented accordingly. That allows an analog to
the classical picture of the phase space as the cotangent bundle. The
mass-independent quantum geodesic equations as equations of free particle
motion under a generic metric as a quantum observable are obtained from an
invariant Hamiltonian. Hermiticity of momentum observables is to be taken as
reference frame dependent. Our results have a big contrast to the alternative
obtained based on the Schr\"odinger wavefunction representation. Hence, the
work points to a very different approach to quantum gravity.
|
[
{
"created": "Thu, 20 Jun 2024 10:44:06 GMT",
"version": "v1"
}
] |
2024-06-25
|
[
[
"Kong",
"Otto C. W.",
"",
"Nat'l Central U, Taiwan"
]
] |
We have previously presented a version of the Weak Equivalence Principle for a quantum particle as an exact analog of the classical case, based on the Heisenberg picture analysis of free particle motion. Here, we take that to a full formalism of quantum mechanics in a generic curved space(time). Our basic perspective is to take seriously the noncommutative symplectic geometry corresponding to the quantum observable algebra. Particle position coordinate transformations and a nontrivial metric assigning an invariant inner product to vectors, and covectors, are implemented accordingly. That allows an analog to the classical picture of the phase space as the cotangent bundle. The mass-independent quantum geodesic equations as equations of free particle motion under a generic metric as a quantum observable are obtained from an invariant Hamiltonian. Hermiticity of momentum observables is to be taken as reference frame dependent. Our results have a big contrast to the alternative obtained based on the Schr\"odinger wavefunction representation. Hence, the work points to a very different approach to quantum gravity.
|
2403.04888
|
Dhruba Jyoti Gogoi Dr.
|
Yassine Sekhmani, Dhruba Jyoti Gogoi, Ratbay Myrzakulov and Javlon
Rayimbaev
|
Phase structures and critical behaviour of rational non-linear
electrodynamics AdS black holes in Rastall gravity
|
23 pages, 7 figures
|
Communications in Theoretical Physics (2024)
|
10.1088/1572-9494/ad30f4
| null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
This research paper presents a black hole solution with a rational non-linear
electrodynamics source in the Rastall gravity framework. The paper analyzes the
thermodynamic properties of the solution in normal phase space and explores its
critical behavior. The phase structure is examined using the extended first law
of thermodynamics, with the cosmological constant $\Lambda$ serving as pressure
$P$. The isotherms exhibit van der Waals behavior at small values of horizon
$r_+$. The paper also investigates the Gibbs free energy behavior and finds two
critical points with two pressures where the reentrant phase transition occurs
and disappears. On the other hand, we explore the prevalent microstructure of
black holes in Ruppeiner geometry, uncovering significant deviations in the
nature of particle interactions from conventional practice. Moreover, the
thermodynamic geometry is analyzed using the Ruppeiner formalism, with the
normalized Ricci scalar indicating possible point-phase transitions of the heat
capacity, and the normalized extrinsic curvature having the same sign as the
normalized Ricci scalar. The three-phase transitions of the heat capacity are
those that we find for the normalized Ruppeiner curvatures. Thus, there is an
absolute correspondence.
|
[
{
"created": "Thu, 7 Mar 2024 20:44:50 GMT",
"version": "v1"
}
] |
2024-03-11
|
[
[
"Sekhmani",
"Yassine",
""
],
[
"Gogoi",
"Dhruba Jyoti",
""
],
[
"Myrzakulov",
"Ratbay",
""
],
[
"Rayimbaev",
"Javlon",
""
]
] |
This research paper presents a black hole solution with a rational non-linear electrodynamics source in the Rastall gravity framework. The paper analyzes the thermodynamic properties of the solution in normal phase space and explores its critical behavior. The phase structure is examined using the extended first law of thermodynamics, with the cosmological constant $\Lambda$ serving as pressure $P$. The isotherms exhibit van der Waals behavior at small values of horizon $r_+$. The paper also investigates the Gibbs free energy behavior and finds two critical points with two pressures where the reentrant phase transition occurs and disappears. On the other hand, we explore the prevalent microstructure of black holes in Ruppeiner geometry, uncovering significant deviations in the nature of particle interactions from conventional practice. Moreover, the thermodynamic geometry is analyzed using the Ruppeiner formalism, with the normalized Ricci scalar indicating possible point-phase transitions of the heat capacity, and the normalized extrinsic curvature having the same sign as the normalized Ricci scalar. The three-phase transitions of the heat capacity are those that we find for the normalized Ruppeiner curvatures. Thus, there is an absolute correspondence.
|
1610.04543
|
Takuya Tsuchiya
|
Takuya Tsuchiya and Gen Yoneda
|
Constructing of constraint preserving scheme for Einstein equations
|
8 pages, 1 figure
|
JSIAM Letters Vol. 9 (2017) p. 57-60
|
10.14495/jsiaml.9.57
| null |
gr-qc math.DS math.NA
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We propose a new numerical scheme of evolution for the Einstein equations
using the discrete variational derivative method (DVDM). We derive the discrete
evolution equation of the constraint using this scheme and show the constraint
preserves in the discrete level. In addition, to confirm the numerical
stability using this scheme, we perform some numerical simulations by
discretized equations with the Crank-Nicolson scheme and with the new scheme,
and we find that the new discretized equations have better stability than that
of the Crank-Nicolson scheme.
|
[
{
"created": "Fri, 14 Oct 2016 17:19:44 GMT",
"version": "v1"
},
{
"created": "Mon, 17 Oct 2016 02:18:33 GMT",
"version": "v2"
},
{
"created": "Fri, 14 Jul 2017 09:08:21 GMT",
"version": "v3"
}
] |
2017-10-24
|
[
[
"Tsuchiya",
"Takuya",
""
],
[
"Yoneda",
"Gen",
""
]
] |
We propose a new numerical scheme of evolution for the Einstein equations using the discrete variational derivative method (DVDM). We derive the discrete evolution equation of the constraint using this scheme and show the constraint preserves in the discrete level. In addition, to confirm the numerical stability using this scheme, we perform some numerical simulations by discretized equations with the Crank-Nicolson scheme and with the new scheme, and we find that the new discretized equations have better stability than that of the Crank-Nicolson scheme.
|
gr-qc/9301002
| null |
Edward Malec
|
Event horizons and apparent horizons in spherically symmetric geometries
|
5 pages, plaintex
|
Phys.Rev.D49:6475-6483,1994
|
10.1103/PhysRevD.49.6475
| null |
gr-qc
| null |
Spherical configurations that are very massive must be surrounded by apparent
horizons. These in turn, when placed outside a collapsing body, must propagate
outward with a velocity equal to the velocity of radially outgoing photons.
That proves, within the framework of (1+3) formalism and without resorting to
the Birkhoff theorem, that apparent horizons coincide with event horizons.
|
[
{
"created": "Wed, 6 Jan 1993 14:47:00 GMT",
"version": "v1"
}
] |
2014-11-17
|
[
[
"Malec",
"Edward",
""
]
] |
Spherical configurations that are very massive must be surrounded by apparent horizons. These in turn, when placed outside a collapsing body, must propagate outward with a velocity equal to the velocity of radially outgoing photons. That proves, within the framework of (1+3) formalism and without resorting to the Birkhoff theorem, that apparent horizons coincide with event horizons.
|
1509.04539
|
Enrico Barausse
|
Enrico Barausse and Kent Yagi
|
Gravitational-wave emission in shift-symmetric Horndeski theories
|
6 pages. Minor changes to match version accepted for publication in
PRL
|
Phys. Rev. Lett. 115, 211105 (2015)
|
10.1103/PhysRevLett.115.211105
| null |
gr-qc astro-ph.CO hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Gravity theories beyond General Relativity typically predict dipolar
gravitational emission by compact-star binaries. This emission is sourced by
"sensitivity" parameters depending on the stellar compactness. We introduce a
general formalism to calculate these parameters, and show that in
shift-symmetric Horndeski theories stellar sensitivities and dipolar radiation
vanish, provided that the binary's dynamics is perturbative (i.e. the
post-Newtonian formalism is applicable) and cosmological-expansion effects can
be neglected. This allows reproducing the binary-pulsar observed orbital decay.
|
[
{
"created": "Tue, 15 Sep 2015 13:25:05 GMT",
"version": "v1"
},
{
"created": "Wed, 4 Nov 2015 22:28:52 GMT",
"version": "v2"
}
] |
2015-11-25
|
[
[
"Barausse",
"Enrico",
""
],
[
"Yagi",
"Kent",
""
]
] |
Gravity theories beyond General Relativity typically predict dipolar gravitational emission by compact-star binaries. This emission is sourced by "sensitivity" parameters depending on the stellar compactness. We introduce a general formalism to calculate these parameters, and show that in shift-symmetric Horndeski theories stellar sensitivities and dipolar radiation vanish, provided that the binary's dynamics is perturbative (i.e. the post-Newtonian formalism is applicable) and cosmological-expansion effects can be neglected. This allows reproducing the binary-pulsar observed orbital decay.
|
gr-qc/0601066
|
Yasusada Nambu
|
H. Furuhashi and Y. Nambu and H. Saida
|
Simulation of Acoustic Black Hole in a Laval Nozzle
|
26 pages, published version
|
Class.Quant.Grav. 23 (2006) 5417-5438
|
10.1088/0264-9381/23/17/018
| null |
gr-qc
| null |
A numerical simulation of fluid flows in a Laval nozzle is performed to
observe formations of acoustic black holes and the classical counterpart to
Hawking radiation under a realistic setting of the laboratory experiment. We
determined the Hawking temperature of the acoustic black hole from obtained
numerical data. Some noteworthy points in analyzing the experimental data are
clarified through our numerical simulation.
|
[
{
"created": "Tue, 17 Jan 2006 03:55:55 GMT",
"version": "v1"
},
{
"created": "Thu, 14 Sep 2006 04:04:52 GMT",
"version": "v2"
}
] |
2009-11-11
|
[
[
"Furuhashi",
"H.",
""
],
[
"Nambu",
"Y.",
""
],
[
"Saida",
"H.",
""
]
] |
A numerical simulation of fluid flows in a Laval nozzle is performed to observe formations of acoustic black holes and the classical counterpart to Hawking radiation under a realistic setting of the laboratory experiment. We determined the Hawking temperature of the acoustic black hole from obtained numerical data. Some noteworthy points in analyzing the experimental data are clarified through our numerical simulation.
|
1211.4337
|
Tehani Finch
|
Tehani K. Finch
|
Coordinate families for the Schwarzschild geometry based on radial
timelike geodesics
|
13 pages and 10 figures. New title and abstract; expanded discussion
on Gautreau-Hoffmann coordinates, and coordinate classifications; figures
added; references added. Submitted for publication
|
Gen.Rel.Grav. 47 (2015) 56
|
10.1007/s10714-015-1891-7
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We explore the connections between various coordinate systems associated with
observers moving inwardly along radial geodesics in the Schwarzschild geometry.
Painlev\'e-Gullstrand (PG) time is adapted to freely falling observers dropped
from rest from infinity; Lake-Martel-Poisson (LMP) time coordinates are adapted
to observers who start at infinity with non-zero initial inward velocity;
Gautreau-Hoffmann (GH) time coordinates are adapted to observers dropped from
rest from a finite distance from the black hole horizon. We construct from
these an LMP family and a proper-time family of time coordinates, the
intersection of which is PG time. We demonstrate that these coordinate families
are distinct, but related, one-parameter generalizations of PG time, and show
linkage to Lema\^itre coordinates as well.
|
[
{
"created": "Mon, 19 Nov 2012 09:05:09 GMT",
"version": "v1"
},
{
"created": "Tue, 23 Dec 2014 03:53:43 GMT",
"version": "v2"
}
] |
2015-06-17
|
[
[
"Finch",
"Tehani K.",
""
]
] |
We explore the connections between various coordinate systems associated with observers moving inwardly along radial geodesics in the Schwarzschild geometry. Painlev\'e-Gullstrand (PG) time is adapted to freely falling observers dropped from rest from infinity; Lake-Martel-Poisson (LMP) time coordinates are adapted to observers who start at infinity with non-zero initial inward velocity; Gautreau-Hoffmann (GH) time coordinates are adapted to observers dropped from rest from a finite distance from the black hole horizon. We construct from these an LMP family and a proper-time family of time coordinates, the intersection of which is PG time. We demonstrate that these coordinate families are distinct, but related, one-parameter generalizations of PG time, and show linkage to Lema\^itre coordinates as well.
|
2009.05012
|
Jorge Ananias Neto
|
Everton M. C. Abreu and Jorge Ananias Neto
|
On the nature of R\'enyi modified entropy and the Incomplete statistics
approach in black holes thermodynamics
|
Extended version. Title changed. To appear in Europhysics Letters
(EPL)
| null | null | null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this work we have investigated the effects of the two highlighted
nongaussian entropies which are the modified R\'enyi entropy and the so-called
Incomplete statistics in the analysis of the thermodynamics of black holes
(BHs). We have obtained the equipartition theorems and after that we obtained
the heat capacities for both approaches. Depending on the values of both
$\lambda-$parameter and $M$, the BH mass, relative to a modified R\'enyi
entropy and, depending on the values of the $q-$parameter and $M$, the
Incomplete entropy can determine if the BH has an unstable thermal equilibrium
or not for each model.
|
[
{
"created": "Thu, 10 Sep 2020 17:20:28 GMT",
"version": "v1"
},
{
"created": "Tue, 13 Apr 2021 00:39:47 GMT",
"version": "v2"
}
] |
2021-04-14
|
[
[
"Abreu",
"Everton M. C.",
""
],
[
"Neto",
"Jorge Ananias",
""
]
] |
In this work we have investigated the effects of the two highlighted nongaussian entropies which are the modified R\'enyi entropy and the so-called Incomplete statistics in the analysis of the thermodynamics of black holes (BHs). We have obtained the equipartition theorems and after that we obtained the heat capacities for both approaches. Depending on the values of both $\lambda-$parameter and $M$, the BH mass, relative to a modified R\'enyi entropy and, depending on the values of the $q-$parameter and $M$, the Incomplete entropy can determine if the BH has an unstable thermal equilibrium or not for each model.
|
0712.0272
|
Julio Cesar Fabris
|
J.C. Fabris, D.F. Jardim, S.V.B. Goncalves
|
Instability of scalar perturbation in a phantomic cosmological scenario
|
Latex file, 6 pages
|
Europhys.Lett.82:69001,2008
|
10.1209/0295-5075/82/69001
| null |
gr-qc astro-ph hep-th
| null |
Scalar perturbations can grow during a phantomic cosmological phase as the
big rip is approached, in spite of the high accelerated expansion regime, if
the equation of state is such that $\frac{p}{\rho} = \alpha < - {5/3}$. It is
shown that such result is independent of the spatial curvature. The perturbed
equations are exactly solved for any value of the curvature parameter $k$ and
of the equation of state parameter $\alpha$. Growing modes are found
asymptotically under the condition $\alpha < - {5/3}$. Since the Hubble radius
decreases in a phantom universe, such result indicates that a phantom scenario
may not survive longtime due to gravitational instability.
|
[
{
"created": "Mon, 3 Dec 2007 12:31:52 GMT",
"version": "v1"
}
] |
2008-11-26
|
[
[
"Fabris",
"J. C.",
""
],
[
"Jardim",
"D. F.",
""
],
[
"Goncalves",
"S. V. B.",
""
]
] |
Scalar perturbations can grow during a phantomic cosmological phase as the big rip is approached, in spite of the high accelerated expansion regime, if the equation of state is such that $\frac{p}{\rho} = \alpha < - {5/3}$. It is shown that such result is independent of the spatial curvature. The perturbed equations are exactly solved for any value of the curvature parameter $k$ and of the equation of state parameter $\alpha$. Growing modes are found asymptotically under the condition $\alpha < - {5/3}$. Since the Hubble radius decreases in a phantom universe, such result indicates that a phantom scenario may not survive longtime due to gravitational instability.
|
gr-qc/0110059
|
Robert T. Jantzen
|
Donato Bini, Robert T Jantzen, Giovanni Miniutti
|
The Cotton, Simon-Mars and Cotton-York Tensors in Stationary Spacetimes
|
14 pages latex(2e) iopart style, no figures
|
Class.Quant.Grav. 18 (2001) 4969
|
10.1088/0264-9381/18/22/317
| null |
gr-qc
| null |
The Cotton-York and Simon-Mars tensors in stationary vacuum spacetimes are
studied in the language of the congruence approach pioneered by Hawking and
Ellis. Their relationships with the Papapetrou field defined by the stationary
Killing congruence and with a recent characterization of the Kerr spacetime in
terms of the alignment between of the principal null directions of the Weyl
tensor with those of the Papapetrou field are also investigated in this more
transparent language.
|
[
{
"created": "Thu, 11 Oct 2001 15:21:05 GMT",
"version": "v1"
}
] |
2009-11-07
|
[
[
"Bini",
"Donato",
""
],
[
"Jantzen",
"Robert T",
""
],
[
"Miniutti",
"Giovanni",
""
]
] |
The Cotton-York and Simon-Mars tensors in stationary vacuum spacetimes are studied in the language of the congruence approach pioneered by Hawking and Ellis. Their relationships with the Papapetrou field defined by the stationary Killing congruence and with a recent characterization of the Kerr spacetime in terms of the alignment between of the principal null directions of the Weyl tensor with those of the Papapetrou field are also investigated in this more transparent language.
|
1302.3833
|
Alejandro Corichi
|
Ivan Agullo and Alejandro Corichi
|
Loop Quantum Cosmology
|
To appear as a Chapter of "The Springer Handbook of Spacetime,"
edited by A. Ashtekar and V. Petkov. (Springer-Verlag, at Press). 52 pages, 5
figures
| null |
10.1007/978-3-642-41992-8_39
| null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
This Chapter provides an up to date, pedagogical review of some of the most
relevant advances in loop quantum cosmology. We review the quantization of
homogeneous cosmological models, their singularity resolution and the
formulation of effective equations that incorporate the main quantum
corrections to the dynamics. We also summarize the theory of quantized metric
perturbations propagating in those quantum backgrounds. Finally, we describe
how this framework can be applied to obtain a self-consistent extension of the
inflationary scenario to incorporate quantum aspects of gravity, and to explore
possible phenomenological consequences.
|
[
{
"created": "Fri, 15 Feb 2013 18:20:53 GMT",
"version": "v1"
}
] |
2015-06-15
|
[
[
"Agullo",
"Ivan",
""
],
[
"Corichi",
"Alejandro",
""
]
] |
This Chapter provides an up to date, pedagogical review of some of the most relevant advances in loop quantum cosmology. We review the quantization of homogeneous cosmological models, their singularity resolution and the formulation of effective equations that incorporate the main quantum corrections to the dynamics. We also summarize the theory of quantized metric perturbations propagating in those quantum backgrounds. Finally, we describe how this framework can be applied to obtain a self-consistent extension of the inflationary scenario to incorporate quantum aspects of gravity, and to explore possible phenomenological consequences.
|
1811.01391
|
Plyatsko Roman
|
Roman Plyatsko, Volodymyr Panat, Mykola Fenyk
|
Nonequatorial circular orbits of spinning particles in the
Schwarzschild-de Sitter background
|
18 pages
|
Gen. Relativ. Gravit. 2018, 50:150
|
10.1007/s10714-018-2474-1
| null |
gr-qc astro-ph.HE hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this paper analytical solutions of the Mathisson-Papapetrou equations that
describe nonequatorial circular orbits of a spinning particle in the
Schwarzschild-de Sitter background are studied, and the role of the
cosmological constant is emphasized. It is shown that generally speaking a
highly relativistic velocity of the particle is a necessary condition of motion
along this type of orbits, with an exception of orbits locating close to the
position of the static equilibrium, where low velocities are possible as well.
Depending on the correlation between the spin orientation of the particle and
its orbital velocity some of the possible nonequatorial circular orbits exist
due to the repulsive action on the particle caused by the spin-gravity coupling
and the others are caused by the attractive action.Here values of the energy of
the particle on the corresponding orbits are also analyzed.
|
[
{
"created": "Sun, 4 Nov 2018 16:00:26 GMT",
"version": "v1"
},
{
"created": "Sat, 1 Dec 2018 18:10:15 GMT",
"version": "v2"
}
] |
2018-12-04
|
[
[
"Plyatsko",
"Roman",
""
],
[
"Panat",
"Volodymyr",
""
],
[
"Fenyk",
"Mykola",
""
]
] |
In this paper analytical solutions of the Mathisson-Papapetrou equations that describe nonequatorial circular orbits of a spinning particle in the Schwarzschild-de Sitter background are studied, and the role of the cosmological constant is emphasized. It is shown that generally speaking a highly relativistic velocity of the particle is a necessary condition of motion along this type of orbits, with an exception of orbits locating close to the position of the static equilibrium, where low velocities are possible as well. Depending on the correlation between the spin orientation of the particle and its orbital velocity some of the possible nonequatorial circular orbits exist due to the repulsive action on the particle caused by the spin-gravity coupling and the others are caused by the attractive action.Here values of the energy of the particle on the corresponding orbits are also analyzed.
|
gr-qc/0210016
|
Marcelo J. Reboucas
|
G.I. Gomero, M.J. Reboucas, R. Tavakol
|
Limits on the Detectability of Cosmic Topology in Hyperbolic Universes
|
10 pages, 2 figures, LaTeX2e. To appear in Int. J. Mod. Phys. A
(2002). Contribution to the Fifth Alexander Friedmann International Seminar
on Gravitation and Cosmology
|
Int.J.Mod.Phys. A17 (2002) 4261-4272
|
10.1142/S0217751X02013307
|
CBPF-NF-026/02
|
gr-qc astro-ph hep-th math-ph math.MP
| null |
We reexamine the possibility of the detection of the cosmic topology in
nearly flat hyperbolic Friedmann-Lemaitre-Robertson-Walker (FLRW) universes by
using patterns repetition. We update and extend our recent results in two
important ways: by employing recent observational constraints on the
cosmological density parameters as well as the recent mathematical results
concerning small hyperbolic 3-manifolds. This produces new bounds with
consequences for the detectability of the cosmic topology. In addition to
obtaining new bounds, we also give a concrete example of the sensitive
dependence of detectability of cosmic topology on the uncertainties in the
observational values of the density parameters.
|
[
{
"created": "Fri, 4 Oct 2002 23:31:56 GMT",
"version": "v1"
}
] |
2009-11-07
|
[
[
"Gomero",
"G. I.",
""
],
[
"Reboucas",
"M. J.",
""
],
[
"Tavakol",
"R.",
""
]
] |
We reexamine the possibility of the detection of the cosmic topology in nearly flat hyperbolic Friedmann-Lemaitre-Robertson-Walker (FLRW) universes by using patterns repetition. We update and extend our recent results in two important ways: by employing recent observational constraints on the cosmological density parameters as well as the recent mathematical results concerning small hyperbolic 3-manifolds. This produces new bounds with consequences for the detectability of the cosmic topology. In addition to obtaining new bounds, we also give a concrete example of the sensitive dependence of detectability of cosmic topology on the uncertainties in the observational values of the density parameters.
|
2106.07128
|
Kazufumi Takahashi
|
Kazufumi Takahashi, Hayato Motohashi
|
Black hole perturbations in DHOST theories: Master variables, gradient
instability, and strong coupling
|
25 pages
|
JCAP 08 (2021) 013
|
10.1088/1475-7516/2021/08/013
|
YITP-21-38
|
gr-qc hep-th
|
http://creativecommons.org/licenses/by/4.0/
|
We study linear perturbations about static and spherically symmetric black
hole solutions with stealth scalar hair in degenerate higher-order
scalar-tensor (DHOST) theories. We clarify master variables and derive the
quadratic Lagrangian for both odd- and even-parity perturbations. It is shown
that the even modes are in general plagued by gradient instabilities, or
otherwise the perturbations would be strongly coupled. Several possible ways
out are also discussed.
|
[
{
"created": "Mon, 14 Jun 2021 01:37:03 GMT",
"version": "v1"
},
{
"created": "Tue, 10 Aug 2021 13:34:32 GMT",
"version": "v2"
}
] |
2021-08-11
|
[
[
"Takahashi",
"Kazufumi",
""
],
[
"Motohashi",
"Hayato",
""
]
] |
We study linear perturbations about static and spherically symmetric black hole solutions with stealth scalar hair in degenerate higher-order scalar-tensor (DHOST) theories. We clarify master variables and derive the quadratic Lagrangian for both odd- and even-parity perturbations. It is shown that the even modes are in general plagued by gradient instabilities, or otherwise the perturbations would be strongly coupled. Several possible ways out are also discussed.
|
1712.07978
|
Freddy Cueva Solano
|
Freddy Cueva Solano
|
Modeling interacting dark energy models with Chebyshev polynomials:
Exploring their constraints and effects
|
15pages,7 figures,Submitted for PRD. arXiv admin note: text overlap
with arXiv:1612.02484
| null | null | null |
gr-qc
|
http://creativecommons.org/publicdomain/zero/1.0/
|
In this work, we examine the main cosmological effects derived from a
time-varying coupling ($\bar{Q}$) between a dark matter (DM) fluid and a dark
energy (DE) fluid with time-varying DE equation state (EoS) parameter
($\omega_{DE}$), in two different coupled DE models. These scenarios were built
in terms of Chebyschev polynomials. Our results show that such models within
dark sector can suffer an instability in their perturbations at early times and
a slight departure on the amplitude of the cosmic structure growth
($f\sigma_{8}$) from the standard background evolution of the matter. These
effects depend on the form of both $\bar{Q}$ and $\omega_{DE}$. Here, we also
perform a combined statistical analysis using current data to put tighter
constraints on the parameters space. Finally, we use some selections criteria
to distinguish our models.
|
[
{
"created": "Tue, 19 Dec 2017 22:33:05 GMT",
"version": "v1"
}
] |
2017-12-22
|
[
[
"Solano",
"Freddy Cueva",
""
]
] |
In this work, we examine the main cosmological effects derived from a time-varying coupling ($\bar{Q}$) between a dark matter (DM) fluid and a dark energy (DE) fluid with time-varying DE equation state (EoS) parameter ($\omega_{DE}$), in two different coupled DE models. These scenarios were built in terms of Chebyschev polynomials. Our results show that such models within dark sector can suffer an instability in their perturbations at early times and a slight departure on the amplitude of the cosmic structure growth ($f\sigma_{8}$) from the standard background evolution of the matter. These effects depend on the form of both $\bar{Q}$ and $\omega_{DE}$. Here, we also perform a combined statistical analysis using current data to put tighter constraints on the parameters space. Finally, we use some selections criteria to distinguish our models.
|
gr-qc/0312005
|
Dan Brown
|
Daniel Brown
|
A Graph Model for the quantum mechanics of a moving cyclic disturbance
interacting at a spatial position
|
17 pages, 2 figures
| null | null | null |
gr-qc
| null |
An analysis is made of a moving disturbance using a directed cyclic graph.
A statistical approach is used to calculate the alternative positions in
space and state of the disturbance with a defined observed time. The
probability for a freely moving entity interacting in a particular spatial
position is calculated and a formulation is derived for the minimum locus of
uncertainty in position and momentum. This is found to accord with calculations
for quantum mechanics. The model has proven amenable to computer modelling; a
copy of the "SimulTime" program is available on request.
|
[
{
"created": "Sun, 30 Nov 2003 20:45:12 GMT",
"version": "v1"
},
{
"created": "Tue, 9 Mar 2004 16:37:59 GMT",
"version": "v2"
},
{
"created": "Thu, 12 Aug 2004 11:09:09 GMT",
"version": "v3"
},
{
"created": "Mon, 20 Mar 2006 09:36:54 GMT",
"version": "v4"
},
{
"created": "Fri, 24 Mar 2006 12:28:20 GMT",
"version": "v5"
}
] |
2007-05-23
|
[
[
"Brown",
"Daniel",
""
]
] |
An analysis is made of a moving disturbance using a directed cyclic graph. A statistical approach is used to calculate the alternative positions in space and state of the disturbance with a defined observed time. The probability for a freely moving entity interacting in a particular spatial position is calculated and a formulation is derived for the minimum locus of uncertainty in position and momentum. This is found to accord with calculations for quantum mechanics. The model has proven amenable to computer modelling; a copy of the "SimulTime" program is available on request.
|
gr-qc/0305021
|
Marcus S. Cohen
|
Marcus S. Cohen
|
Clifford Tetrads, Null Zig Zags, and Quantum Gravity
|
32 pages, submitted to Advances in Applied Clifford Algebras
| null | null | null |
gr-qc
| null |
Quantum Gravity has been so elusive because we have tried to approach it by
two paths which can never meet: standard quantum field theory and general
relativity. The gateway is covariance under the complexified Clifford algebra
of our space-time manifold M, and its spinor representations, which Sachs
dubbed the Einstein group, E. On the microscopic scale, quantum gravity appears
as the statistical mechanics of the null zig-zag rays of spinor fields in
imaginary time T. Our unified field/particle action L_g also contains new
couplings of gravitomagnetic fields to strong fields and weak potentials. These
predict new physical phenomena: Axial jets of nuclear decay products emitted
with left helicity along the axis of a massive, spinning body.
|
[
{
"created": "Mon, 5 May 2003 18:43:45 GMT",
"version": "v1"
}
] |
2007-05-23
|
[
[
"Cohen",
"Marcus S.",
""
]
] |
Quantum Gravity has been so elusive because we have tried to approach it by two paths which can never meet: standard quantum field theory and general relativity. The gateway is covariance under the complexified Clifford algebra of our space-time manifold M, and its spinor representations, which Sachs dubbed the Einstein group, E. On the microscopic scale, quantum gravity appears as the statistical mechanics of the null zig-zag rays of spinor fields in imaginary time T. Our unified field/particle action L_g also contains new couplings of gravitomagnetic fields to strong fields and weak potentials. These predict new physical phenomena: Axial jets of nuclear decay products emitted with left helicity along the axis of a massive, spinning body.
|
1112.6349
|
Ernesto F. Eiroa
|
Leonardo Amarilla, Ernesto F. Eiroa
|
Shadow of a rotating braneworld black hole
|
11 pages, 6 figures. v2: improved version (includes 2 new figures)
|
Phys.Rev.D85:064019,2012
|
10.1103/PhysRevD.85.064019
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We investigate the shadow cast by a rotating braneworld black hole, in the
Randall-Sundrum scenario. In addition to the angular momentum, the tidal charge
term deforms the shape of the shadow. For a given value of the rotation
parameter, the presence of a negative tidal charge enlarges the shadow and
reduces its deformation with respect to Kerr spacetime, while for a positive
charge, the opposite effect is obtained. We also analyze the case in which the
combination of the rotation parameter and the tidal charge results in a naked
singularity. We discuss the observational prospects corresponding to the
supermassive black hole at the Galactic center.
|
[
{
"created": "Thu, 29 Dec 2011 17:09:00 GMT",
"version": "v1"
},
{
"created": "Fri, 16 Mar 2012 15:08:01 GMT",
"version": "v2"
}
] |
2012-03-19
|
[
[
"Amarilla",
"Leonardo",
""
],
[
"Eiroa",
"Ernesto F.",
""
]
] |
We investigate the shadow cast by a rotating braneworld black hole, in the Randall-Sundrum scenario. In addition to the angular momentum, the tidal charge term deforms the shape of the shadow. For a given value of the rotation parameter, the presence of a negative tidal charge enlarges the shadow and reduces its deformation with respect to Kerr spacetime, while for a positive charge, the opposite effect is obtained. We also analyze the case in which the combination of the rotation parameter and the tidal charge results in a naked singularity. We discuss the observational prospects corresponding to the supermassive black hole at the Galactic center.
|
1503.07556
|
Shannon Ray
|
Shannon Ray, Warner A. Miller, Paul M. Alsing and Shing-Tung Yau
|
Adiabatic Isometric Mapping Algorithm for Embedding 2-Surfaces in
Euclidean 3-Space
|
This version has updated figures and corrected typos
| null |
10.1088/0264-9381/32/23/235012
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Alexandrov proved that any simplicial complex homeomorphic to a sphere with
strictly non-negative Gaussian curvature at each vertex can be isometrically
embedded uniquely in $\mathbb{R}^3$ as a convex polyhedron. Due to the
nonconstructive nature of his proof, there have yet to be any algorithms, that
we know of, that realizes the Alexandrov embedding in polynomial time.
Following his proof, we developed the adiabatic isometric mapping (AIM)
algorithm. AIM uses a guided adiabatic pull-back procedure to produce "smooth"
embeddings. Tests of AIM applied to two different polyhedral metrics suggests
that its run time is sub cubic with respect to the number of vertices. Although
Alexandrov's theorem specifically addresses the embedding of convex polyhedral
metrics, we tested AIM on a broader class of polyhedral metrics that included
regions of negative Gaussian curvature. One test was on a surface just outside
the ergosphere of a Kerr black hole.
|
[
{
"created": "Wed, 25 Mar 2015 21:02:18 GMT",
"version": "v1"
},
{
"created": "Thu, 26 Oct 2017 19:45:23 GMT",
"version": "v2"
}
] |
2017-10-30
|
[
[
"Ray",
"Shannon",
""
],
[
"Miller",
"Warner A.",
""
],
[
"Alsing",
"Paul M.",
""
],
[
"Yau",
"Shing-Tung",
""
]
] |
Alexandrov proved that any simplicial complex homeomorphic to a sphere with strictly non-negative Gaussian curvature at each vertex can be isometrically embedded uniquely in $\mathbb{R}^3$ as a convex polyhedron. Due to the nonconstructive nature of his proof, there have yet to be any algorithms, that we know of, that realizes the Alexandrov embedding in polynomial time. Following his proof, we developed the adiabatic isometric mapping (AIM) algorithm. AIM uses a guided adiabatic pull-back procedure to produce "smooth" embeddings. Tests of AIM applied to two different polyhedral metrics suggests that its run time is sub cubic with respect to the number of vertices. Although Alexandrov's theorem specifically addresses the embedding of convex polyhedral metrics, we tested AIM on a broader class of polyhedral metrics that included regions of negative Gaussian curvature. One test was on a surface just outside the ergosphere of a Kerr black hole.
|
1812.11264
|
I. V. Kanatchikov
|
I.V. Kanatchikov
|
Precanonical structure of the Schr\"odinger wave functional in curved
space-time
|
13 pages. arXiv admin note: text overlap with arXiv:1810.09968
| null | null | null |
gr-qc math-ph math.MP
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
A relationship between the functional Schr\"odinger representation and the
precanonical quantization of a scalar field theory is extended to an arbitrary
curved space-time. The canonical functional derivative Schr\"odinger equation
is derived from the manifestly covariant precanonical Schr\"odinger equation
and the Schr\"odinger wave functional is expressed as the trace of the product
integral of Clifford-algebra-valued precanonical wave functions restricted to a
certain field configuration when the ultraviolet parameter $\varkappa$
introduced in precanonical quantization is infinite. Thus the standard QFT in
functional Schr\"odinger representation emerges from the precanonical
formulation of quantum fields as a singular limiting case.
|
[
{
"created": "Sat, 29 Dec 2018 01:55:14 GMT",
"version": "v1"
}
] |
2019-02-08
|
[
[
"Kanatchikov",
"I. V.",
""
]
] |
A relationship between the functional Schr\"odinger representation and the precanonical quantization of a scalar field theory is extended to an arbitrary curved space-time. The canonical functional derivative Schr\"odinger equation is derived from the manifestly covariant precanonical Schr\"odinger equation and the Schr\"odinger wave functional is expressed as the trace of the product integral of Clifford-algebra-valued precanonical wave functions restricted to a certain field configuration when the ultraviolet parameter $\varkappa$ introduced in precanonical quantization is infinite. Thus the standard QFT in functional Schr\"odinger representation emerges from the precanonical formulation of quantum fields as a singular limiting case.
|
1501.06234
|
Leo Medeiros Gouvea
|
R. R. Cuzinatto, C. A. M. de Melo, K. C. de Vasconcelos, L. G.
Medeiros, P. J. Pompeia
|
Non-linear effects on radiation propagation around a charged compact
object
|
7 pages, no figures, new references added, minor corrections in some
equations
|
Astrophys. Space Sci. v.359 p.59 (2015)
|
10.1007/s10509-015-2505-2
| null |
gr-qc astro-ph.HE astro-ph.SR hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The propagation of non-linear electromagnetic waves is carefully analyzed on
a curved spacetime created by static spherically symmetric mass and charge
distribution. We compute how non-linear electrodynamics affects the geodesic
deviation and the redshift of photons propagating near this massive charged
object. In the first order approximation, the effects of electromagnetic
self-interaction can be distinguished from the usual Reissner-Nordstr\"om
terms. In the particular case of Euler-Heisenberg effective Lagrangian, we find
that these self-interaction effects might be important near extremal compact
charged objects.
|
[
{
"created": "Mon, 26 Jan 2015 02:09:57 GMT",
"version": "v1"
},
{
"created": "Sun, 26 Apr 2015 04:56:24 GMT",
"version": "v2"
},
{
"created": "Thu, 22 Dec 2016 04:47:23 GMT",
"version": "v3"
}
] |
2016-12-23
|
[
[
"Cuzinatto",
"R. R.",
""
],
[
"de Melo",
"C. A. M.",
""
],
[
"de Vasconcelos",
"K. C.",
""
],
[
"Medeiros",
"L. G.",
""
],
[
"Pompeia",
"P. J.",
""
]
] |
The propagation of non-linear electromagnetic waves is carefully analyzed on a curved spacetime created by static spherically symmetric mass and charge distribution. We compute how non-linear electrodynamics affects the geodesic deviation and the redshift of photons propagating near this massive charged object. In the first order approximation, the effects of electromagnetic self-interaction can be distinguished from the usual Reissner-Nordstr\"om terms. In the particular case of Euler-Heisenberg effective Lagrangian, we find that these self-interaction effects might be important near extremal compact charged objects.
|
2209.05905
|
Karim Thebault
|
Karim P. Y. Thebault
|
Big Bang Singularity Resolution In Quantum Cosmology
|
forthcoming in Classical and Quantum Gravity
| null |
10.1088/1361-6382/acb752
| null |
gr-qc
|
http://creativecommons.org/licenses/by/4.0/
|
We evaluate the physical viability and logical strength of an array of
putative criteria for big bang singularity resolution in quantum cosmology.
Based on this analysis, we propose a mutually consistent set of constitutive
conditions, which we argue should be taken to jointly define `global' and
`local' big bang singularity resolution in this context. Whilst the present
article will focus exclusively on evaluating resolution criteria for big bang
singularities in the context of finite dimensional models of quantum cosmology,
it is also hoped that the core features of our analysis will be extendable to a
more general analysis of criteria for quantum singularity resolution in
cosmology and black hole physics.
|
[
{
"created": "Tue, 13 Sep 2022 11:39:45 GMT",
"version": "v1"
},
{
"created": "Thu, 26 Jan 2023 09:28:51 GMT",
"version": "v2"
}
] |
2023-02-22
|
[
[
"Thebault",
"Karim P. Y.",
""
]
] |
We evaluate the physical viability and logical strength of an array of putative criteria for big bang singularity resolution in quantum cosmology. Based on this analysis, we propose a mutually consistent set of constitutive conditions, which we argue should be taken to jointly define `global' and `local' big bang singularity resolution in this context. Whilst the present article will focus exclusively on evaluating resolution criteria for big bang singularities in the context of finite dimensional models of quantum cosmology, it is also hoped that the core features of our analysis will be extendable to a more general analysis of criteria for quantum singularity resolution in cosmology and black hole physics.
|
gr-qc/0011016
|
Yavuz Nutku
|
A. N. Aliev and Y. Nutku
|
Impulsive spherical gravitational waves
| null |
Class.Quant.Grav. 18 (2001) 891-906
|
10.1088/0264-9381/18/5/308
| null |
gr-qc
| null |
Penrose's identification with warp provides the general framework for
constructing the continuous form of impulsive gravitational wave metrics. We
present the 2-component spinor formalism for the derivation of the full family
of impulsive spherical gravitational wave metrics which brings out the power in
identification with warp and leads to the simplest derivation of exact
solutions. These solutions of the Einstein vacuum field equations are obtained
by cutting Minkowski space into two pieces along a null cone and re-identifying
them with warp which is given by an arbitrary non-linear holomorphic
transformation. Using 2-component spinor techniques we construct a new metric
describing an impulsive spherical gravitational wave where the vertex of the
null cone lies on a world-line with constant acceleration.
|
[
{
"created": "Mon, 6 Nov 2000 13:39:45 GMT",
"version": "v1"
}
] |
2009-10-31
|
[
[
"Aliev",
"A. N.",
""
],
[
"Nutku",
"Y.",
""
]
] |
Penrose's identification with warp provides the general framework for constructing the continuous form of impulsive gravitational wave metrics. We present the 2-component spinor formalism for the derivation of the full family of impulsive spherical gravitational wave metrics which brings out the power in identification with warp and leads to the simplest derivation of exact solutions. These solutions of the Einstein vacuum field equations are obtained by cutting Minkowski space into two pieces along a null cone and re-identifying them with warp which is given by an arbitrary non-linear holomorphic transformation. Using 2-component spinor techniques we construct a new metric describing an impulsive spherical gravitational wave where the vertex of the null cone lies on a world-line with constant acceleration.
|
1011.0061
|
Gerard Hooft 't
|
Gerard 't Hooft
|
The Conformal Constraint in Canonical Quantum Gravity
| null | null | null | null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Perturbative canonical quantum gravity is considered, when coupled to a
renormalizable model for matter fields. It is proposed that the functional
integral over the dilaton field should be disentangled from the other
integrations over the metric fields. This should generate a conformally
invariant theory as an intermediate result, where the conformal anomalies must
be constrained to cancel out. When the residual metric is treated as a
background, and if this background is taken to be flat, this leads to a novel
constraint: in combination with the dilaton contributions, the matter
lagrangian should have a vanishing beta function. The zeros of this beta
function are isolated points in the landscape of quantum field theories, and so
we arrive at a denumerable, or perhaps even finite, set of quantum theories for
matter, where not only the coupling constants, but also the masses and the
cosmological constant are all fixed, and computable, in terms of the Planck
units.
|
[
{
"created": "Sat, 30 Oct 2010 11:22:42 GMT",
"version": "v1"
}
] |
2010-11-02
|
[
[
"Hooft",
"Gerard 't",
""
]
] |
Perturbative canonical quantum gravity is considered, when coupled to a renormalizable model for matter fields. It is proposed that the functional integral over the dilaton field should be disentangled from the other integrations over the metric fields. This should generate a conformally invariant theory as an intermediate result, where the conformal anomalies must be constrained to cancel out. When the residual metric is treated as a background, and if this background is taken to be flat, this leads to a novel constraint: in combination with the dilaton contributions, the matter lagrangian should have a vanishing beta function. The zeros of this beta function are isolated points in the landscape of quantum field theories, and so we arrive at a denumerable, or perhaps even finite, set of quantum theories for matter, where not only the coupling constants, but also the masses and the cosmological constant are all fixed, and computable, in terms of the Planck units.
|
2308.12811
|
Jansen Formiga
|
J. B. Formiga and Jo\~ao Duarte
|
On the gravitational energy problem and the energy of photons
|
It has been published in Physical Review D under the title
Gravitational energy problem and the energy of photons
|
Phys. Rev. D 108, 044043 (2023)
|
10.1103/PhysRevD.108.044043
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The lack of a well-established solution for the gravitational energy problem
might be one of the reasons why a clear road to quantum gravity does not exist.
In this paper, the gravitational energy is studied in detail with the help of
the teleparallel approach that is equivalent to general relativity. This
approach is applied to the solutions of the Einstein-Maxwell equations known as
$pp$-wave spacetimes. The quantization of the electromagnetic energy is assumed
and it is shown that the proper area measured by an observer must satisfy an
equation for consistency. The meaning of this equation is discussed and it is
argued that the spacetime geometry should become discrete once all matter
fields are quantized, including the constituents of the frame; it is shown that
for a harmonic oscillation with wavelength $\lambda_0$, the area and the volume
take the form $A=4(N+1/2)l_p^2/n$ and $V=2(N+1/2)l_p^2\lambda_0$, where $N$ is
the number of photons, $l_p$ the Planck length, and $n$ is a natural number
associated with the length along the $z$-axis of a box with cross-sectional
area $A$. The localization of the gravitational energy problem is also
discussed. The stress-energy tensors for the gravitational and electromagnetic
fields are decomposed into energy density, pressures and heat flow. The
resultant expressions are consistent with the properties of the fields, thus
indicating that one can have a well-defined energy density for the
gravitational field regardless of the principle of equivalence.
|
[
{
"created": "Thu, 24 Aug 2023 14:14:59 GMT",
"version": "v1"
}
] |
2023-08-25
|
[
[
"Formiga",
"J. B.",
""
],
[
"Duarte",
"João",
""
]
] |
The lack of a well-established solution for the gravitational energy problem might be one of the reasons why a clear road to quantum gravity does not exist. In this paper, the gravitational energy is studied in detail with the help of the teleparallel approach that is equivalent to general relativity. This approach is applied to the solutions of the Einstein-Maxwell equations known as $pp$-wave spacetimes. The quantization of the electromagnetic energy is assumed and it is shown that the proper area measured by an observer must satisfy an equation for consistency. The meaning of this equation is discussed and it is argued that the spacetime geometry should become discrete once all matter fields are quantized, including the constituents of the frame; it is shown that for a harmonic oscillation with wavelength $\lambda_0$, the area and the volume take the form $A=4(N+1/2)l_p^2/n$ and $V=2(N+1/2)l_p^2\lambda_0$, where $N$ is the number of photons, $l_p$ the Planck length, and $n$ is a natural number associated with the length along the $z$-axis of a box with cross-sectional area $A$. The localization of the gravitational energy problem is also discussed. The stress-energy tensors for the gravitational and electromagnetic fields are decomposed into energy density, pressures and heat flow. The resultant expressions are consistent with the properties of the fields, thus indicating that one can have a well-defined energy density for the gravitational field regardless of the principle of equivalence.
|
2303.10352
|
Shaobo Zhang
|
Shaobo Zhang, Zengli Ba, Denghui Ning, Nianfu Zhai, Zhengtian Lu, Dong
Sheng
|
Search for spin-dependent gravitational interactions at the Earth range
|
Accepted by Physical Review Letters
| null |
10.1103/PhysRevLett.130.201401
| null |
gr-qc hep-ex physics.atom-ph
|
http://creativecommons.org/licenses/by/4.0/
|
Among the four fundamental forces, only gravity does not couple to particle
spins according to the general theory of relativity. We test this principle by
searching for an anomalous scalar coupling between the neutron spin and the
Earth gravity on the ground. We develop an atomic gas comagnetometer to measure
the ratio of nuclear spin-precession frequencies between $^{129}$Xe and
$^{131}$Xe, and search for a change of this ratio to the precision of 10$^{-9}$
as the sensor is flipped in the Earth gravitational field. The null results of
this search set an upper limit on the coupling energy between the neutron spin
and the gravity on the ground at 5.3$\times$10$^{-22}$~eV (95\% confidence
level), resulting in a 17-fold improvement over the previous limit. The results
can also be used to constrain several other anomalous interactions. In
particular, the limit on the coupling strength of axion-mediated
monopole-dipole interactions at the range of the Earth radius is improved by a
factor of 17.
|
[
{
"created": "Sat, 18 Mar 2023 07:13:31 GMT",
"version": "v1"
}
] |
2023-05-24
|
[
[
"Zhang",
"Shaobo",
""
],
[
"Ba",
"Zengli",
""
],
[
"Ning",
"Denghui",
""
],
[
"Zhai",
"Nianfu",
""
],
[
"Lu",
"Zhengtian",
""
],
[
"Sheng",
"Dong",
""
]
] |
Among the four fundamental forces, only gravity does not couple to particle spins according to the general theory of relativity. We test this principle by searching for an anomalous scalar coupling between the neutron spin and the Earth gravity on the ground. We develop an atomic gas comagnetometer to measure the ratio of nuclear spin-precession frequencies between $^{129}$Xe and $^{131}$Xe, and search for a change of this ratio to the precision of 10$^{-9}$ as the sensor is flipped in the Earth gravitational field. The null results of this search set an upper limit on the coupling energy between the neutron spin and the gravity on the ground at 5.3$\times$10$^{-22}$~eV (95\% confidence level), resulting in a 17-fold improvement over the previous limit. The results can also be used to constrain several other anomalous interactions. In particular, the limit on the coupling strength of axion-mediated monopole-dipole interactions at the range of the Earth radius is improved by a factor of 17.
|
1206.5229
|
Frank B. Estabrook
|
Frank B. Estabrook
|
Specialized Orthonormal Frames and Embedding
| null |
SIGMA 9 (2013), 012, 5 pages
|
10.3842/SIGMA.2013.012
| null |
gr-qc math-ph math.MP
|
http://creativecommons.org/licenses/by-nc-sa/3.0/
|
We discuss some specializations of the frames of flat orthonormal frame
bundles over geometries of indefinite signature, and the resulting symmetries
of families of embedded Riemannian or pseudo-Riemannian geometries. The
specializations are closed sets of linear constraints on the connection 1-forms
of the framing. The embeddings can be isometric, as in minimal surfaces or
Regge-Teitelboim gravity, or torsion-free, as in Einstein vacuum gravity.
Involutive exterior differential systems are given, and their Cartan character
tables calculated to express the well-posedness of the underlying partial
differential embedding and specialization equations.
|
[
{
"created": "Fri, 22 Jun 2012 18:44:14 GMT",
"version": "v1"
},
{
"created": "Fri, 15 Feb 2013 06:28:50 GMT",
"version": "v2"
}
] |
2013-02-18
|
[
[
"Estabrook",
"Frank B.",
""
]
] |
We discuss some specializations of the frames of flat orthonormal frame bundles over geometries of indefinite signature, and the resulting symmetries of families of embedded Riemannian or pseudo-Riemannian geometries. The specializations are closed sets of linear constraints on the connection 1-forms of the framing. The embeddings can be isometric, as in minimal surfaces or Regge-Teitelboim gravity, or torsion-free, as in Einstein vacuum gravity. Involutive exterior differential systems are given, and their Cartan character tables calculated to express the well-posedness of the underlying partial differential embedding and specialization equations.
|
1005.1432
|
Paul O'Hara
|
Paul O'Hara
|
Non-geodesic Motion in General Relativity and Thermodynamics
|
11 pages
| null | null | null |
gr-qc quant-ph
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In a previous article a relationship was established between the linearized
metrics of General Relativity associated with geodesics and the Dirac Equation
of quantum mechanics. In this paper the extension of that result to arbitrary
curves is investigated. In the case of scalar fields, a relationship between
mass and temperature is also worked out.
|
[
{
"created": "Mon, 10 May 2010 00:12:44 GMT",
"version": "v1"
}
] |
2010-05-11
|
[
[
"O'Hara",
"Paul",
""
]
] |
In a previous article a relationship was established between the linearized metrics of General Relativity associated with geodesics and the Dirac Equation of quantum mechanics. In this paper the extension of that result to arbitrary curves is investigated. In the case of scalar fields, a relationship between mass and temperature is also worked out.
|
2204.05470
|
Yaoguang Zheng
|
Wen-Xiang Chen, Yao-Guang Zheng
|
Thermodynamic geometry analysis of new Schwarzschild black holes
| null | null | null | null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
This article puts forward a hypothesis.In this article, the derivative of the
cosmological constant is positive, and there is a possibility that the constant
evolves from negative in the early universe to positive in the later period. We
see that when the black hole is an extreme black hole $r_{+}=r_{-}$, the
curvature scalar vanishes to zero. In general, the curvature scalar is not
equal to zero. When $r_{+}=3 r_{-}$, the curvature scalar is equal to negative
infinity. According to Ruppeiner's theory, this time represents the phase
transition of the system. It is very interesting that the divergence point of
the curvature scalar happens to be the Davis transition point. We have found
the phase transition point of the new Schwarzschild black hole.
|
[
{
"created": "Tue, 12 Apr 2022 01:42:58 GMT",
"version": "v1"
},
{
"created": "Sat, 16 Apr 2022 01:41:24 GMT",
"version": "v2"
}
] |
2022-04-19
|
[
[
"Chen",
"Wen-Xiang",
""
],
[
"Zheng",
"Yao-Guang",
""
]
] |
This article puts forward a hypothesis.In this article, the derivative of the cosmological constant is positive, and there is a possibility that the constant evolves from negative in the early universe to positive in the later period. We see that when the black hole is an extreme black hole $r_{+}=r_{-}$, the curvature scalar vanishes to zero. In general, the curvature scalar is not equal to zero. When $r_{+}=3 r_{-}$, the curvature scalar is equal to negative infinity. According to Ruppeiner's theory, this time represents the phase transition of the system. It is very interesting that the divergence point of the curvature scalar happens to be the Davis transition point. We have found the phase transition point of the new Schwarzschild black hole.
|
gr-qc/9610010
|
Piotr Chrusciel
|
Piotr T. Chru\'sciel
|
Uniqueness of stationary, electro-vacuum black holes revisited
|
24 pages, latex with amsfonts
|
Helv.Phys.Acta 69 (1996) 529-552
| null | null |
gr-qc
| null |
In recent years there has been some progress in the understanding of the
global structure of stationary black hole space-times. In this paper we review
some new results concerning the structure of stationary black hole space-times.
In particular we prove a corrected version of the ``black hole rigidity
theorem'', and we prove a uniqueness theorem for static black holes with
degenerate connected horizons. This paper is an expanded version of a lecture
given at the Journ\'ees relativistes in Ascona, May 1996.
|
[
{
"created": "Wed, 9 Oct 1996 10:50:23 GMT",
"version": "v1"
}
] |
2007-05-23
|
[
[
"Chruściel",
"Piotr T.",
""
]
] |
In recent years there has been some progress in the understanding of the global structure of stationary black hole space-times. In this paper we review some new results concerning the structure of stationary black hole space-times. In particular we prove a corrected version of the ``black hole rigidity theorem'', and we prove a uniqueness theorem for static black holes with degenerate connected horizons. This paper is an expanded version of a lecture given at the Journ\'ees relativistes in Ascona, May 1996.
|
1511.03324
|
Philippe G. LeFloch
|
Philippe G. LeFloch and Yue Ma
|
The global nonlinear stability of Minkowski space for self-gravitating
massive fields
|
165 pages
| null | null | null |
gr-qc math.AP
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The theory presented in this monograph establishes the first mathematically
rigorous result on the global nonlinear stability of self-gravitating matter
under small perturbations of an asymptotically flat, spacelike hypersurface of
Minkowski spacetime. It allows one to exclude the existence of dynamically
unstable, self-gravitating massive fields and, therefore, solves a
long-standing open problem in General Relativity. By a significant extension of
the Hyperboloidal Foliation Method they introduced in 2014, the authors
establish global-in-time existence for the Einstein equations expressed as a
coupled wave-Klein-Gordon system of partial differential equations. The metric
and matter fields are sought for in Sobolev-type functional spaces, suitably
defined from the translations and the boosts of Minkowski spacetime.
|
[
{
"created": "Tue, 10 Nov 2015 22:42:42 GMT",
"version": "v1"
},
{
"created": "Thu, 12 May 2016 01:49:36 GMT",
"version": "v2"
},
{
"created": "Thu, 29 Dec 2016 18:28:13 GMT",
"version": "v3"
},
{
"created": "Mon, 3 Jul 2017 16:23:13 GMT",
"version": "v4"
}
] |
2017-07-04
|
[
[
"LeFloch",
"Philippe G.",
""
],
[
"Ma",
"Yue",
""
]
] |
The theory presented in this monograph establishes the first mathematically rigorous result on the global nonlinear stability of self-gravitating matter under small perturbations of an asymptotically flat, spacelike hypersurface of Minkowski spacetime. It allows one to exclude the existence of dynamically unstable, self-gravitating massive fields and, therefore, solves a long-standing open problem in General Relativity. By a significant extension of the Hyperboloidal Foliation Method they introduced in 2014, the authors establish global-in-time existence for the Einstein equations expressed as a coupled wave-Klein-Gordon system of partial differential equations. The metric and matter fields are sought for in Sobolev-type functional spaces, suitably defined from the translations and the boosts of Minkowski spacetime.
|
gr-qc/9506045
|
Manuela Campanelli
|
Manuela Campanelli
|
Comment on ``Perturbative Method to solve fourth-order Gravity Field
Equations"
|
6 pages, Revtex
| null | null |
UAB-FT-371
|
gr-qc astro-ph hep-th
| null |
We reconsider the cosmic string perturbative solution to the classical
fourth-order gravity field equations, obtained in Ref.\cite{CLA94}, and we
obtain that static, cylindricaly symmetric gauge cosmic strings, with constant
energy density, can contain only $\beta$-terms in the first order corrections
to the interior gravitational field, while the exact exterior solution is a
conical spacetime with deficit angle $D=8\pi\mu$.
|
[
{
"created": "Thu, 22 Jun 1995 11:14:06 GMT",
"version": "v1"
}
] |
2007-05-23
|
[
[
"Campanelli",
"Manuela",
""
]
] |
We reconsider the cosmic string perturbative solution to the classical fourth-order gravity field equations, obtained in Ref.\cite{CLA94}, and we obtain that static, cylindricaly symmetric gauge cosmic strings, with constant energy density, can contain only $\beta$-terms in the first order corrections to the interior gravitational field, while the exact exterior solution is a conical spacetime with deficit angle $D=8\pi\mu$.
|
2312.16081
|
Mohsen Khodadi
|
Seyed Naseh Sajadi, Mohsen Khodadi, Orlando Luongo, Hernando Quevedo
|
Anisotropic Generalized Polytropic Spheres: Regular 3D Black Holes
|
17 pages, 9 figures, 1 table, 2 appendix, v2: discussion improved and
extended, figures added, references updated, version accepted for publication
|
Phys.Dark Univ. 45 (2024) 101525
|
10.1016/j.dark.2024.101525
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We model gravitating relativistic 3D spheres composed of an anisotropic fluid
in which the radial and transverse components of the pressure correspond to the
vacuum energy and a generalized polytropic equation-of-state, respectively. By
using the generalized Tolman-Oppenheimer-Volkoff (TOV) equation, and solving
the complete system of equations for these anisotropic generalized polytropic
spheres, for a given range of model parameters, we find three novel classes of
asymptotically AdS black hole solutions with regular core. We show the
regularity of the solutions using curvature scalars and the formalism of
geodesic completeness. Then, using the eigenvalues of the Riemann curvature
tensor, we consider the effects of repulsive gravity in the three static 3D
regular black holes, concluding that their regular behavior can be explained as
due to the presence of repulsive gravity near the center of the objects.
Finally, we study the stability of the regular black holes under the flow of
the energy through the Cauchy horizon.
|
[
{
"created": "Tue, 26 Dec 2023 15:09:35 GMT",
"version": "v1"
},
{
"created": "Tue, 7 May 2024 18:05:56 GMT",
"version": "v2"
}
] |
2024-05-20
|
[
[
"Sajadi",
"Seyed Naseh",
""
],
[
"Khodadi",
"Mohsen",
""
],
[
"Luongo",
"Orlando",
""
],
[
"Quevedo",
"Hernando",
""
]
] |
We model gravitating relativistic 3D spheres composed of an anisotropic fluid in which the radial and transverse components of the pressure correspond to the vacuum energy and a generalized polytropic equation-of-state, respectively. By using the generalized Tolman-Oppenheimer-Volkoff (TOV) equation, and solving the complete system of equations for these anisotropic generalized polytropic spheres, for a given range of model parameters, we find three novel classes of asymptotically AdS black hole solutions with regular core. We show the regularity of the solutions using curvature scalars and the formalism of geodesic completeness. Then, using the eigenvalues of the Riemann curvature tensor, we consider the effects of repulsive gravity in the three static 3D regular black holes, concluding that their regular behavior can be explained as due to the presence of repulsive gravity near the center of the objects. Finally, we study the stability of the regular black holes under the flow of the energy through the Cauchy horizon.
|
1504.00453
|
Mohammad Vahid Takook
|
S. Parsamehr, M. Enayati and M.V. Takook
|
Super-gauge Field in de Sitter Universe
|
21 pages
|
Eur. Phys. J. C (2016) 76: 260
|
10.1140/epjc/s10052-016-4027-7
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The Gupta-Bleuler triplet for vector-spinor gauge field is presented in de
Sitter ambient space formalism. The invariant space of field equation solutions
is obtained with respect to an indecomposable representation of the de Sitter
group. By using the general solution of the massless spin-$\frac{3}{2}$ field
equation, the vector-spinor quantum field operator and its corresponding Fock
space is constructed. The quantum field operator can be written in terms of the
vector-spinor polarization states and a quantum conformally coupled massless
scalar field, which is constructed on Bunch-Davies vacuum state. The two-point
function is also presented, which is de Sitter covariant and analytic.
|
[
{
"created": "Thu, 2 Apr 2015 06:45:13 GMT",
"version": "v1"
},
{
"created": "Wed, 20 Jul 2016 06:18:09 GMT",
"version": "v2"
}
] |
2016-07-22
|
[
[
"Parsamehr",
"S.",
""
],
[
"Enayati",
"M.",
""
],
[
"Takook",
"M. V.",
""
]
] |
The Gupta-Bleuler triplet for vector-spinor gauge field is presented in de Sitter ambient space formalism. The invariant space of field equation solutions is obtained with respect to an indecomposable representation of the de Sitter group. By using the general solution of the massless spin-$\frac{3}{2}$ field equation, the vector-spinor quantum field operator and its corresponding Fock space is constructed. The quantum field operator can be written in terms of the vector-spinor polarization states and a quantum conformally coupled massless scalar field, which is constructed on Bunch-Davies vacuum state. The two-point function is also presented, which is de Sitter covariant and analytic.
|
1309.6221
|
Berit Behnke
|
The LIGO Scientific Collaboration and The Virgo Collaboration: J.
Aasi, J. Abadie, B. P. Abbott, R. Abbott, T. Abbott, M. R. Abernathy, T.
Accadia, F. Acernese, C. Adams, T. Adams, R. X. Adhikari, C. Affeldt, M.
Agathos, N. Aggarwal, O. D. Aguiar, P. Ajith, B. Allen, A. Allocca, E. Amador
Ceron, D. Amariutei, R. A. Anderson, S. B. Anderson, W. G. Anderson, K. Arai,
M. C. Araya, C. Arceneaux, J. Areeda, S. Ast, S. M. Aston, P. Astone, P.
Aufmuth, C. Aulbert, L. Austin, B. E. Aylott, S. Babak, P. T. Baker, G.
Ballardin, S. W. Ballmer, J. C. Barayoga, D. Barker, S. H. Barnum, F. Barone,
B. Barr, L. Barsotti, M. Barsuglia, M. A. Barton, I. Bartos, R. Bassiri, A.
Basti, J. Batch, J. Bauchrowitz, Th. S. Bauer, M. Bebronne, B. Behnke, M.
Bejger, M.G. Beker, A. S. Bell, C. Bell, I. Belopolski, G. Bergmann, J. M.
Berliner, A. Bertolini, D. Bessis, J. Betzwieser, P. T. Beyersdorf, T.
Bhadbhade, I. A. Bilenko, G. Billingsley, J. Birch, M. Bitossi, M. A.
Bizouard, E. Black, J. K. Blackburn, L. Blackburn, D. Blair, M. Blom, O.
Bock, T. P. Bodiya, M. Boer, C. Bogan, C. Bond, F. Bondu, L. Bonelli, R.
Bonnand, R. Bork, M. Born, S. Bose, L. Bosi, J. Bowers, C. Bradaschia, P. R.
Brady, V. B. Braginsky, M. Branchesi, C. A. Brannen, J. E. Brau, J. Breyer,
T. Briant, D. O. Bridges, A. Brillet, M. Brinkmann, V. Brisson, M. Britzger,
A. F. Brooks, D. A. Brown, D. D. Brown, F. Br\"uckner, T. Bulik, H. J.
Bulten, A. Buonanno, D. Buskulic, C. Buy, R. L. Byer, L. Cadonati, G.
Cagnoli, J. Calder\'on Bustillo, E. Calloni, J. B. Camp, P. Campsie, K. C.
Cannon, B. Canuel, J. Cao, C. D. Capano, F. Carbognani, L. Carbone, S.
Caride, A. Castiglia, S. Caudill, M. Cavagli\'a, F. Cavalier, R. Cavalieri,
G. Cella, C. Cepeda, E. Cesarini, R. Chakraborty, T. Chalermsongsak, S. Chao,
P. Charlton, E. Chassande-Mottin, X. Chen, Y. Chen, A. Chincarini, A.
Chiummo, H. S. Cho, J. Chow, N. Christensen, Q. Chu, S. S. Y. Chua, S. Chung,
G. Ciani, F. Clara, D. E. Clark, J. A. Clark, F. Cleva, E. Coccia, P.-F.
Cohadon, A. Colla, M. Colombini, M. Constancio Jr, A. Conte, R. Conte, D.
Cook, T. R. Corbitt, M. Cordier, N. Cornish, A. Corsi, C. A. Costa, M. W.
Coughlin, J.-P. Coulon, S. Countryman, P. Couvares, D. M. Coward, M. Cowart,
D. C. Coyne, K. Craig, J. D. E. Creighton, T. D. Creighton, S. G. Crowder, A.
Cumming, L. Cunningham, E. Cuoco, K. Dahl, T. Dal Canton, M. Damjanic, S. L.
Danilishin, S. D'Antonio, K. Danzmann, V. Dattilo, B. Daudert, H. Daveloza,
M. Davier, G. S. Davies, E. J. Daw, R. Day, T. Dayanga, R. De Rosa, G.
Debreczeni, J. Degallaix, W. Del Pozzo, E. Deleeuw, S. Del\'eglise, T.
Denker, T. Dent, H. Dereli, V. Dergachev, R. DeRosa, R. DeSalvo, S.
Dhurandhar, L. Di Fiore, A. Di Lieto, I. Di Palma, A. Di Virgilio, M. D\'iaz,
A. Dietz, K. Dmitry, F. Donovan, K. L. Dooley, S. Doravari, M. Drago, R. W.
P. Drever, J. C. Driggers, Z. Du, J. -C. Dumas, S. Dwyer, T. Eberle, M.
Edwards, A. Effler, P. Ehrens, J. Eichholz, S. S. Eikenberry, G. Endr\"oczi,
R. Essick, T. Etzel, K. Evans, M. Evans, T. Evans, M. Factourovich, V.
Fafone, S. Fairhurst, Q. Fang, B. Farr, W. Farr, M. Favata, D. Fazi, H.
Fehrmann, D. Feldbaum, I. Ferrante, F. Ferrini, F. Fidecaro, L. S. Finn, I.
Fiori, R. Fisher, R. Flaminio, E. Foley, S. Foley, E. Forsi, L. A. Forte, N.
Fotopoulos, J.-D. Fournier, S. Franco, S. Frasca, F. Frasconi, M. Frede, M.
Frei, Z. Frei, A. Freise, R. Frey, T. T. Fricke, P. Fritschel, V. V. Frolov,
M.-K. Fujimoto, P. Fulda, M. Fyffe, J. Gair, L. Gammaitoni, J. Garcia, F.
Garufi, N. Gehrels, G. Gemme, E. Genin, A. Gennai, L. Gergely, S. Ghosh, J.
A. Giaime, S. Giampanis, K. D. Giardina, A. Giazotto, S. Gil-Casanova, C.
Gill, J. Gleason, E. Goetz, R. Goetz, L. Gondan, G. Gonz\'alez, N. Gordon, M.
L. Gorodetsky, S. Gossan, S. Go{\ss}ler, R. Gouaty, C. Graef, P. B. Graff, M.
Granata, A. Grant, S. Gras, C. Gray, R. J. S. Greenhalgh, A. M. Gretarsson,
C. Griffo, H. Grote, K. Grover, S. Grunewald, G. M. Guidi, C. Guido, K. E.
Gushwa, E. K. Gustafson, R. Gustafson, B. Hall, E. Hall, D. Hammer, G.
Hammond, M. Hanke, J. Hanks, C. Hanna, J. Hanson, J. Harms, G. M. Harry, I.
W. Harry, E. D. Harstad, M. T. Hartman, K. Haughian, K. Hayama, J. Heefner,
A. Heidmann, M. Heintze, H. Heitmann, P. Hello, G. Hemming, M. Hendry, I. S.
Heng, A. W. Heptonstall, M. Heurs, S. Hild, D. Hoak, K. A. Hodge, K. Holt, M.
Holtrop, T. Hong, S. Hooper, T. Horrom, D. J. Hosken, J. Hough, E. J. Howell,
Y. Hu, Z. Hua, V. Huang, E. A. Huerta, B. Hughey, S. Husa, S. H. Huttner, M.
Huynh, T. Huynh-Dinh, J. Iafrate, D. R. Ingram, R. Inta, T. Isogai, A.
Ivanov, B. R. Iyer, K. Izumi, M. Jacobson, E. James, H. Jang, Y. J. Jang, P.
Jaranowski, F. Jim\'enez-Forteza, W. W. Johnson, D. Jones, D. I. Jones, R.
Jones, R.J.G. Jonker, L. Ju, Haris K, P. Kalmus, V. Kalogera, S. Kandhasamy,
G. Kang, J. B. Kanner, M. Kasprzack, R. Kasturi, E. Katsavounidis, W.
Katzman, H. Kaufer, K. Kaufman, K. Kawabe, S. Kawamura, F. Kawazoe, F.
K\'ef\'elian, D. Keitel, D. B. Kelley, W. Kells, D. G. Keppel, A.
Khalaidovski, F. Y. Khalili, E. A. Khazanov, B. K. Kim, C. Kim, K. Kim, N.
Kim, W. Kim, Y.-M. Kim, E. J. King, P. J. King, D. L. Kinzel, J. S. Kissel,
S. Klimenko, J. Kline, S. Koehlenbeck, K. Kokeyama, V. Kondrashov, S.
Koranda, W. Z. Korth, I. Kowalska, D. Kozak, A. Kremin, V. Kringel, B.
Krishnan, A. Kr\'olak, C. Kucharczyk, S. Kudla, G. Kuehn, A. Kumar, P. Kumar,
R. Kumar, R. Kurdyumov, P. Kwee, M. Landry, B. Lantz, S. Larson, P. D. Lasky,
C. Lawrie, A. Lazzarini, A. Le Roux, P. Leaci, E. O. Lebigot, C.-H. Lee, H.
K. Lee, H. M. Lee, J. Lee, J. Lee, M. Leonardi, J. R. Leong, N. Leroy, N.
Letendre, B. Levine, J. B. Lewis, V. Lhuillier, T. G. F. Li, A. C. Lin, T. B.
Littenberg, V. Litvine, F. Liu, H. Liu, Y. Liu, Z. Liu, D. Lloyd, N. A.
Lockerbie, V. Lockett, D. Lodhia, K. Loew, J. Logue, A. L. Lombardi, M.
Lorenzini, V. Loriette, M. Lormand, G. Losurdo, J. Lough, J. Luan, M. J.
Lubinski, H. L\"uck, A. P. Lundgren, J. Macarthur, E. Macdonald, B.
Machenschalk, M. MacInnis, D. M. Macleod, F. Magana-Sandoval, M. Mageswaran,
K. Mailand, E. Majorana, I. Maksimovic, V. Malvezzi, N. Man, G. M. Manca, I.
Mandel, V. Mandic, V. Mangano, M. Mantovani, F. Marchesoni, F. Marion, S.
M\'arka, Z. M\'arka, A. Markosyan, E. Maros, J. Marque, F. Martelli, I. W.
Martin, R. M. Martin, L. Martinelli, D. Martynov, J. N. Marx, K. Mason, A.
Masserot, T. J. Massinger, F. Matichard, L. Matone, R. A. Matzner, N.
Mavalvala, G. May, N. Mazumder, G. Mazzolo, R. McCarthy, D. E. McClelland, S.
C. McGuire, G. McIntyre, J. McIver, D. Meacher, G. D. Meadors, M. Mehmet, J.
Meidam, T. Meier, A. Melatos, G. Mendell, R. A. Mercer, S. Meshkov, C.
Messenger, M. S. Meyer, H. Miao, C. Michel, E. E. Mikhailov, L. Milano, J.
Miller, Y. Minenkov, C. M. F. Mingarelli, S. Mitra, V. P. Mitrofanov, G.
Mitselmakher, R. Mittleman, B. Moe, M. Mohan, S. R. P. Mohapatra, F. Mokler,
D. Moraru, G. Moreno, N. Morgado, T. Mori, S. R. Morriss, K. Mossavi, B.
Mours, C. M. Mow-Lowry, C. L. Mueller, G. Mueller, S. Mukherjee, A. Mullavey,
J. Munch, D. Murphy, P. G. Murray, A. Mytidis, M. F. Nagy, D. Nanda Kumar, I.
Nardecchia, T. Nash, L. Naticchioni, R. Nayak, V. Necula, I. Neri, G. Newton,
T. Nguyen, E. Nishida, A. Nishizawa, A. Nitz, F. Nocera, D. Nolting, M. E.
Normandin, L. K. Nuttall, E. Ochsner, J. O'Dell, E. Oelker, G. H. Ogin, J. J.
Oh, S. H. Oh, F. Ohme, P. Oppermann, B. O'Reilly, W. Ortega Larcher, R.
O'Shaughnessy, C. Osthelder, D. J. Ottaway, R. S. Ottens, J. Ou, H. Overmier,
B. J. Owen, C. Padilla, A. Pai, C. Palomba, Y. Pan, C. Pankow, F. Paoletti,
R. Paoletti, M. A. Papa, H. Paris, A. Pasqualetti, R. Passaquieti, D.
Passuello, M. Pedraza, P. Peiris, S. Penn, A. Perreca, M. Phelps, M. Pichot,
M. Pickenpack, F. Piergiovanni, V. Pierro, L. Pinard, B. Pindor, I. M. Pinto,
M. Pitkin, H. J. Pletsch, J. Poeld, R. Poggiani, V. Poole, C. Poux, V.
Predoi, T. Prestegard, L. R. Price, M. Prijatelj, M. Principe, S. Privitera,
R. Prix, G. A. Prodi, L. Prokhorov, O. Puncken, M. Punturo, P. Puppo, V.
Quetschke, E. Quintero, R. Quitzow-James, F. J. Raab, D. S. Rabeling, I.
R\'acz, H. Radkins, P. Raffai, S. Raja, G. Rajalakshmi, M. Rakhmanov, C.
Ramet, P. Rapagnani, V. Raymond, V. Re, C. M. Reed, T. Reed, T. Regimbau, S.
Reid, D. H. Reitze, F. Ricci, R. Riesen, K. Riles, N. A. Robertson, F.
Robinet, A. Rocchi, S. Roddy, C. Rodriguez, M. Rodruck, C. Roever, L.
Rolland, J. G. Rollins, J. D. Romano, R. Romano, G. Romanov, J. H. Romie, D.
Rosi\'nska, S. Rowan, A. R\"udiger, P. Ruggi, K. Ryan, F. Salemi, L. Sammut,
V. Sandberg, J. Sanders, V. Sannibale, I. Santiago-Prieto, E. Saracco, B.
Sassolas, B. S. Sathyaprakash, P. R. Saulson, R. Savage, R. Schilling, R.
Schnabel, R. M. S. Schofield, E. Schreiber, D. Schuette, B. Schulz, B. F.
Schutz, P. Schwinberg, J. Scott, S. M. Scott, F. Seifert, D. Sellers, A. S.
Sengupta, D. Sentenac, A. Sergeev, D. Shaddock, S. Shah, M. S. Shahriar, M.
Shaltev, B. Shapiro, P. Shawhan, D. H. Shoemaker, T. L. Sidery, K. Siellez,
X. Siemens, D. Sigg, D. Simakov, A. Singer, L. Singer, A. M. Sintes, G. R.
Skelton, B. J. J. Slagmolen, J. Slutsky, J. R. Smith, M. R. Smith, R. J. E.
Smith, N. D. Smith-Lefebvre, K. Soden, E. J. Son, B. Sorazu, T. Souradeep, L.
Sperandio, A. Staley, E. Steinert, J. Steinlechner, S. Steinlechner, S.
Steplewski, D. Stevens, A. Stochino, R. Stone, K. A. Strain, S. Strigin, A.
S. Stroeer, R. Sturani, A. L. Stuver, T. Z. Summerscales, S. Susmithan, P. J.
Sutton, B. Swinkels, G. Szeifert, M. Tacca, D. Talukder, L. Tang, D. B.
Tanner, S. P. Tarabrin, R. Taylor, A. P. M. ter Braack, M. P.
Thirugnanasambandam, M. Thomas, P. Thomas, K. A. Thorne, K. S. Thorne, E.
Thrane, V. Tiwari, K. V. Tokmakov, C. Tomlinson, A. Toncelli, M. Tonelli, O.
Torre, C. V. Torres, C. I. Torrie, F. Travasso, G. Traylor, M. Tse, D.
Ugolini, C. S. Unnikrishnan, H. Vahlbruch, G. Vajente, M. Vallisneri, J. F.
J. van den Brand, C. Van Den Broeck, S. van der Putten, M. V. van der Sluys,
J. van Heijningen, A. A. van Veggel, S. Vass, M. Vas\'uth, R. Vaulin, A.
Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, K. Venkateswara, D. Verkindt,
S. Verma, F. Vetrano, A. Vicer\'e, R. Vincent-Finley, J.-Y. Vinet, S. Vitale,
B. Vlcek, T. Vo, H. Vocca, C. Vorvick, W. D. Vousden, D. Vrinceanu, S. P.
Vyachanin, A. Wade, L. Wade, M. Wade, S. J. Waldman, M. Walker, L. Wallace,
Y. Wan, J. Wang, M. Wang, X. Wang, A. Wanner, R. L. Ward, M. Was, B. Weaver,
L.-W. Wei, M. Weinert, A. J. Weinstein, R. Weiss, T. Welborn, L. Wen, P.
Wessels, M. West, T. Westphal, K. Wette, J. T. Whelan, S. E. Whitcomb, D. J.
White, B. F. Whiting, S. Wibowo, K. Wiesner, C. Wilkinson, L. Williams, R.
Williams, T. Williams, J. L. Willis, B. Willke, M. Wimmer, L. Winkelmann, W.
Winkler, C. C. Wipf, H. Wittel, G. Woan, J. Worden, J. Yablon, I. Yakushin,
H. Yamamoto, C. C. Yancey, H. Yang, D. Yeaton-Massey, S. Yoshida, H. Yum, M.
Yvert, A. Zadrony, M. Zanolin, J.-P. Zendri, F. Zhang, L. Zhang, C. Zhao, H.
Zhu, X. J. Zhu, N. Zotov, M. E. Zucker, and J. Zweizig
|
A directed search for continuous Gravitational Waves from the Galactic
Center
|
12 pages, 3 figures, 1 table; PDFLaTeX; to be published in
Phys.Rev.D; a science summary can be found at
http://www.ligo.org/science/Publication-GCSearch/index.php
|
Phys. Rev. D 88, 102002 (2013)
|
10.1103/PhysRevD.88.102002
|
LIGO-P1300037
|
gr-qc astro-ph.HE
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We present the results of a directed search for continuous gravitational
waves from unknown, isolated neutron stars in the Galactic Center region,
performed on two years of data from LIGO's fifth science run from two LIGO
detectors. The search uses a semi-coherent approach, analyzing coherently 630
segments, each spanning 11.5 hours, and then incoherently combining the results
of the single segments. It covers gravitational wave frequencies in a range
from 78 to 496 Hz and a frequency-dependent range of first order spindown
values down to -7.86 x 10^-8 Hz/s at the highest frequency. No gravitational
waves were detected. We place 90% confidence upper limits on the gravitational
wave amplitude of sources at the Galactic Center. Placing 90% confidence upper
limits on the gravitational wave amplitude of sources at the Galactic Center,
we reach ~3.35x10^-25 for frequencies near 150 Hz. These upper limits are the
most constraining to date for a large-parameter-space search for continuous
gravitational wave signals.
|
[
{
"created": "Tue, 24 Sep 2013 15:41:41 GMT",
"version": "v1"
},
{
"created": "Fri, 27 Sep 2013 09:54:20 GMT",
"version": "v2"
}
] |
2013-11-27
|
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"M.",
""
],
[
"Talukder",
"D.",
""
],
[
"Tang",
"L.",
""
],
[
"Tanner",
"D. B.",
""
],
[
"Tarabrin",
"S. P.",
""
],
[
"Taylor",
"R.",
""
],
[
"ter Braack",
"A. P. M.",
""
],
[
"Thirugnanasambandam",
"M. P.",
""
],
[
"Thomas",
"M.",
""
],
[
"Thomas",
"P.",
""
],
[
"Thorne",
"K. A.",
""
],
[
"Thorne",
"K. S.",
""
],
[
"Thrane",
"E.",
""
],
[
"Tiwari",
"V.",
""
],
[
"Tokmakov",
"K. V.",
""
],
[
"Tomlinson",
"C.",
""
],
[
"Toncelli",
"A.",
""
],
[
"Tonelli",
"M.",
""
],
[
"Torre",
"O.",
""
],
[
"Torres",
"C. V.",
""
],
[
"Torrie",
"C. I.",
""
],
[
"Travasso",
"F.",
""
],
[
"Traylor",
"G.",
""
],
[
"Tse",
"M.",
""
],
[
"Ugolini",
"D.",
""
],
[
"Unnikrishnan",
"C. S.",
""
],
[
"Vahlbruch",
"H.",
""
],
[
"Vajente",
"G.",
""
],
[
"Vallisneri",
"M.",
""
],
[
"Brand",
"J. F. J. van den",
""
],
[
"Broeck",
"C. Van Den",
""
],
[
"van der Putten",
"S.",
""
],
[
"van der Sluys",
"M. V.",
""
],
[
"van Heijningen",
"J.",
""
],
[
"van Veggel",
"A. A.",
""
],
[
"Vass",
"S.",
""
],
[
"Vasúth",
"M.",
""
],
[
"Vaulin",
"R.",
""
],
[
"Vecchio",
"A.",
""
],
[
"Vedovato",
"G.",
""
],
[
"Veitch",
"J.",
""
],
[
"Veitch",
"P. J.",
""
],
[
"Venkateswara",
"K.",
""
],
[
"Verkindt",
"D.",
""
],
[
"Verma",
"S.",
""
],
[
"Vetrano",
"F.",
""
],
[
"Viceré",
"A.",
""
],
[
"Vincent-Finley",
"R.",
""
],
[
"Vinet",
"J. -Y.",
""
],
[
"Vitale",
"S.",
""
],
[
"Vlcek",
"B.",
""
],
[
"Vo",
"T.",
""
],
[
"Vocca",
"H.",
""
],
[
"Vorvick",
"C.",
""
],
[
"Vousden",
"W. D.",
""
],
[
"Vrinceanu",
"D.",
""
],
[
"Vyachanin",
"S. P.",
""
],
[
"Wade",
"A.",
""
],
[
"Wade",
"L.",
""
],
[
"Wade",
"M.",
""
],
[
"Waldman",
"S. J.",
""
],
[
"Walker",
"M.",
""
],
[
"Wallace",
"L.",
""
],
[
"Wan",
"Y.",
""
],
[
"Wang",
"J.",
""
],
[
"Wang",
"M.",
""
],
[
"Wang",
"X.",
""
],
[
"Wanner",
"A.",
""
],
[
"Ward",
"R. L.",
""
],
[
"Was",
"M.",
""
],
[
"Weaver",
"B.",
""
],
[
"Wei",
"L. -W.",
""
],
[
"Weinert",
"M.",
""
],
[
"Weinstein",
"A. J.",
""
],
[
"Weiss",
"R.",
""
],
[
"Welborn",
"T.",
""
],
[
"Wen",
"L.",
""
],
[
"Wessels",
"P.",
""
],
[
"West",
"M.",
""
],
[
"Westphal",
"T.",
""
],
[
"Wette",
"K.",
""
],
[
"Whelan",
"J. T.",
""
],
[
"Whitcomb",
"S. E.",
""
],
[
"White",
"D. J.",
""
],
[
"Whiting",
"B. F.",
""
],
[
"Wibowo",
"S.",
""
],
[
"Wiesner",
"K.",
""
],
[
"Wilkinson",
"C.",
""
],
[
"Williams",
"L.",
""
],
[
"Williams",
"R.",
""
],
[
"Williams",
"T.",
""
],
[
"Willis",
"J. L.",
""
],
[
"Willke",
"B.",
""
],
[
"Wimmer",
"M.",
""
],
[
"Winkelmann",
"L.",
""
],
[
"Winkler",
"W.",
""
],
[
"Wipf",
"C. C.",
""
],
[
"Wittel",
"H.",
""
],
[
"Woan",
"G.",
""
],
[
"Worden",
"J.",
""
],
[
"Yablon",
"J.",
""
],
[
"Yakushin",
"I.",
""
],
[
"Yamamoto",
"H.",
""
],
[
"Yancey",
"C. C.",
""
],
[
"Yang",
"H.",
""
],
[
"Yeaton-Massey",
"D.",
""
],
[
"Yoshida",
"S.",
""
],
[
"Yum",
"H.",
""
],
[
"Yvert",
"M.",
""
],
[
"Zadrony",
"A.",
""
],
[
"Zanolin",
"M.",
""
],
[
"Zendri",
"J. -P.",
""
],
[
"Zhang",
"F.",
""
],
[
"Zhang",
"L.",
""
],
[
"Zhao",
"C.",
""
],
[
"Zhu",
"H.",
""
],
[
"Zhu",
"X. J.",
""
],
[
"Zotov",
"N.",
""
],
[
"Zucker",
"M. E.",
""
],
[
"Zweizig",
"J.",
""
]
] |
We present the results of a directed search for continuous gravitational waves from unknown, isolated neutron stars in the Galactic Center region, performed on two years of data from LIGO's fifth science run from two LIGO detectors. The search uses a semi-coherent approach, analyzing coherently 630 segments, each spanning 11.5 hours, and then incoherently combining the results of the single segments. It covers gravitational wave frequencies in a range from 78 to 496 Hz and a frequency-dependent range of first order spindown values down to -7.86 x 10^-8 Hz/s at the highest frequency. No gravitational waves were detected. We place 90% confidence upper limits on the gravitational wave amplitude of sources at the Galactic Center. Placing 90% confidence upper limits on the gravitational wave amplitude of sources at the Galactic Center, we reach ~3.35x10^-25 for frequencies near 150 Hz. These upper limits are the most constraining to date for a large-parameter-space search for continuous gravitational wave signals.
|
gr-qc/0309111
|
Gilberto Medeiros Kremer
|
G. M. Kremer
|
Cosmological models described by a mixture of van der Waals fluid and
dark energy
|
5 pages, 5 figures. To be published in Physical Review D
|
Phys.Rev. D68 (2003) 123507
|
10.1103/PhysRevD.68.123507
| null |
gr-qc
| null |
The Universe is modeled as a binary mixture whose constituents are described
by a van der Waals fluid and by a dark energy density. The dark energy density
is considered either as the quintessence or as the Chaplygin gas. The
irreversible processes concerning the energy transfer between the van der Waals
fluid and the gravitational field are taken into account. This model can
simulate: (a) an inflationary period where the acceleration grows exponentially
and the van der Waals fluid behaves like an inflaton; (b) an inflationary
period where the acceleration is positive but it decreases and tends to zero
whereas the energy density of the van der Waals fluid decays; (c) a decelerated
period which corresponds to a matter dominated period with a non-negative
pressure; and (d) a present accelerated period where the dark energy density
outweighs the energy density of the van der Waals fluid.
|
[
{
"created": "Tue, 23 Sep 2003 11:39:10 GMT",
"version": "v1"
}
] |
2009-11-10
|
[
[
"Kremer",
"G. M.",
""
]
] |
The Universe is modeled as a binary mixture whose constituents are described by a van der Waals fluid and by a dark energy density. The dark energy density is considered either as the quintessence or as the Chaplygin gas. The irreversible processes concerning the energy transfer between the van der Waals fluid and the gravitational field are taken into account. This model can simulate: (a) an inflationary period where the acceleration grows exponentially and the van der Waals fluid behaves like an inflaton; (b) an inflationary period where the acceleration is positive but it decreases and tends to zero whereas the energy density of the van der Waals fluid decays; (c) a decelerated period which corresponds to a matter dominated period with a non-negative pressure; and (d) a present accelerated period where the dark energy density outweighs the energy density of the van der Waals fluid.
|
2112.12519
|
Erick Tuiran
|
O. Ruiz and E. Tuiran
|
Non-Perturbative Quantum Correction to the Reissner-Nordstr\"om
spacetime with Running Newton's Constant
|
45 pages, 6 figures
|
Phys. Rev. D 107, 066003 (2023)
| null | null |
gr-qc hep-th
|
http://creativecommons.org/licenses/by/4.0/
|
We study the consequences of the running Newton's constant on several key
aspects of spherically symmetric charged black holes by performing a
renormalization group improvement of the classical Reissner-Nordstr\"om metric
within the framework of the Einstein-Hilbert truncation in quantum Einstein
gravity. In particular, we determine that the event horizon surfaces are stable
except for the extremal case and we corroborate the appearance of a new
extremality condition at the Planck scale that hints at the existence of a
final stage after the black hole evaporation process. We find explicit
expressions for the area and surface gravity of the event horizon and we show
the existence of an exact form $dS$ with the surface gravity as integrating
factor. This result is a first clue towards finding a generalization of the
first law of black hole dynamics, for improved charged spherically symmetric
spacetimes in contrast to a previous no-go result for axially symmetric ones
with null charge. We finally calculate an explicit formula for the Komar mass
at the event horizon, and we compare it with the total mass at infinity for a
wide domain of values of the black hole parameters M, Q and $\bar{w}$, showing
a loss of mass which can be interpreted as a consequence of the antiscreening
effect of the gravitational field between the event horizon and infinity.
|
[
{
"created": "Thu, 23 Dec 2021 13:20:18 GMT",
"version": "v1"
}
] |
2023-03-09
|
[
[
"Ruiz",
"O.",
""
],
[
"Tuiran",
"E.",
""
]
] |
We study the consequences of the running Newton's constant on several key aspects of spherically symmetric charged black holes by performing a renormalization group improvement of the classical Reissner-Nordstr\"om metric within the framework of the Einstein-Hilbert truncation in quantum Einstein gravity. In particular, we determine that the event horizon surfaces are stable except for the extremal case and we corroborate the appearance of a new extremality condition at the Planck scale that hints at the existence of a final stage after the black hole evaporation process. We find explicit expressions for the area and surface gravity of the event horizon and we show the existence of an exact form $dS$ with the surface gravity as integrating factor. This result is a first clue towards finding a generalization of the first law of black hole dynamics, for improved charged spherically symmetric spacetimes in contrast to a previous no-go result for axially symmetric ones with null charge. We finally calculate an explicit formula for the Komar mass at the event horizon, and we compare it with the total mass at infinity for a wide domain of values of the black hole parameters M, Q and $\bar{w}$, showing a loss of mass which can be interpreted as a consequence of the antiscreening effect of the gravitational field between the event horizon and infinity.
|
2211.12349
|
Arthur Menezes Lima
|
A. Lima, G. Alencar and J. Furtado
|
Black string bounce to traversable wormhole
|
8 pages, 6 figures
| null | null | null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this work, a regular black string solution will be presented from the
method used by Simpson-Visser to regularize the Schwarzschild solution. As in
the Simpson-Visser work, in this new black string solution, it is possible to
represent both a regular black hole and a wormhole just by changing the value
of a parameter "$a$" used in its metric. Tensors and curvature invariants were
analyzed to verify the regularity of the solution, as well as the energy
conditions of the system. It was found that the null energy condition will
always be violated for the entire space. The analysis of the thermodynamic
properties of the regular black string was also carried out, in which the
modifications generated about the original solution of the black string, were
evaluated, specifically, the Hawking temperature, entropy, its thermal
capacity, and the Helmholtz free energy. Finally, we investigate the possible
stable or unstable circular orbits for photons and massive particles. The
results were compared with those of the non-regular black string, seeking to
make a parallel with the Simpson-Visser work.
|
[
{
"created": "Tue, 22 Nov 2022 15:37:01 GMT",
"version": "v1"
}
] |
2022-11-23
|
[
[
"Lima",
"A.",
""
],
[
"Alencar",
"G.",
""
],
[
"Furtado",
"J.",
""
]
] |
In this work, a regular black string solution will be presented from the method used by Simpson-Visser to regularize the Schwarzschild solution. As in the Simpson-Visser work, in this new black string solution, it is possible to represent both a regular black hole and a wormhole just by changing the value of a parameter "$a$" used in its metric. Tensors and curvature invariants were analyzed to verify the regularity of the solution, as well as the energy conditions of the system. It was found that the null energy condition will always be violated for the entire space. The analysis of the thermodynamic properties of the regular black string was also carried out, in which the modifications generated about the original solution of the black string, were evaluated, specifically, the Hawking temperature, entropy, its thermal capacity, and the Helmholtz free energy. Finally, we investigate the possible stable or unstable circular orbits for photons and massive particles. The results were compared with those of the non-regular black string, seeking to make a parallel with the Simpson-Visser work.
|
gr-qc/9811068
|
Martin Goliath
|
Martin Goliath and George F. R. Ellis
|
Homogeneous cosmologies with cosmological constant
|
10 pages, 13 eps-figures. Submitted to Phys. Rev. D
|
Phys.Rev.D60:023502,1999
|
10.1103/PhysRevD.60.023502
|
mth.uct.ac.za-9811
|
gr-qc astro-ph
| null |
Spatially homogeneous cosmological models with a positive cosmological
constant are investigated, using dynamical systems methods. We focus on the
future evolution of these models. In particular, we address the question
whether there are models within this class that are de Sitter-like in the
future, but are tilted.
|
[
{
"created": "Thu, 19 Nov 1998 16:56:32 GMT",
"version": "v1"
},
{
"created": "Wed, 24 Feb 1999 11:23:48 GMT",
"version": "v2"
}
] |
2011-07-18
|
[
[
"Goliath",
"Martin",
""
],
[
"Ellis",
"George F. R.",
""
]
] |
Spatially homogeneous cosmological models with a positive cosmological constant are investigated, using dynamical systems methods. We focus on the future evolution of these models. In particular, we address the question whether there are models within this class that are de Sitter-like in the future, but are tilted.
|
2203.03174
|
Sizheng Ma
|
Sizheng Ma, Qingwen Wang, Nils Deppe, Fran\c{c}ois H\'ebert, Lawrence
E. Kidder, Jordan Moxon, William Throwe, Nils L. Vu, Mark A. Scheel, Yanbei
Chen
|
Gravitational-wave echoes from numerical-relativity waveforms via
space-time construction near merging compact objects
| null |
Phys. Rev. D 105, 104007 (2022)
|
10.1103/PhysRevD.105.104007
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We propose a new approach toward reconstructing the late-time near-horizon
geometry of merging binary black holes, and toward computing gravitational-wave
echoes from exotic compact objects. A binary black-hole merger spacetime can be
divided by a time-like hypersurface into a Black-Hole Perturbation (BHP)
region, in which the space-time geometry can be approximated by homogeneous
linear perturbations of the final Kerr black hole, and a nonlinear region. At
late times, the boundary between the two regions is an infalling shell. The BHP
region contains late-time gravitational-waves emitted toward the future
horizon, as well as those emitted toward future null infinity. In this region,
by imposing no-ingoing wave conditions at past null infinity, and matching
out-going waves at future null infinity with waveforms computed from numerical
relativity, we can obtain waves that travel toward the future horizon. In
particular, the Newman-Penrose $\psi_0$ associated with the in-going wave on
the horizon is related to tidal deformations measured by fiducial observers
floating above the horizon. We further determine the boundary of the BHP region
on the future horizon by imposing that $\psi_0$ inside the BHP region can be
faithfully represented by quasi-normal modes. Using a physically-motivated way
to impose boundary conditions near the horizon, and applying the so-called
Boltzmann reflectivity, we compute the quasi-normal modes of non-rotating ECOs,
as well as gravitational-wave echoes. We also investigate the detectability of
these echoes in current and future detectors, and prospects for parameter
estimation.
|
[
{
"created": "Mon, 7 Mar 2022 06:56:42 GMT",
"version": "v1"
},
{
"created": "Thu, 21 Apr 2022 18:35:35 GMT",
"version": "v2"
}
] |
2022-05-06
|
[
[
"Ma",
"Sizheng",
""
],
[
"Wang",
"Qingwen",
""
],
[
"Deppe",
"Nils",
""
],
[
"Hébert",
"François",
""
],
[
"Kidder",
"Lawrence E.",
""
],
[
"Moxon",
"Jordan",
""
],
[
"Throwe",
"William",
""
],
[
"Vu",
"Nils L.",
""
],
[
"Scheel",
"Mark A.",
""
],
[
"Chen",
"Yanbei",
""
]
] |
We propose a new approach toward reconstructing the late-time near-horizon geometry of merging binary black holes, and toward computing gravitational-wave echoes from exotic compact objects. A binary black-hole merger spacetime can be divided by a time-like hypersurface into a Black-Hole Perturbation (BHP) region, in which the space-time geometry can be approximated by homogeneous linear perturbations of the final Kerr black hole, and a nonlinear region. At late times, the boundary between the two regions is an infalling shell. The BHP region contains late-time gravitational-waves emitted toward the future horizon, as well as those emitted toward future null infinity. In this region, by imposing no-ingoing wave conditions at past null infinity, and matching out-going waves at future null infinity with waveforms computed from numerical relativity, we can obtain waves that travel toward the future horizon. In particular, the Newman-Penrose $\psi_0$ associated with the in-going wave on the horizon is related to tidal deformations measured by fiducial observers floating above the horizon. We further determine the boundary of the BHP region on the future horizon by imposing that $\psi_0$ inside the BHP region can be faithfully represented by quasi-normal modes. Using a physically-motivated way to impose boundary conditions near the horizon, and applying the so-called Boltzmann reflectivity, we compute the quasi-normal modes of non-rotating ECOs, as well as gravitational-wave echoes. We also investigate the detectability of these echoes in current and future detectors, and prospects for parameter estimation.
|
1708.08125
|
Kirill Bronnikov
|
K.A. Bronnikov
|
Dyonic configurations in nonlinear electrodynamics coupled to general
relativity
|
6 two-column pages, no figures
|
Grav. Cosmol. 23, 343-348 (2017)
|
10.1134/S0202289317040053
| null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We consider static, spherically symmetric configurations in general
relativity, supported by nonlinear electromagnetic fields with gauge-invariant
Lagrangians depending on the single invariant $f = F_{\mu\nu} F^{\mu\nu}$.
After a brief review on black hole (BH) and solitonic solutions, obtained so
far with pure electric or magnetic fields, an attempt is made to obtain dyonic
solutions, those with both electric and magnetic charges. A general scheme is
suggested, leading to solutions in quadratures for an arbitrary Lagrangian
function $L(f)$ (up to some monotonicity restrictions); such solutions are
expressed in terms of $f$ as a new radial coordinate instead of the usual
coordinate $r$. For the truncated Born-Infeld theory (depending on the
invariant $f$ only), a general dyonic solution is obtained in terms of $r$. A
feature of interest in this solution is the existence of a special case with a
self-dual electromagnetic field, $f \equiv 0$ and the Reissner-Nordstr\"om
metric.
|
[
{
"created": "Sun, 27 Aug 2017 19:15:19 GMT",
"version": "v1"
}
] |
2020-10-20
|
[
[
"Bronnikov",
"K. A.",
""
]
] |
We consider static, spherically symmetric configurations in general relativity, supported by nonlinear electromagnetic fields with gauge-invariant Lagrangians depending on the single invariant $f = F_{\mu\nu} F^{\mu\nu}$. After a brief review on black hole (BH) and solitonic solutions, obtained so far with pure electric or magnetic fields, an attempt is made to obtain dyonic solutions, those with both electric and magnetic charges. A general scheme is suggested, leading to solutions in quadratures for an arbitrary Lagrangian function $L(f)$ (up to some monotonicity restrictions); such solutions are expressed in terms of $f$ as a new radial coordinate instead of the usual coordinate $r$. For the truncated Born-Infeld theory (depending on the invariant $f$ only), a general dyonic solution is obtained in terms of $r$. A feature of interest in this solution is the existence of a special case with a self-dual electromagnetic field, $f \equiv 0$ and the Reissner-Nordstr\"om metric.
|
2404.18811
|
Christian Pfeifer
|
Manuel Hohmann, Christian Pfeifer, Fabian Wagner
|
Weak equivalence principle and nonrelativistic limit of general
dispersion relations
|
18 pages
| null | null | null |
gr-qc hep-ph hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We study the weak equivalence principle in the context of modified dispersion
relations, a prevalent approach to quantum gravity phenomenology. We find that
generic modified dispersion relations violate the weak equivalence principle.
The acceleration in general depends on the mass of the test body, unless the
Hamiltonian is either two-homogeneous in the test particles' 4-momenta or the
corresponding Lagrangian differs from the homogeneous case by a total
derivative only. The key ingredient of this calculation is a $3+1$
decomposition of the parametrization invariant relativistic test particle
action derived from the dispersion relation. Additionally, we apply a
perturbative expansion in the test particle's spatial velocity and the inverse
speed of light. To quantify our result, we provide a general formula for the
E\"otv\'os factor of modified dispersion relations. As a specific example, we
study the $\kappa$-Poincar\'e dispersion relation. Comparing the ensuing
non-vanishing E\"otv\'os factor to recent data from the MICROSCOPE experiment,
we obtain a bound of $\kappa^{-1}\geq10^{15}{\rm GeV}/c^2.$.
|
[
{
"created": "Mon, 29 Apr 2024 15:48:49 GMT",
"version": "v1"
}
] |
2024-04-30
|
[
[
"Hohmann",
"Manuel",
""
],
[
"Pfeifer",
"Christian",
""
],
[
"Wagner",
"Fabian",
""
]
] |
We study the weak equivalence principle in the context of modified dispersion relations, a prevalent approach to quantum gravity phenomenology. We find that generic modified dispersion relations violate the weak equivalence principle. The acceleration in general depends on the mass of the test body, unless the Hamiltonian is either two-homogeneous in the test particles' 4-momenta or the corresponding Lagrangian differs from the homogeneous case by a total derivative only. The key ingredient of this calculation is a $3+1$ decomposition of the parametrization invariant relativistic test particle action derived from the dispersion relation. Additionally, we apply a perturbative expansion in the test particle's spatial velocity and the inverse speed of light. To quantify our result, we provide a general formula for the E\"otv\'os factor of modified dispersion relations. As a specific example, we study the $\kappa$-Poincar\'e dispersion relation. Comparing the ensuing non-vanishing E\"otv\'os factor to recent data from the MICROSCOPE experiment, we obtain a bound of $\kappa^{-1}\geq10^{15}{\rm GeV}/c^2.$.
|
2005.10871
|
Demosthenes Kivotides
|
Demosthenes Kivotides
|
Gravitomagnetic relativistic effects on turbulence
|
17 pages, 5 figures
|
International Journal of Modern Physics C (2021)
|
10.1142/S0129183121501291
| null |
gr-qc physics.flu-dyn
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The dynamics of fluid-matter under the influence of gravitomagnetic fields
are formulated and solved for the case of fully developed turbulence.
Gravitomagnetic effects reduce the vortical complexity and nonlinearity of
turbulence, even leading to its extinction within large volumes, and generate
departures from Kolmogorov turbulence scalings, that are explained via a
combination of dimensional and exact analysis arguments.
|
[
{
"created": "Thu, 21 May 2020 19:43:59 GMT",
"version": "v1"
}
] |
2021-04-29
|
[
[
"Kivotides",
"Demosthenes",
""
]
] |
The dynamics of fluid-matter under the influence of gravitomagnetic fields are formulated and solved for the case of fully developed turbulence. Gravitomagnetic effects reduce the vortical complexity and nonlinearity of turbulence, even leading to its extinction within large volumes, and generate departures from Kolmogorov turbulence scalings, that are explained via a combination of dimensional and exact analysis arguments.
|
2207.09641
|
Chae-Min Yun
|
Chae-min Yun, Jubin Park, Myung-Ki Cheoun and Dukjae Jang
|
An exact solution of the higher-order gravity in standard
radiation-dominated era
| null | null |
10.1016/j.physletb.2022.137652
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We report that the standard evolution of radiation-dominated era (RDE)
universe $a \propto t^{1/2}$ is a sufficient condition for solving a sixth
order gravitational field equation derived from the Lagrangian containing $B
R^{ab}R_{ab} + C R {R^{;c}}_{c}$ as well as a polynomial $f(R)$ for a spatially
flat radiation FLRW universe. By virtue of the similarity between
$R^{ab}R_{ab}$ and $R^2$ models up to the background order and of the vanishing
property of ${R^{;c}}_{c}$ for $ H = 1/(2t)$, the analytical solution can be
obtained from a special case to general one. This proves that the standard
cosmic evolution is valid even within modified gravitational theory involving
higher-order terms. An application of this background solution to the
tensor-type perturbation reduces the complicated equation to the standard
second order equation of gravitational wave. We discuss the possible ways to
discriminate the modified gravity model on the observations such as the
gravitational wave from the disturbed universe and primordial abundances.
|
[
{
"created": "Wed, 20 Jul 2022 04:05:53 GMT",
"version": "v1"
},
{
"created": "Thu, 28 Jul 2022 01:35:24 GMT",
"version": "v2"
},
{
"created": "Fri, 30 Sep 2022 03:59:46 GMT",
"version": "v3"
},
{
"created": "Mon, 2 Jan 2023 08:27:57 GMT",
"version": "v4"
}
] |
2023-01-04
|
[
[
"Yun",
"Chae-min",
""
],
[
"Park",
"Jubin",
""
],
[
"Cheoun",
"Myung-Ki",
""
],
[
"Jang",
"Dukjae",
""
]
] |
We report that the standard evolution of radiation-dominated era (RDE) universe $a \propto t^{1/2}$ is a sufficient condition for solving a sixth order gravitational field equation derived from the Lagrangian containing $B R^{ab}R_{ab} + C R {R^{;c}}_{c}$ as well as a polynomial $f(R)$ for a spatially flat radiation FLRW universe. By virtue of the similarity between $R^{ab}R_{ab}$ and $R^2$ models up to the background order and of the vanishing property of ${R^{;c}}_{c}$ for $ H = 1/(2t)$, the analytical solution can be obtained from a special case to general one. This proves that the standard cosmic evolution is valid even within modified gravitational theory involving higher-order terms. An application of this background solution to the tensor-type perturbation reduces the complicated equation to the standard second order equation of gravitational wave. We discuss the possible ways to discriminate the modified gravity model on the observations such as the gravitational wave from the disturbed universe and primordial abundances.
|
gr-qc/9811062
|
Cenalo T. A. Vaz
|
Cenalo Vaz (U. do Algarve) and Louis Witten (U. of Cincinnati)
|
Mass Quantization of the Schwarzschild Black Hole
|
Change in eq. (13). Factors of 4 cleaned up. Refs. added
|
Phys.Rev. D60 (1999) 024009
|
10.1103/PhysRevD.60.024009
|
UATP/9807
|
gr-qc hep-th
| null |
We examine the Wheeler-DeWitt equaton for a static, eternal Schwarzschild
black hole in Kucha\v r-Brown variables and obtain its energy eigenstates.
Consistent solutions vanish in the exterior of the Kruskal manifold and are
non-vanishing only in the interior. The system is reminiscent of a particle in
a box. States of definite parity avoid the singular geometry by vanishing at
the origin. These definite parity states admit a discrete energy spectrum,
depending on one quantum number which determines the Arnowitt-Deser-Misner
(ADM) mass of the black hole according to a relation conjectured long ago by
Bekenstein, $M \sim \sqrt{n}M_p$. If attention is restricted only to these
quantized energy states, a black hole is described not only by its mass but
also by its parity. States of indefinite parity do not admit a quantized mass
spectrum.
|
[
{
"created": "Wed, 18 Nov 1998 21:30:38 GMT",
"version": "v1"
},
{
"created": "Fri, 20 Nov 1998 19:06:08 GMT",
"version": "v2"
}
] |
2009-10-31
|
[
[
"Vaz",
"Cenalo",
"",
"U. do Algarve"
],
[
"Witten",
"Louis",
"",
"U. of Cincinnati"
]
] |
We examine the Wheeler-DeWitt equaton for a static, eternal Schwarzschild black hole in Kucha\v r-Brown variables and obtain its energy eigenstates. Consistent solutions vanish in the exterior of the Kruskal manifold and are non-vanishing only in the interior. The system is reminiscent of a particle in a box. States of definite parity avoid the singular geometry by vanishing at the origin. These definite parity states admit a discrete energy spectrum, depending on one quantum number which determines the Arnowitt-Deser-Misner (ADM) mass of the black hole according to a relation conjectured long ago by Bekenstein, $M \sim \sqrt{n}M_p$. If attention is restricted only to these quantized energy states, a black hole is described not only by its mass but also by its parity. States of indefinite parity do not admit a quantized mass spectrum.
|
1402.2063
|
Megandhren Govender
|
M. Govender
|
Non-adiabatic spherical collapse with a two-fluid atmosphere
|
12 pages, 2 figures
| null | null | null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this work we present an exact model of a spherically symmetric star
undergoing dissipative collapse in the form of a radial heat flux. The interior
of the star is matched smoothly to the generalised Vaidya line element
representing a two-fluid atmosphere comprising null radiation and a string
fluid. The influence of the string density on the thermal behaviour of the
model is investigated by employing a causal heat transport equation of
Maxwell-Cattaneo form.
|
[
{
"created": "Mon, 10 Feb 2014 08:18:19 GMT",
"version": "v1"
}
] |
2014-02-11
|
[
[
"Govender",
"M.",
""
]
] |
In this work we present an exact model of a spherically symmetric star undergoing dissipative collapse in the form of a radial heat flux. The interior of the star is matched smoothly to the generalised Vaidya line element representing a two-fluid atmosphere comprising null radiation and a string fluid. The influence of the string density on the thermal behaviour of the model is investigated by employing a causal heat transport equation of Maxwell-Cattaneo form.
|
gr-qc/0211036
|
Zoltan Perjes
|
Zolt\'an Perj\'es and M\'aty\'as Vas\'uth
|
Charged black holes: Wave equations for gravitational and
electromagnetic perturbations
|
12 pages, to appear in Ap.J
|
Astrophys.J. 582 (2003) 342-346
|
10.1086/344572
| null |
gr-qc astro-ph
| null |
A pair of wave equations for the electromagnetic and gravitational
perturbations of the charged Kerr black hole are derived. The perturbed
Einstein-Maxwell equations in a new gauge are employed in the derivation. The
wave equations refer to the perturbed Maxwell spinor $\Phi_0$ and to the shear
$\sigma$ of a principal null direction of the Weyl curvature. The whole
construction rests on the tripod of three distinct derivatives of the first
curvature $\kappa$ of a principal null direction.
|
[
{
"created": "Mon, 11 Nov 2002 14:30:03 GMT",
"version": "v1"
}
] |
2009-11-07
|
[
[
"Perjés",
"Zoltán",
""
],
[
"Vasúth",
"Mátyás",
""
]
] |
A pair of wave equations for the electromagnetic and gravitational perturbations of the charged Kerr black hole are derived. The perturbed Einstein-Maxwell equations in a new gauge are employed in the derivation. The wave equations refer to the perturbed Maxwell spinor $\Phi_0$ and to the shear $\sigma$ of a principal null direction of the Weyl curvature. The whole construction rests on the tripod of three distinct derivatives of the first curvature $\kappa$ of a principal null direction.
|
gr-qc/0510050
|
Sergei Alexandrov
|
Sergei Alexandrov
|
Reality conditions for Ashtekar gravity from Lorentz-covariant
formulation
|
14 pages
|
Class.Quant.Grav. 23 (2006) 1837-1850
|
10.1088/0264-9381/23/6/002
|
ITP-UU-05/45, SPIN-05/31
|
gr-qc
| null |
We show the equivalence of the Lorentz-covariant canonical formulation
considered for the Immirzi parameter $\beta=i$ to the selfdual Ashtekar
gravity. We also propose to deal with the reality conditions in terms of Dirac
brackets derived from the covariant formulation and defined on an extended
phase space which involves, besides the selfdual variables, also their
anti-selfdual counterparts.
|
[
{
"created": "Mon, 10 Oct 2005 15:56:41 GMT",
"version": "v1"
}
] |
2009-11-11
|
[
[
"Alexandrov",
"Sergei",
""
]
] |
We show the equivalence of the Lorentz-covariant canonical formulation considered for the Immirzi parameter $\beta=i$ to the selfdual Ashtekar gravity. We also propose to deal with the reality conditions in terms of Dirac brackets derived from the covariant formulation and defined on an extended phase space which involves, besides the selfdual variables, also their anti-selfdual counterparts.
|
1609.01340
|
Carlos A. R. Herdeiro
|
P. V. P. Cunha, J. Grover, C. Herdeiro, E. Radu, H. Runarsson, A.
Wittig
|
Chaotic lensing around boson stars and Kerr black holes with scalar hair
|
43 pages, 22 figures
|
Phys. Rev. D 94, 104023 (2016)
|
10.1103/PhysRevD.94.104023
| null |
gr-qc astro-ph.HE hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In a recent letter, arXiv:1509.00021, it was shown that the lensing of light
around rotating boson stars and Kerr black holes with scalar hair can exhibit
chaotic patterns. Since no separation of variables is known (or expected) for
geodesic motion on these backgrounds, we examine the 2D effective potentials
for photon trajectories, to obtain a deeper understanding of this phenomenon.
We find that the emergence of stable light rings on the background spacetimes,
allows the formation of "pockets" in one of the effective potentials, for open
sets of impact parameters, leading to an effective trapping of some
trajectories, dubbed quasi-bound orbits. We conclude that pocket formation
induces chaotic scattering, although not all chaotic orbits are associated to
pockets. These and other features are illustrated in a gallery of examples,
obtained with a new ray-tracing code, PYHOLE, which includes tools for a
simple, simultaneous visualization of the effective potential together with the
spacetime trajectory, for any given point in a lensing image. An analysis of
photon orbits allows us to further establish a positive correlation between
photon orbits in chaotic regions and those with more than one turning point in
the radial direction; we recall that the latter is not possible around Kerr
black holes. Moreover, we observe that the existence of several light rings
around a horizon (several fundamental orbits, including a stable one), is a
central ingredient for the existence of multiple shadows of a single hairy
black hole. We also exhibit the lensing and shadows by Kerr black holes with
scalar hair, observed away from the equatorial plane, obtained with PYHOLE.
|
[
{
"created": "Mon, 5 Sep 2016 22:12:58 GMT",
"version": "v1"
}
] |
2016-11-15
|
[
[
"Cunha",
"P. V. P.",
""
],
[
"Grover",
"J.",
""
],
[
"Herdeiro",
"C.",
""
],
[
"Radu",
"E.",
""
],
[
"Runarsson",
"H.",
""
],
[
"Wittig",
"A.",
""
]
] |
In a recent letter, arXiv:1509.00021, it was shown that the lensing of light around rotating boson stars and Kerr black holes with scalar hair can exhibit chaotic patterns. Since no separation of variables is known (or expected) for geodesic motion on these backgrounds, we examine the 2D effective potentials for photon trajectories, to obtain a deeper understanding of this phenomenon. We find that the emergence of stable light rings on the background spacetimes, allows the formation of "pockets" in one of the effective potentials, for open sets of impact parameters, leading to an effective trapping of some trajectories, dubbed quasi-bound orbits. We conclude that pocket formation induces chaotic scattering, although not all chaotic orbits are associated to pockets. These and other features are illustrated in a gallery of examples, obtained with a new ray-tracing code, PYHOLE, which includes tools for a simple, simultaneous visualization of the effective potential together with the spacetime trajectory, for any given point in a lensing image. An analysis of photon orbits allows us to further establish a positive correlation between photon orbits in chaotic regions and those with more than one turning point in the radial direction; we recall that the latter is not possible around Kerr black holes. Moreover, we observe that the existence of several light rings around a horizon (several fundamental orbits, including a stable one), is a central ingredient for the existence of multiple shadows of a single hairy black hole. We also exhibit the lensing and shadows by Kerr black holes with scalar hair, observed away from the equatorial plane, obtained with PYHOLE.
|
1406.3712
|
Behrouz Mirza
|
Fatemeh Lalehgani Dezaki, Behrouz Mirza
|
Generalized entropies and the expansion law of the universe
|
7 pages
|
Gen Relativ Gravit (2015) 47:67
|
10.1007/s10714-015-1910-8
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We suggest that using the first law of thermodynamics is a convenient method
to obtain a correct form of the expansion law of the universe \cite{T.
Padmanabhan1}. We will, then, use this idea to obtain the expansion law for a
Kodama observer. By using the expansion law for a Kodama observer, we can
obtain the dynamic equation of the FRW universe for deformed Horava-Lifshitz
gravity. The use of the first law of thermodynamics also leads to a new
approach for obtaining the Friedmann equations for f(R) and scalar tensor
gravities.
|
[
{
"created": "Sat, 14 Jun 2014 10:21:24 GMT",
"version": "v1"
},
{
"created": "Sat, 4 Jul 2015 08:46:11 GMT",
"version": "v2"
}
] |
2015-07-07
|
[
[
"Dezaki",
"Fatemeh Lalehgani",
""
],
[
"Mirza",
"Behrouz",
""
]
] |
We suggest that using the first law of thermodynamics is a convenient method to obtain a correct form of the expansion law of the universe \cite{T. Padmanabhan1}. We will, then, use this idea to obtain the expansion law for a Kodama observer. By using the expansion law for a Kodama observer, we can obtain the dynamic equation of the FRW universe for deformed Horava-Lifshitz gravity. The use of the first law of thermodynamics also leads to a new approach for obtaining the Friedmann equations for f(R) and scalar tensor gravities.
|
gr-qc/9506059
| null |
Vicente Pleitez
|
Concerning the vacuum velocity of gravitational waves
|
6 pages, REVTEX
| null | null |
IFT-P.031/95
|
gr-qc
| null |
It is pointed out that if gravitational interactions among ordinary bodies
propagate in extra space-time dimensions the velocity of gravitational waves in
vacuum could be different from the speed of light $c$.
|
[
{
"created": "Tue, 27 Jun 1995 14:11:00 GMT",
"version": "v1"
}
] |
2007-05-23
|
[
[
"Pleitez",
"Vicente",
""
]
] |
It is pointed out that if gravitational interactions among ordinary bodies propagate in extra space-time dimensions the velocity of gravitational waves in vacuum could be different from the speed of light $c$.
|
gr-qc/0411059
|
Roman Konoplya
|
R.A. Konoplya and A.V. Zhidenko
|
Decay of massive scalar field in a Schwarzschild background
|
8 pages, 3 figures, Physics Letters B, at press
|
Phys.Lett. B609 (2005) 377-384
|
10.1016/j.physletb.2005.01.078
| null |
gr-qc
| null |
The decay of massive scalar field in the Schwarzschild black hole background
is investigated here by consideration its quasinormal spectrum. It has been
proved that the so-called $quasi-resonant$ modes, which are arbitrary long
living (purely real) modes, can exist only if the effective potential is not
zero at least at one of the boundaries of the $R$-region. We have observed that
the quasinormal spectrum exists for all field masses and proved both
analytically and numerically that when $n \to \infty$ the real part of the
frequencies approaches the same asymptotical value ($\ln3/(8\pi M)$) as in the
case of the massless field.
|
[
{
"created": "Thu, 11 Nov 2004 19:50:05 GMT",
"version": "v1"
},
{
"created": "Sun, 6 Feb 2005 16:51:02 GMT",
"version": "v2"
}
] |
2009-11-10
|
[
[
"Konoplya",
"R. A.",
""
],
[
"Zhidenko",
"A. V.",
""
]
] |
The decay of massive scalar field in the Schwarzschild black hole background is investigated here by consideration its quasinormal spectrum. It has been proved that the so-called $quasi-resonant$ modes, which are arbitrary long living (purely real) modes, can exist only if the effective potential is not zero at least at one of the boundaries of the $R$-region. We have observed that the quasinormal spectrum exists for all field masses and proved both analytically and numerically that when $n \to \infty$ the real part of the frequencies approaches the same asymptotical value ($\ln3/(8\pi M)$) as in the case of the massless field.
|
0808.3575
|
Jose' P. S. Lemos
|
Gon\c{c}alo A. S. Dias, Jos\'e P. S. Lemos
|
Hamiltonian thermodynamics of charged three-dimensional dilatonic black
holes
|
38 pages, 3 figures
|
Phys.Rev.D78:084020,2008
|
10.1103/PhysRevD.78.084020
| null |
gr-qc hep-th math-ph math.MP
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The action for a class of three-dimensional dilaton-gravity theories, with an
electromagnetic Maxwell field and a cosmological constant, can be recast in a
Brans-Dicke-Maxwell type action, with its free $\omega$ parameter. For a
negative cosmological constant, these theories have static, electrically
charged, and spherically symmetric black hole solutions. Those theories with
well formulated asymptotics are studied through a Hamiltonian formalism, and
their thermodynamical properties are found. The theories studied are general
relativity, a dimensionally reduced cylindrical four-dimensional general
relativity theory, and a theory representing a class of theories, all with a
Maxwell term. The Hamiltonian formalism is setup in three dimensions through
foliations on the right region of the Carter-Penrose diagram, with the
bifurcation 1-sphere as the left boundary, and anti-de Sitter infinity as the
right one. The metric functions on the hypersurfaces and the radial component
of the vector potential one-form are the canonical coordinates. The Hamiltonian
action is written, the Hamiltonian being a sum of constraints. One finds a new
action which yields an unconstrained theory with two pairs of canonical
coordinates ${M,P_M; Q,P_Q}$, where $M$ is the mass parameter, which needs
renormalization, $P_M$ its conjugate momenta, $Q$ is the charge parameter, and
$P_Q$ its conjugate momentum. The resulting Hamiltonian is a sum of boundary
terms only. A quantization of the theory is performed. The Schr\"odinger
evolution operator is constructed, the trace is taken, and the partition
function of the grand canonical ensemble is obtained, the chemical potential
being the electric potential. The charged black hole entropies differ, in
general, from the usual quarter of the horizon area due to the dilaton.
|
[
{
"created": "Tue, 26 Aug 2008 19:48:56 GMT",
"version": "v1"
},
{
"created": "Tue, 26 Aug 2008 20:16:04 GMT",
"version": "v2"
}
] |
2009-02-23
|
[
[
"Dias",
"Gonçalo A. S.",
""
],
[
"Lemos",
"José P. S.",
""
]
] |
The action for a class of three-dimensional dilaton-gravity theories, with an electromagnetic Maxwell field and a cosmological constant, can be recast in a Brans-Dicke-Maxwell type action, with its free $\omega$ parameter. For a negative cosmological constant, these theories have static, electrically charged, and spherically symmetric black hole solutions. Those theories with well formulated asymptotics are studied through a Hamiltonian formalism, and their thermodynamical properties are found. The theories studied are general relativity, a dimensionally reduced cylindrical four-dimensional general relativity theory, and a theory representing a class of theories, all with a Maxwell term. The Hamiltonian formalism is setup in three dimensions through foliations on the right region of the Carter-Penrose diagram, with the bifurcation 1-sphere as the left boundary, and anti-de Sitter infinity as the right one. The metric functions on the hypersurfaces and the radial component of the vector potential one-form are the canonical coordinates. The Hamiltonian action is written, the Hamiltonian being a sum of constraints. One finds a new action which yields an unconstrained theory with two pairs of canonical coordinates ${M,P_M; Q,P_Q}$, where $M$ is the mass parameter, which needs renormalization, $P_M$ its conjugate momenta, $Q$ is the charge parameter, and $P_Q$ its conjugate momentum. The resulting Hamiltonian is a sum of boundary terms only. A quantization of the theory is performed. The Schr\"odinger evolution operator is constructed, the trace is taken, and the partition function of the grand canonical ensemble is obtained, the chemical potential being the electric potential. The charged black hole entropies differ, in general, from the usual quarter of the horizon area due to the dilaton.
|
2207.03125
|
Josu Aurrekoetxea
|
Josu C. Aurrekoetxea, Katy Clough, Eugene A. Lim
|
CTTK: A new method to solve the initial data constraints in numerical
relativity
|
14 pages, 4 figures, 1 appendix. Matches version published in CQG
| null |
10.1088/1361-6382/acb883
| null |
gr-qc
|
http://creativecommons.org/licenses/by/4.0/
|
In numerical relativity simulations with non-trivial matter configurations,
one must solve the Hamiltonian and momentum constraints of the ADM formulation
for the metric variables in the initial data. We introduce a new scheme based
on the standard Conformal Transverse-Traceless (CTT) decomposition, in which
instead of solving the Hamiltonian constraint as a 2nd order elliptic equation
for a choice of mean curvature $K$, we solve an algebraic equation for $K$ for
a choice of conformal factor. By doing so, we evade the existence and
uniqueness problem of solutions of the Hamiltonian constraint without using the
usual conformal rescaling of the source terms. This is particularly important
when the sources are fundamental fields, as reconstructing the fields'
configurations from the rescaled quantities is potentially problematic. Using
an iterative multigrid solver, we show that this method provides rapid
convergent solutions for several initial conditions that have not yet been
studied in numerical relativity; namely (i) periodic inhomogeneous spacetimes
with large random Gaussian scalar field perturbations and (ii) asymptotically
flat black hole spacetimes with rotating scalar clouds.
|
[
{
"created": "Thu, 7 Jul 2022 07:11:02 GMT",
"version": "v1"
},
{
"created": "Mon, 6 Mar 2023 14:14:00 GMT",
"version": "v2"
}
] |
2023-03-15
|
[
[
"Aurrekoetxea",
"Josu C.",
""
],
[
"Clough",
"Katy",
""
],
[
"Lim",
"Eugene A.",
""
]
] |
In numerical relativity simulations with non-trivial matter configurations, one must solve the Hamiltonian and momentum constraints of the ADM formulation for the metric variables in the initial data. We introduce a new scheme based on the standard Conformal Transverse-Traceless (CTT) decomposition, in which instead of solving the Hamiltonian constraint as a 2nd order elliptic equation for a choice of mean curvature $K$, we solve an algebraic equation for $K$ for a choice of conformal factor. By doing so, we evade the existence and uniqueness problem of solutions of the Hamiltonian constraint without using the usual conformal rescaling of the source terms. This is particularly important when the sources are fundamental fields, as reconstructing the fields' configurations from the rescaled quantities is potentially problematic. Using an iterative multigrid solver, we show that this method provides rapid convergent solutions for several initial conditions that have not yet been studied in numerical relativity; namely (i) periodic inhomogeneous spacetimes with large random Gaussian scalar field perturbations and (ii) asymptotically flat black hole spacetimes with rotating scalar clouds.
|
1109.5501
|
Wei-Tou Ni
|
Wei-Tou Ni
|
Foundations of Electromagnetism, Equivalence Principles and Cosmic
Interactions
|
25 pages, 4 figures, 2 pages, it is written as a chapter for the book
"Electromagnetism" (ISBN 979-953-307-400-8) to be published by INTECH (open
access), December, 2011
|
Trends in Electromagnetism - From Fundamentals to Applications
(March, 2012), InTech, pp. 45-68
| null | null |
gr-qc astro-ph.CO hep-ph
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We look at the foundations of electromagnetism in this chapter of the
"eletromagnetism" book. For doing this, after some review (constraints on
photon mass etc.), we use two approaches. The first one is to formulate a
Parametrized Post-Maxwellian framework to include QED corrections and a
pseudoscalar photon interaction. We discuss various vacuum birefringence
experiments - ongoing and proposed - to measure these parameters. The second
approach is to look at electromagnetism in gravity and various experiments and
observations to determine its empirical foundation. We found that the
foundation is solid with the only exception of a potentially possible
pseudoscalar-photon interaction. We discussed its experimental constraints and
look forward to more future experiments.
|
[
{
"created": "Mon, 26 Sep 2011 09:30:07 GMT",
"version": "v1"
}
] |
2012-03-26
|
[
[
"Ni",
"Wei-Tou",
""
]
] |
We look at the foundations of electromagnetism in this chapter of the "eletromagnetism" book. For doing this, after some review (constraints on photon mass etc.), we use two approaches. The first one is to formulate a Parametrized Post-Maxwellian framework to include QED corrections and a pseudoscalar photon interaction. We discuss various vacuum birefringence experiments - ongoing and proposed - to measure these parameters. The second approach is to look at electromagnetism in gravity and various experiments and observations to determine its empirical foundation. We found that the foundation is solid with the only exception of a potentially possible pseudoscalar-photon interaction. We discussed its experimental constraints and look forward to more future experiments.
|
1603.06039
|
Xin-Zhou Li
|
Ping Li, Xin-zhou Li and Ping Xi
|
Black hole solutions in de Rham-Gabadadze-Tolley massive gravity
|
12pages, no figure
|
Phys. Rev. D 93, 064040 (2016)
|
10.1103/PhysRevD.93.064040
| null |
gr-qc astro-ph.CO hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We present a detailed study of the static spherically symmetric solutions in
de Rham-Gabadadze-Tolley (dRGT) theory. Since the diffeomorphism invariance can
be restored by introducing the St\"{u}ckelberg fields $\phi^a$, there is new
invariant $I^{ab}=g^{\mu\nu}\partial_{\mu}\phi^a\partial_\nu\phi^b$ in the
massive gravity, which adds to the ones usually encountered in general
relativity (GR). In the unitary gauge $\phi^a=x^\mu\delta_\mu^a$, any inverse
metric $g^{\mu\nu}$ that has divergence including the coordinate singularity in
GR would exhibit a singularity in the invariant $I^{ab}$. Therefore, there is
no conventional Schwarzschild metric if we choose unitary gauge. In this paper,
we obtain a self-consistent static spherically symmetric ansatz in the
nonunitary gauge. Under this ansatz, we find that there are seven solutions
including the Schwarzschild solution, Reissner-Nordstr\"{o}m solution and five
other solutions. These solutions may possess an event horizon depending upon
the physical parameters (Schwarzschild radius $r_s$, scalar charge $S$ and/or
electric charge $Q$). If these solutions possess an event horizon, we show that
the singularity of $I^{ab}$ is absent at the horizon. Therefore, these
solutions may become candidates for black holes in dRGT.
|
[
{
"created": "Sat, 19 Mar 2016 03:40:05 GMT",
"version": "v1"
}
] |
2016-04-13
|
[
[
"Li",
"Ping",
""
],
[
"Li",
"Xin-zhou",
""
],
[
"Xi",
"Ping",
""
]
] |
We present a detailed study of the static spherically symmetric solutions in de Rham-Gabadadze-Tolley (dRGT) theory. Since the diffeomorphism invariance can be restored by introducing the St\"{u}ckelberg fields $\phi^a$, there is new invariant $I^{ab}=g^{\mu\nu}\partial_{\mu}\phi^a\partial_\nu\phi^b$ in the massive gravity, which adds to the ones usually encountered in general relativity (GR). In the unitary gauge $\phi^a=x^\mu\delta_\mu^a$, any inverse metric $g^{\mu\nu}$ that has divergence including the coordinate singularity in GR would exhibit a singularity in the invariant $I^{ab}$. Therefore, there is no conventional Schwarzschild metric if we choose unitary gauge. In this paper, we obtain a self-consistent static spherically symmetric ansatz in the nonunitary gauge. Under this ansatz, we find that there are seven solutions including the Schwarzschild solution, Reissner-Nordstr\"{o}m solution and five other solutions. These solutions may possess an event horizon depending upon the physical parameters (Schwarzschild radius $r_s$, scalar charge $S$ and/or electric charge $Q$). If these solutions possess an event horizon, we show that the singularity of $I^{ab}$ is absent at the horizon. Therefore, these solutions may become candidates for black holes in dRGT.
|
1507.08496
|
Shahram Panahiyan
|
S. H. Hendi, S. Panahiyan, R. Mamasani
|
Thermodynamic stability of charged BTZ black holes: Ensemble dependency
problem and its solution
|
20 pages and 15 figures
|
Gen. Relativ. Gravit. 47, 91 (2015)
|
10.1007/s10714-015-1932-2
| null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Motivated by the wide applications of thermal stability and phase transition,
we investigate thermodynamic properties of charged BTZ black holes. We apply
the standard method to calculate the heat capacity and the Hessian matrix and
find that thermal stability of charged BTZ solutions depends on the choice of
ensemble. To overcome this problem, we take into account cosmological constant
as a thermodynamical variable. By this modification, we show that the ensemble
dependency is eliminated and thermal stability conditions are the same in both
ensembles. Then, we generalize our solutions to the case of nonlinear
electrodynamics. We show how nonlinear matter field modifies the geometrical
behavior of the metric function. We also study phase transition and thermal
stability of these black holes in context of both canonical and grand canonical
ensembles. We show that by considering the cosmological constant as a
thermodynamical variable and modifying the Hessian matrix, the ensemble
dependency of thermal stability will be eliminated.
|
[
{
"created": "Tue, 28 Jul 2015 09:28:56 GMT",
"version": "v1"
}
] |
2015-11-25
|
[
[
"Hendi",
"S. H.",
""
],
[
"Panahiyan",
"S.",
""
],
[
"Mamasani",
"R.",
""
]
] |
Motivated by the wide applications of thermal stability and phase transition, we investigate thermodynamic properties of charged BTZ black holes. We apply the standard method to calculate the heat capacity and the Hessian matrix and find that thermal stability of charged BTZ solutions depends on the choice of ensemble. To overcome this problem, we take into account cosmological constant as a thermodynamical variable. By this modification, we show that the ensemble dependency is eliminated and thermal stability conditions are the same in both ensembles. Then, we generalize our solutions to the case of nonlinear electrodynamics. We show how nonlinear matter field modifies the geometrical behavior of the metric function. We also study phase transition and thermal stability of these black holes in context of both canonical and grand canonical ensembles. We show that by considering the cosmological constant as a thermodynamical variable and modifying the Hessian matrix, the ensemble dependency of thermal stability will be eliminated.
|
0910.5295
|
Ali Shojai
|
A. Shojai and F. Shojai
|
Statefinder diagnosis of nearly flat and thawing non-minimal
quintessence
|
8 figures. To appear in Euro. Phys. Lett. 2009
|
Europhys.Lett.88:30002,2009
|
10.1209/0295-5075/88/30002
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Non-minimally coupled scalar field models of dark energy are equivalent to an
interacting quintessence in the Einstein's frame. Considering two special
important choices of the potential of the scalar field, i.e. nearly flat and
thawing potential, one has an analytical expression for the equation of state
parameter as a function of the density parameter of the scalar field for any
choice. Here we investigate the non-minimal quintessence model by applying the
method of statefinder diagnosis to it and plotting the evolutionary
trajectories of the statefinder parameters.
|
[
{
"created": "Wed, 28 Oct 2009 05:25:21 GMT",
"version": "v1"
}
] |
2010-05-27
|
[
[
"Shojai",
"A.",
""
],
[
"Shojai",
"F.",
""
]
] |
Non-minimally coupled scalar field models of dark energy are equivalent to an interacting quintessence in the Einstein's frame. Considering two special important choices of the potential of the scalar field, i.e. nearly flat and thawing potential, one has an analytical expression for the equation of state parameter as a function of the density parameter of the scalar field for any choice. Here we investigate the non-minimal quintessence model by applying the method of statefinder diagnosis to it and plotting the evolutionary trajectories of the statefinder parameters.
|
gr-qc/0511074
|
Ricardo E. Gamboa Saravi
|
Ricardo E. Gamboa Saravi
|
The white wall, a gravitational mirror
|
8 pages, 1 figure, final version
|
Int.J.Mod.Phys.A23:1995-2003,2008
|
10.1142/S0217751X08039864
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We describe the exact solution of Einstein's equation corresponding to a
static homogenous distribution of matter with plane symmetry lying below $z=0$.
We study the geodesics in it and we show that this simple spacetime exhibits
very curious properties. In particular, it has a repelling singular boundary
and all geodesics bounce off it.
|
[
{
"created": "Mon, 14 Nov 2005 15:07:27 GMT",
"version": "v1"
},
{
"created": "Tue, 7 Mar 2006 15:46:36 GMT",
"version": "v2"
},
{
"created": "Mon, 16 Jul 2007 17:22:16 GMT",
"version": "v3"
},
{
"created": "Wed, 6 Feb 2008 14:00:25 GMT",
"version": "v4"
},
{
"created": "Tue, 11 Nov 2008 22:18:37 GMT",
"version": "v5"
}
] |
2008-11-26
|
[
[
"Saravi",
"Ricardo E. Gamboa",
""
]
] |
We describe the exact solution of Einstein's equation corresponding to a static homogenous distribution of matter with plane symmetry lying below $z=0$. We study the geodesics in it and we show that this simple spacetime exhibits very curious properties. In particular, it has a repelling singular boundary and all geodesics bounce off it.
|
gr-qc/9510023
|
Donald Marolf
|
Donald Marolf
|
Mass Superselection, Canonical Gauge Transformations, and Asymptotically
Flat Variational Principles
|
15 pages, ReVTeX, Minor changes made in response to referee's
commments
|
Class.Quant.Grav. 13 (1996) 1871-1884
|
10.1088/0264-9381/13/7/017
|
UCSBTH-95-25
|
gr-qc
| null |
The phase space reduction of Schwarzschild black holes by Thiemann and
Kastrup and by Kucha\v{r} is reexamined from a different perspective on gauge
freedom. This perspective introduces additional gauge transformations which
correspond to asymptotically nontrivial diffeomorphisms. Various subtleties
concerning variational principles for asymptotically flat systems are addressed
which allow us to avoid the usual conclusion that treating such transformations
as gauge implies the vanishing of corresponding total charges. Instead,
superselection rules are found for the (nonvanishing) ADM mass at the
asymptotic boundaries. The addition of phenomenological clocks at each
asymptotic boundary is also studied and compared with the `parametrization
clocks' of Kucha\v{r}.
|
[
{
"created": "Thu, 12 Oct 1995 22:57:01 GMT",
"version": "v1"
},
{
"created": "Tue, 7 Nov 1995 23:51:30 GMT",
"version": "v2"
},
{
"created": "Tue, 28 Nov 1995 00:58:53 GMT",
"version": "v3"
},
{
"created": "Wed, 3 Apr 1996 18:06:27 GMT",
"version": "v4"
}
] |
2009-10-28
|
[
[
"Marolf",
"Donald",
""
]
] |
The phase space reduction of Schwarzschild black holes by Thiemann and Kastrup and by Kucha\v{r} is reexamined from a different perspective on gauge freedom. This perspective introduces additional gauge transformations which correspond to asymptotically nontrivial diffeomorphisms. Various subtleties concerning variational principles for asymptotically flat systems are addressed which allow us to avoid the usual conclusion that treating such transformations as gauge implies the vanishing of corresponding total charges. Instead, superselection rules are found for the (nonvanishing) ADM mass at the asymptotic boundaries. The addition of phenomenological clocks at each asymptotic boundary is also studied and compared with the `parametrization clocks' of Kucha\v{r}.
|
gr-qc/0507127
|
Filimonova Irina V
|
D.J. Cirilo Lombardo
|
Nonlinear monopole, regularity conditions and the electromagnetic mass
in Einstein-Born-Infeld theories
|
Plenary talk presented at Workshop on High Energy Physics&Field
Theory (Protvino, Russia, 2004)
| null | null |
HEPFT/2004/8
|
gr-qc
| null |
In this work a new asymptotically flat solution of the coupled
Einstein-Born-Infeld equations for a static spherically symmetric space-time is
obtained. When the intrinsic mass is zero the resulting spacetime is regular
everywhere, in the sense given by B. Hoffmann and L. Infeld in 1937, and the
Einstein-Born-Infeld theory leads to the identification of the gravitational
with the electromagnetic mass.
|
[
{
"created": "Fri, 29 Jul 2005 07:04:45 GMT",
"version": "v1"
}
] |
2007-05-23
|
[
[
"Lombardo",
"D. J. Cirilo",
""
]
] |
In this work a new asymptotically flat solution of the coupled Einstein-Born-Infeld equations for a static spherically symmetric space-time is obtained. When the intrinsic mass is zero the resulting spacetime is regular everywhere, in the sense given by B. Hoffmann and L. Infeld in 1937, and the Einstein-Born-Infeld theory leads to the identification of the gravitational with the electromagnetic mass.
|
0709.1005
|
Roberto A. Sussman
|
Roberto A. Sussman
|
A dynamical system approach to inhomogeneous dust solutions
|
Enhanced version accepted for publication in Classical and Quantum
Gravity. Compiled with PdfLatex. RevTex style, 18 pdf figures
|
Class.Quant.Grav.25:015012,2008
|
10.1088/0264-9381/25/1/015012
| null |
gr-qc astro-ph math.DS nlin.SI
| null |
We examine numerically and qualitatively the Lema\^\i tre--Tolman--Bondi
(LTB) inhomogeneous dust solutions as a 3--dimensional dynamical system
characterized by six critical points. One of the coordinates of the phase space
is an average density parameter, $<\Omega>$, which behaves as the ordinary
$\Omega$ in Friedman-Lema\^\i tre--Robertson--Walker (FLRW) dust spacetimes.
The other two coordinates, a shear parameter and a density contrast function,
convey the effects of inhomogeneity. As long as shell crossing singularities
are absent, this phase space is bounded or it can be trivially compactified.
This space contains several invariant subspaces which define relevant
particular cases, such as: ``parabolic'' evolution, FLRW dust and the
Schwarzschild--Kruskal vacuum limit. We examine in detail the phase space
evolution of several dust configurations: a low density void formation
scenario, high density re--collapsing universes with open, closed and wormhole
topologies, a structure formation scenario with a black hole surrounded by an
expanding background, and the Schwarzschild--Kruskal vacuum case. Solution
curves start expanding from a past attractor (source) in the plane
$<\Omega>=1$, associated with self similar regime at an initial singularity.
Depending on the initial conditions and specific configurations, the curves
approach several saddle points as they evolve between this past attractor and
other two possible future attractors: perpetually expanding curves terminate at
a line of sinks at $<\Omega>=0$, while collapsing curves reach maximal
expansion as $<\Omega>$ diverges and end up in sink that coincides with the
past attractor and is also associated with self similar behavior.
|
[
{
"created": "Fri, 7 Sep 2007 06:25:23 GMT",
"version": "v1"
},
{
"created": "Sat, 24 Nov 2007 21:23:21 GMT",
"version": "v2"
}
] |
2008-11-26
|
[
[
"Sussman",
"Roberto A.",
""
]
] |
We examine numerically and qualitatively the Lema\^\i tre--Tolman--Bondi (LTB) inhomogeneous dust solutions as a 3--dimensional dynamical system characterized by six critical points. One of the coordinates of the phase space is an average density parameter, $<\Omega>$, which behaves as the ordinary $\Omega$ in Friedman-Lema\^\i tre--Robertson--Walker (FLRW) dust spacetimes. The other two coordinates, a shear parameter and a density contrast function, convey the effects of inhomogeneity. As long as shell crossing singularities are absent, this phase space is bounded or it can be trivially compactified. This space contains several invariant subspaces which define relevant particular cases, such as: ``parabolic'' evolution, FLRW dust and the Schwarzschild--Kruskal vacuum limit. We examine in detail the phase space evolution of several dust configurations: a low density void formation scenario, high density re--collapsing universes with open, closed and wormhole topologies, a structure formation scenario with a black hole surrounded by an expanding background, and the Schwarzschild--Kruskal vacuum case. Solution curves start expanding from a past attractor (source) in the plane $<\Omega>=1$, associated with self similar regime at an initial singularity. Depending on the initial conditions and specific configurations, the curves approach several saddle points as they evolve between this past attractor and other two possible future attractors: perpetually expanding curves terminate at a line of sinks at $<\Omega>=0$, while collapsing curves reach maximal expansion as $<\Omega>$ diverges and end up in sink that coincides with the past attractor and is also associated with self similar behavior.
|
2112.15077
|
Yang Liu
|
Yang Liu
|
Non-extensive Statistical Mechanics and the Thermodynamic Stability of
FRW Universe
| null |
EPL 2021
|
10.1209/0295-5075/ac3f52
| null |
gr-qc hep-th
|
http://creativecommons.org/licenses/by/4.0/
|
In this article, we investigate the thermodynamic stability of the FRW
universe for two examples, Tsallis entropy and loop quantum gravity, by
considering non-extensive statistical mechanics. The heat capacity, free energy
and pressure of the universe are obtained. For the Tsallis entropy model, we
obtained the constraint for $\beta$, namely, $1/2 < \beta < 2$. The free energy
of a thermal equilibrium universe must be less than zero. We suggest that the
reason for the accelerated expansion of the universe is not due to Tsallis
entropy. Similar results are obtained for loop quantum gravity. However, since
the values of $\Lambda(\gamma)$ and $q$ cannot be determined in this model, the
results become more subtle than that in the Tsallis entropy model. In addition,
we compare the results for the universe with those for a Schwarzschild black
hole.
|
[
{
"created": "Thu, 30 Dec 2021 14:41:35 GMT",
"version": "v1"
}
] |
2022-01-03
|
[
[
"Liu",
"Yang",
""
]
] |
In this article, we investigate the thermodynamic stability of the FRW universe for two examples, Tsallis entropy and loop quantum gravity, by considering non-extensive statistical mechanics. The heat capacity, free energy and pressure of the universe are obtained. For the Tsallis entropy model, we obtained the constraint for $\beta$, namely, $1/2 < \beta < 2$. The free energy of a thermal equilibrium universe must be less than zero. We suggest that the reason for the accelerated expansion of the universe is not due to Tsallis entropy. Similar results are obtained for loop quantum gravity. However, since the values of $\Lambda(\gamma)$ and $q$ cannot be determined in this model, the results become more subtle than that in the Tsallis entropy model. In addition, we compare the results for the universe with those for a Schwarzschild black hole.
|
gr-qc/0511098
|
Chen Songbai
|
Songbai Chen and Jiliang Jing
|
Late-time tail of a coupled scalar field in the background of a black
hole with a global monopole
|
12 pages, A corrected version to be appeared in MPLA
|
Mod.Phys.Lett.A23:359-369,2008
|
10.1142/S0217732308023888
| null |
gr-qc
| null |
Using the technique of spectral decomposition, we investigated the late-time
tails of massless and massive coupled scalar fields in the background of a
black hole with a global monopole. We found that due to existence of the
coupling between the scalar and gravitational fields, the massless scalar field
decay faster at timelike infinity $i_+$, and so does the massive one in the
intermediate late time. But the asymptotically late-time tail for the massive
scalar field is not affected and its decay rate still is $t^{-5/6}$.
|
[
{
"created": "Thu, 17 Nov 2005 08:23:39 GMT",
"version": "v1"
},
{
"created": "Wed, 20 Feb 2008 08:42:49 GMT",
"version": "v2"
}
] |
2008-11-26
|
[
[
"Chen",
"Songbai",
""
],
[
"Jing",
"Jiliang",
""
]
] |
Using the technique of spectral decomposition, we investigated the late-time tails of massless and massive coupled scalar fields in the background of a black hole with a global monopole. We found that due to existence of the coupling between the scalar and gravitational fields, the massless scalar field decay faster at timelike infinity $i_+$, and so does the massive one in the intermediate late time. But the asymptotically late-time tail for the massive scalar field is not affected and its decay rate still is $t^{-5/6}$.
|
1904.10407
|
Mikica Kocic
|
Mikica Kocic
|
Note on bimetric causal diagrams
|
3 pages, 4 figures, 1 table, Brief technical note
| null | null | null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
A new kind of diagrams is presented, showing the causal structure of bimetric
interactions.
|
[
{
"created": "Tue, 23 Apr 2019 16:24:55 GMT",
"version": "v1"
}
] |
2019-04-24
|
[
[
"Kocic",
"Mikica",
""
]
] |
A new kind of diagrams is presented, showing the causal structure of bimetric interactions.
|
0712.1796
|
Viktor Toth
|
J. W. Moffat and V. T. Toth
|
Fundamental parameter-free solutions in Modified Gravity
|
11 pages, 8 figures; accepted for publication in CQG
|
Class. Quantum Grav. 26 (2009) 085002
|
10.1088/0264-9381/26/8/085002
| null |
gr-qc astro-ph
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Modified Gravity (MOG) has been used successfully to explain the rotation
curves of galaxies, the motion of galaxy clusters, the Bullet Cluster, and
cosmological observations without the use of dark matter or Einstein's
cosmological constant. We now have the ability to demonstrate how these
solutions can be obtained directly from the action principle, without resorting
to the use of fitted parameters or empirical formulae. We obtain numerical
solutions to the theory's field equations that are exact in the sense that no
terms are omitted, in two important cases: the spherically symmetric, static
vacuum solution and the cosmological case of an homogeneous, isotropic
universe. We compare these results to selected astrophysical and cosmological
observations.
|
[
{
"created": "Tue, 11 Dec 2007 19:19:03 GMT",
"version": "v1"
},
{
"created": "Wed, 2 Jan 2008 20:11:52 GMT",
"version": "v2"
},
{
"created": "Mon, 5 May 2008 22:46:33 GMT",
"version": "v3"
},
{
"created": "Sun, 1 Jun 2008 17:24:47 GMT",
"version": "v4"
},
{
"created": "Fri, 27 Feb 2009 15:46:16 GMT",
"version": "v5"
}
] |
2009-04-04
|
[
[
"Moffat",
"J. W.",
""
],
[
"Toth",
"V. T.",
""
]
] |
Modified Gravity (MOG) has been used successfully to explain the rotation curves of galaxies, the motion of galaxy clusters, the Bullet Cluster, and cosmological observations without the use of dark matter or Einstein's cosmological constant. We now have the ability to demonstrate how these solutions can be obtained directly from the action principle, without resorting to the use of fitted parameters or empirical formulae. We obtain numerical solutions to the theory's field equations that are exact in the sense that no terms are omitted, in two important cases: the spherically symmetric, static vacuum solution and the cosmological case of an homogeneous, isotropic universe. We compare these results to selected astrophysical and cosmological observations.
|
1002.3057
|
Jan Steinhoff
|
J. Steinhoff, S. Hergt, G. Sch\"afer
|
ADM canonical formulation with spin and application to post-Newtonian
approximations
|
4 pages, Proceedings of the 12th Marcel Grossman Meeting
| null | null | null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Recently, different methods succeeded in calculating the spin dynamics at
higher orders in the post-Newtonian (PN) approximation. This is an essential
step toward the determination of more accurate templates for gravitational
waves, to be used in future gravitational wave astronomy. We focus on the
extension of the ADM canonical formalism to spinning binary black holes. Using
the global Poincare invariance of asymptotically flat spacetimes as the most
important guiding consistency condition, this extension can be constructed
order by order in the PN approximation. We were able to reach a high order both
in the spin power and the PN counting.
|
[
{
"created": "Tue, 16 Feb 2010 12:04:29 GMT",
"version": "v1"
}
] |
2010-02-17
|
[
[
"Steinhoff",
"J.",
""
],
[
"Hergt",
"S.",
""
],
[
"Schäfer",
"G.",
""
]
] |
Recently, different methods succeeded in calculating the spin dynamics at higher orders in the post-Newtonian (PN) approximation. This is an essential step toward the determination of more accurate templates for gravitational waves, to be used in future gravitational wave astronomy. We focus on the extension of the ADM canonical formalism to spinning binary black holes. Using the global Poincare invariance of asymptotically flat spacetimes as the most important guiding consistency condition, this extension can be constructed order by order in the PN approximation. We were able to reach a high order both in the spin power and the PN counting.
|
1312.4103
|
Yi Xie
|
Yi Xie and Xue-Mei Deng
|
$f(T)$ gravity: effects on astronomical observation and Solar System
experiments and upper-bounds
|
6 pages
|
MNRAS (August 21, 2013) 433 (4): 3584-3589
|
10.1093/mnras/stt991
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
As an extension of a previous work in which perihelion advances are
considered only and as an attempt to find more stringent constraints on its
parameters, we investigate effects on astronomical observation and experiments
conducted in the Solar System due to the $f(T)$ gravity which contains a
quadratic correction of $\alpha T^2$ ($\alpha$ is a model parameter) and the
cosmological constant $\Lambda$. Using a spherical solution describing the
Sun's gravitational field, the resulting secular evolution of planetary orbital
motions, light deflection, gravitational time delay and frequency shift are
calculated up to the leading contribution. Among them, we find qualitatively
that the light deflection holds a unique bound on $\alpha$, without dependence
on $\Lambda$, and the time delay experiments during inferior conjunction impose
a clean constraint on $\Lambda$, regardless of $\alpha$. Based on observation
and experiments, especially the supplementary advances in the perihelia
provided by the INPOP10a ephemeris, we obtain the upper-bounds quantitatively:
$|\alpha| \le 1.2 \times 10^{2}$ m${}^2$ and $ |\Lambda| \le 1.8 \times
10^{-43}$ m${}^{-2}$, at least 10 times tighter than the previous result.
|
[
{
"created": "Sun, 15 Dec 2013 02:56:37 GMT",
"version": "v1"
}
] |
2013-12-17
|
[
[
"Xie",
"Yi",
""
],
[
"Deng",
"Xue-Mei",
""
]
] |
As an extension of a previous work in which perihelion advances are considered only and as an attempt to find more stringent constraints on its parameters, we investigate effects on astronomical observation and experiments conducted in the Solar System due to the $f(T)$ gravity which contains a quadratic correction of $\alpha T^2$ ($\alpha$ is a model parameter) and the cosmological constant $\Lambda$. Using a spherical solution describing the Sun's gravitational field, the resulting secular evolution of planetary orbital motions, light deflection, gravitational time delay and frequency shift are calculated up to the leading contribution. Among them, we find qualitatively that the light deflection holds a unique bound on $\alpha$, without dependence on $\Lambda$, and the time delay experiments during inferior conjunction impose a clean constraint on $\Lambda$, regardless of $\alpha$. Based on observation and experiments, especially the supplementary advances in the perihelia provided by the INPOP10a ephemeris, we obtain the upper-bounds quantitatively: $|\alpha| \le 1.2 \times 10^{2}$ m${}^2$ and $ |\Lambda| \le 1.8 \times 10^{-43}$ m${}^{-2}$, at least 10 times tighter than the previous result.
|
2002.08844
|
M. Farasat Shamir
|
M. Farasat Shamir
|
$f(\mathcal{R},\varphi,\chi)$ Cosmology with Noether Symmetry
|
11 pages, 3 figures
|
Eur. Phys. J. C 80 (2020) 115
|
10.1140/epjc/s10052-020-7682-7
| null |
gr-qc
|
http://creativecommons.org/licenses/by/4.0/
|
This paper is devoted to explore modified $f(\mathcal{R})$ theories of
gravity using Noether symmetry approach. For this purpose,
Friedmann-Robertson-Walker spacetime is chosen to investigate the cosmic
evolution. The study is mainly divided into two parts: Firstly Noether
symmetries of metric $f(\mathcal{R})$ gravity are revisited and some new class
of solutions with the help of conserved quantities are reported. It is shown
that different scenarios of cosmic evolution can be discussed using Noether
symmetries and one of the case indicates the chances for the existence of Big
Rip singularity. Secondly, $f(\mathcal{R})$ theory coupled with scalar field
has been discussed in detail. The Noether equations of modified gravity are
reported with three subcases for flat Friedmann-Robertson-Walker universe. It
is concluded that conserved quantities are quite helpful to find some important
exact solutions in the cosmological contexts. Moreover, the scalar field
involved in the modified gravity plays a vital role in the cosmic evolution and
an accelerated expansion phase can be observed for some suitable choices of
$f(\mathcal{R},\varphi,\chi)$ gravity models.
|
[
{
"created": "Tue, 18 Feb 2020 04:10:53 GMT",
"version": "v1"
}
] |
2020-02-21
|
[
[
"Shamir",
"M. Farasat",
""
]
] |
This paper is devoted to explore modified $f(\mathcal{R})$ theories of gravity using Noether symmetry approach. For this purpose, Friedmann-Robertson-Walker spacetime is chosen to investigate the cosmic evolution. The study is mainly divided into two parts: Firstly Noether symmetries of metric $f(\mathcal{R})$ gravity are revisited and some new class of solutions with the help of conserved quantities are reported. It is shown that different scenarios of cosmic evolution can be discussed using Noether symmetries and one of the case indicates the chances for the existence of Big Rip singularity. Secondly, $f(\mathcal{R})$ theory coupled with scalar field has been discussed in detail. The Noether equations of modified gravity are reported with three subcases for flat Friedmann-Robertson-Walker universe. It is concluded that conserved quantities are quite helpful to find some important exact solutions in the cosmological contexts. Moreover, the scalar field involved in the modified gravity plays a vital role in the cosmic evolution and an accelerated expansion phase can be observed for some suitable choices of $f(\mathcal{R},\varphi,\chi)$ gravity models.
|
1706.09505
|
Liudmila Fesik Ms
|
Liudmila Fesik
|
Polarization states of gravitational waves detected by LIGO-Virgo
antennas
|
45 pages, Master thesis
| null | null | null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The detection of the first gravitational wave events by the Advanced LIGO
Scientific Collaboration has opened a new possibility for the study of
fundamental physics of gravitational interaction.
This work conducts an analysis of possible polarization states of
gravitational waves (GW) radiated by the most promising types of sources to be
detected by the modern interferometric antennas: coalescing compact binaries
and collapsing supernovae. Several theoretical approaches to the current as
well as future gravitational wave signals interpretation are discussed together
with a strategy for a search for corresponding transients by means of
multimessenger astronomy.
One of the aims of this thesis is to develop a new method for GW source
localization depending on a polarization state of an incoming GW in the case of
a detection by two interferometric antennas. Additionally, there is elaborated
a further method focused on a possibility to recognise different polarization
states of a GW detected by means of a network with three and more antennas in
operation. The both proposed methods have been applied to the LIGO events
GW150914, GW151226 and LVT151012, together with the matching of the results
with the currently known electromagnetic follow-ups to these GW events.
The conclusion of this research is that there are opportunities for verifying
different predictions of the scalar-tensor theories of gravitation by means of
the analysis of the polarization states of the detected gravitational waves.
All in all, this work provides a new test of the theoretical assumptions
about the nature of gravity as well as about the processes in relativistic
compact objects of various types.
|
[
{
"created": "Wed, 28 Jun 2017 22:41:55 GMT",
"version": "v1"
}
] |
2017-06-30
|
[
[
"Fesik",
"Liudmila",
""
]
] |
The detection of the first gravitational wave events by the Advanced LIGO Scientific Collaboration has opened a new possibility for the study of fundamental physics of gravitational interaction. This work conducts an analysis of possible polarization states of gravitational waves (GW) radiated by the most promising types of sources to be detected by the modern interferometric antennas: coalescing compact binaries and collapsing supernovae. Several theoretical approaches to the current as well as future gravitational wave signals interpretation are discussed together with a strategy for a search for corresponding transients by means of multimessenger astronomy. One of the aims of this thesis is to develop a new method for GW source localization depending on a polarization state of an incoming GW in the case of a detection by two interferometric antennas. Additionally, there is elaborated a further method focused on a possibility to recognise different polarization states of a GW detected by means of a network with three and more antennas in operation. The both proposed methods have been applied to the LIGO events GW150914, GW151226 and LVT151012, together with the matching of the results with the currently known electromagnetic follow-ups to these GW events. The conclusion of this research is that there are opportunities for verifying different predictions of the scalar-tensor theories of gravitation by means of the analysis of the polarization states of the detected gravitational waves. All in all, this work provides a new test of the theoretical assumptions about the nature of gravity as well as about the processes in relativistic compact objects of various types.
|
2006.16430
|
Jose Wadih Maluf Dr.
|
J. W. Maluf
|
Distorted Torsion Tensor, Teleparallelism and Spin 2 Field Equations
|
13 pages, no figures. A third model is presented, which yields field
equations that are symmetric and invariant under local Lorentz
transformations
| null | null | null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
A notion of distorted torsion tensor was introduced by Okubo, in the
establishment of the Nijenhuis-Bianchi identity and of BRST-like operators.
These quantities are constructed with the help of the Nijenhuis tensor, which
in turn is defined in terms of a (1,1) tensor $S^\lambda_\mu$. This tensor
enters the construction of the distorted torsion tensor. We use this tensor to
extend the teleparallel equivalent of general relativity (TEGR) into a theory
defined by the tetrad fields and by the tensor $S^\lambda_\mu$. The ordinary
TEGR is recovered if $S^\lambda_\mu=\delta^\lambda_\mu$. We consider the flat
space-time formulation of the theory, in terms of $S^\lambda_\mu$ only, and
show that this tensor satisfies the wave equation for massless spin 2 fields.
|
[
{
"created": "Mon, 29 Jun 2020 23:12:39 GMT",
"version": "v1"
},
{
"created": "Tue, 7 Jul 2020 16:40:04 GMT",
"version": "v2"
}
] |
2020-07-08
|
[
[
"Maluf",
"J. W.",
""
]
] |
A notion of distorted torsion tensor was introduced by Okubo, in the establishment of the Nijenhuis-Bianchi identity and of BRST-like operators. These quantities are constructed with the help of the Nijenhuis tensor, which in turn is defined in terms of a (1,1) tensor $S^\lambda_\mu$. This tensor enters the construction of the distorted torsion tensor. We use this tensor to extend the teleparallel equivalent of general relativity (TEGR) into a theory defined by the tetrad fields and by the tensor $S^\lambda_\mu$. The ordinary TEGR is recovered if $S^\lambda_\mu=\delta^\lambda_\mu$. We consider the flat space-time formulation of the theory, in terms of $S^\lambda_\mu$ only, and show that this tensor satisfies the wave equation for massless spin 2 fields.
|
2003.14206
|
Rabia Saleem
|
R. Saleem and M. Zubair
|
Inflationary Solution of Hamilton Jacobi Equations during Weak
Dissipative Regime
|
22 pages, 4 figures
|
Phys. Scr. 95(2020)035214
|
10.1088/1402-4896/ab4954
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
In this paper, an elegant mathematical approach is introduced to solve the
equations of warm inflationary model without using extra approximations other
than slow-roll. This important inflationary method known as Hamilton-Jacobian
formalism. Here tachyon field and the imperfect fluid are considered to be the
cosmic ingredients to create inflation. A general formalism is developed for
the considered inflationary model and further work is restricted to weak
dissipative regime. A detailed analysis of the model is presented for three
different choices of bulk and dissipative coefficients taking as constant as
well as variable (function of Hubble parameter and inflaton). In each case, the
involved model parameters are constrained to plot the physical acceptable range
of scalar spectral index and tensor to scalar ratio. The parametric
trajectories proved that the acquired results for all the three cases are
compatible with Planck astrophysical data. Furthermore, the existence of warm
inflation and slow-roll limit are also verified graphically.
|
[
{
"created": "Sun, 29 Mar 2020 13:40:05 GMT",
"version": "v1"
}
] |
2020-04-08
|
[
[
"Saleem",
"R.",
""
],
[
"Zubair",
"M.",
""
]
] |
In this paper, an elegant mathematical approach is introduced to solve the equations of warm inflationary model without using extra approximations other than slow-roll. This important inflationary method known as Hamilton-Jacobian formalism. Here tachyon field and the imperfect fluid are considered to be the cosmic ingredients to create inflation. A general formalism is developed for the considered inflationary model and further work is restricted to weak dissipative regime. A detailed analysis of the model is presented for three different choices of bulk and dissipative coefficients taking as constant as well as variable (function of Hubble parameter and inflaton). In each case, the involved model parameters are constrained to plot the physical acceptable range of scalar spectral index and tensor to scalar ratio. The parametric trajectories proved that the acquired results for all the three cases are compatible with Planck astrophysical data. Furthermore, the existence of warm inflation and slow-roll limit are also verified graphically.
|
gr-qc/9812066
|
Garcia
|
L.C.Garcia de Andrade
|
Chern-Simons electrodynamics in (2+1)-spacetime with torsion
|
5 pages latex
| null | null | null |
gr-qc
| null |
Chern-Simons electrodynamics in 2+1-spacetimes with torsion is investigated.
We start from the usual Chern-Simons (CS) electrodynamics Lagrangian and Cartan
torsion is introduced in the covariant derivative and by a direct coupling of
torsion vector to the CS field. Variation of the Lagrangian with respect to
torsion shows that Chern-Simons field is proportional to the product of the
square of the scalar field and torsion. The electric field is proportional to
torsion vector and the magnetic flux is computed in terms of the time-component
of the two dimensional torsion. Contrary to early massive electrodynamics in
the present model the photon mass does not depend on torsion.
|
[
{
"created": "Fri, 18 Dec 1998 03:07:47 GMT",
"version": "v1"
}
] |
2007-05-23
|
[
[
"de Andrade",
"L. C. Garcia",
""
]
] |
Chern-Simons electrodynamics in 2+1-spacetimes with torsion is investigated. We start from the usual Chern-Simons (CS) electrodynamics Lagrangian and Cartan torsion is introduced in the covariant derivative and by a direct coupling of torsion vector to the CS field. Variation of the Lagrangian with respect to torsion shows that Chern-Simons field is proportional to the product of the square of the scalar field and torsion. The electric field is proportional to torsion vector and the magnetic flux is computed in terms of the time-component of the two dimensional torsion. Contrary to early massive electrodynamics in the present model the photon mass does not depend on torsion.
|
gr-qc/9710038
|
Luc Blanchet
|
Luc Blanchet
|
Gravitational-wave tails of tails
|
Contains 2 files: a tex file B98tailgrqc.tex and a latex file
tabtail.tex. This version includes the correction of an Erratum to appear in
Classical and Quantum Gravity (2005)
|
Class.Quant.Grav.15:113-141,1998; Erratum-ibid.22:3381,2005
|
10.1088/0264-9381/15/1/009
| null |
gr-qc
| null |
The tails of gravitational waves are caused by scattering of linear waves
onto the space-time curvature generated by the total mass-energy of the source.
Quite naturally, the tails of tails are caused by curvature scattering of the
tails of waves themselves. The tails of tails are associated with the cubic
non-linear interaction between two mass monopole moments and, dominantly, the
mass quadrupole of the source. In this paper we determine the radiation field
at large distances from the source for this particular
monopole-monopole-quadrupole interaction. We find that the tails of tails
appear at the third post-Newtonian (3PN) order beyond the usual quadrupole
radiation. Motivated by the need of accurate templates to be used in the data
analysis of future detectors of gravitational waves, we compute the
contribution of tails, and of tails of tails, up to the 3.5PN order in the
energy flux generated by inspiraling compact binaries.
|
[
{
"created": "Tue, 7 Oct 1997 10:02:11 GMT",
"version": "v1"
},
{
"created": "Fri, 27 May 2005 16:24:16 GMT",
"version": "v2"
}
] |
2011-08-11
|
[
[
"Blanchet",
"Luc",
""
]
] |
The tails of gravitational waves are caused by scattering of linear waves onto the space-time curvature generated by the total mass-energy of the source. Quite naturally, the tails of tails are caused by curvature scattering of the tails of waves themselves. The tails of tails are associated with the cubic non-linear interaction between two mass monopole moments and, dominantly, the mass quadrupole of the source. In this paper we determine the radiation field at large distances from the source for this particular monopole-monopole-quadrupole interaction. We find that the tails of tails appear at the third post-Newtonian (3PN) order beyond the usual quadrupole radiation. Motivated by the need of accurate templates to be used in the data analysis of future detectors of gravitational waves, we compute the contribution of tails, and of tails of tails, up to the 3.5PN order in the energy flux generated by inspiraling compact binaries.
|
gr-qc/9305010
|
Dadhich
|
L. K. Patel and Naresh Dadhich
|
Singularity Free Inhomogeneous Models with Heat Flow
|
6 pages, TeX, to appear in Class.Quant.Grav
|
Class.Quant.Grav.10:L85-L88,1993
|
10.1088/0264-9381/10/7/002
| null |
gr-qc
| null |
We present a class of singularity free exact cosmological solutions of
Einstein's equations describing a perfect fluid with heat flow. It is obtained
as generalization of the Senovilla class [1] corresponding to incoherent
radiation field. The spacetime is cylindrically symmetric and globally regular.
|
[
{
"created": "Wed, 12 May 1993 10:23:57 GMT",
"version": "v1"
}
] |
2010-04-06
|
[
[
"Patel",
"L. K.",
""
],
[
"Dadhich",
"Naresh",
""
]
] |
We present a class of singularity free exact cosmological solutions of Einstein's equations describing a perfect fluid with heat flow. It is obtained as generalization of the Senovilla class [1] corresponding to incoherent radiation field. The spacetime is cylindrically symmetric and globally regular.
|
1511.04439
|
Axel de la Macorra
|
Axel de la Macorra
|
Dark Energy Parametrization motivated by Scalar Field Dynamics
|
23 pages, 15 figures. arXiv admin note: substantial text overlap with
arXiv:1108.0876
| null |
10.1088/0264-9381/33/9/095001
| null |
gr-qc astro-ph.CO
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We propose a new Dark Energy parametrization based on the dynamics of a
scalar field. We use an equation of state w=(x-1)/(x+1), with x=E_k/V, the
ratio of kinetic energy E_k=\dotphi^2/2 and potential V. The equation of motion
gives x=(L/6)(V/3H^2) and has a solution x=([(1+y)^2+2 L/3]^{1/2}-(1+y))/2
where y\equiv \rmm/V and L= (V'/V)^2 (1+q)^2, q=\ddotphi/V'. The resulting EoS
is w=[6+ L- 6 \sqrt((1+y)^2+2L/3)]/(L+6y). Since the universe is accelerating
at present time we use the slow roll approximation in which case we have |q|<<
1 and L\simeq (V'/V)^2. However, the derivation of w is exact and has no
approximation. By choosing an appropriate ansatz for L we obtain a wide class
of behavior for the evolution of Dark Energy without the need to specify the
potential V. The EoS w can either grow and later decrease, or other way around,
as a function of redshift and it is constraint between -1\leq w\leq 1 as for
any canonical scalar field with only gravitational interaction. To determine
the dynamics of Dark Energy we calculate the background evolution and its
perturbations, since they are important to discriminate between different DE
models. Our parametrization follows closely the dynamics of a scalar field
scalar fields and the function L allow us to connect it with the potential
V(phi) of the scalar field phi.
|
[
{
"created": "Thu, 12 Nov 2015 23:48:17 GMT",
"version": "v1"
}
] |
2016-04-27
|
[
[
"de la Macorra",
"Axel",
""
]
] |
We propose a new Dark Energy parametrization based on the dynamics of a scalar field. We use an equation of state w=(x-1)/(x+1), with x=E_k/V, the ratio of kinetic energy E_k=\dotphi^2/2 and potential V. The equation of motion gives x=(L/6)(V/3H^2) and has a solution x=([(1+y)^2+2 L/3]^{1/2}-(1+y))/2 where y\equiv \rmm/V and L= (V'/V)^2 (1+q)^2, q=\ddotphi/V'. The resulting EoS is w=[6+ L- 6 \sqrt((1+y)^2+2L/3)]/(L+6y). Since the universe is accelerating at present time we use the slow roll approximation in which case we have |q|<< 1 and L\simeq (V'/V)^2. However, the derivation of w is exact and has no approximation. By choosing an appropriate ansatz for L we obtain a wide class of behavior for the evolution of Dark Energy without the need to specify the potential V. The EoS w can either grow and later decrease, or other way around, as a function of redshift and it is constraint between -1\leq w\leq 1 as for any canonical scalar field with only gravitational interaction. To determine the dynamics of Dark Energy we calculate the background evolution and its perturbations, since they are important to discriminate between different DE models. Our parametrization follows closely the dynamics of a scalar field scalar fields and the function L allow us to connect it with the potential V(phi) of the scalar field phi.
|
1704.05632
|
Sergey Chervon
|
Sunil D. Maharaj, Aroonkumar Beesham, Sergey V. Chervon and Aleksandr
S. Kubasov
|
New Exact Solutions for a Chiral Cosmological Model in 5D EGB Gravity
|
9 pages, the article is a reflection of the talk given at the
Ulyanovsk International School-Seminar "Problems of theoretical and
observation cosmology - UISS 2016", September 19-30, Ulyanovsk, Russia
| null |
10.1134/S0202289317040120
| null |
gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We consider a chiral cosmological model in the framework of
Einstein-Gauss-Bonnet cosmology. Using a decomposition of the latter equations
in such a way that the first chiral field is responsible for the Einstein part
of the model, while the second field together with the kinetic interaction is
connected with the Gauss--Bonnet part of the theory, we find new exact
solutions for the 2-component chiral cosmological model with and without the
kinetic interaction between fields.
|
[
{
"created": "Wed, 19 Apr 2017 07:10:56 GMT",
"version": "v1"
}
] |
2017-12-06
|
[
[
"Maharaj",
"Sunil D.",
""
],
[
"Beesham",
"Aroonkumar",
""
],
[
"Chervon",
"Sergey V.",
""
],
[
"Kubasov",
"Aleksandr S.",
""
]
] |
We consider a chiral cosmological model in the framework of Einstein-Gauss-Bonnet cosmology. Using a decomposition of the latter equations in such a way that the first chiral field is responsible for the Einstein part of the model, while the second field together with the kinetic interaction is connected with the Gauss--Bonnet part of the theory, we find new exact solutions for the 2-component chiral cosmological model with and without the kinetic interaction between fields.
|
2206.14320
|
Katsuki Aoki
|
Katsuki Aoki and Masato Minamitsuji
|
Resolving the pathologies of self-interacting Proca fields: A case study
of Proca stars
|
14 pages, 7 figures, to appear in PRD
| null | null |
YITP-22-67
|
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
It has been argued that a self-interacting massive vector field is
pathological due to a dynamical formation of a singular effective metric of the
vector field, which is the onset of a gradient or ghost instability. We discuss
that this singularity formation is not necessarily a fundamental problem but a
breakdown of the effective field theory (EFT) description of the massive vector
field. By using a model of ultraviolet (UV) completion of the massive vector
field, we demonstrate that a Proca star, a self-gravitating condensate of the
vector field, continues to exist even after the EFT suffers from a gradient
instability without any pathology at UV, in which the EFT description is still
valid and the gradient instability in EFT may be interpreted as a standard
dynamical instability of a high-density boson star from the UV perspective. On
the other hand, we find that the EFT description is broken before the ghost
instability appears. This suggests that a heavy degree of freedom may be
spontaneously excited to cure the pathology of the EFT as the EFT dynamically
tends to approach the onset of the ghost instability.
|
[
{
"created": "Tue, 28 Jun 2022 23:09:44 GMT",
"version": "v1"
},
{
"created": "Wed, 14 Sep 2022 07:43:39 GMT",
"version": "v2"
}
] |
2022-09-15
|
[
[
"Aoki",
"Katsuki",
""
],
[
"Minamitsuji",
"Masato",
""
]
] |
It has been argued that a self-interacting massive vector field is pathological due to a dynamical formation of a singular effective metric of the vector field, which is the onset of a gradient or ghost instability. We discuss that this singularity formation is not necessarily a fundamental problem but a breakdown of the effective field theory (EFT) description of the massive vector field. By using a model of ultraviolet (UV) completion of the massive vector field, we demonstrate that a Proca star, a self-gravitating condensate of the vector field, continues to exist even after the EFT suffers from a gradient instability without any pathology at UV, in which the EFT description is still valid and the gradient instability in EFT may be interpreted as a standard dynamical instability of a high-density boson star from the UV perspective. On the other hand, we find that the EFT description is broken before the ghost instability appears. This suggests that a heavy degree of freedom may be spontaneously excited to cure the pathology of the EFT as the EFT dynamically tends to approach the onset of the ghost instability.
|
1404.1874
|
Betti Hartmann
|
Yves Brihaye (Universite de Mons, Belgium), Betti Hartmann (IFSC,
Universidade de S\~ao Paulo, Brazil), J\"urgen Riedel (LABORES Paris, France)
|
Self-interacting boson stars with a single Killing vector field in
Anti-de Sitter
|
v5: 17 pages, 10 figures, matches version accepted for publication in
Phys. Rev. D
|
Phys. Rev. D 92, 044049 (2015)
|
10.1103/PhysRevD.92.044049
| null |
gr-qc hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We construct rotating boson stars in (4+1)-dimensional asymptotically Anti-de
Sitter space-time (aAdS) with two equal angular momenta that are composed out
of a massive and self-interacting scalar field. These solutions possess a
single Killing vector field. We construct explicit solutions of the equations
in the case of a fixed AdS background and vanishing self-coupling of the scalar
field. These are the generalizations of the oscillons discussed in the
literature previously now taking the mass of the scalar field into account. We
study the evolution of the spectrum of massive oscillons when taking
backreaction and/or the self-coupling into account numerically. We observe that
very compact boson stars possess an ergoregion.
|
[
{
"created": "Mon, 7 Apr 2014 18:18:25 GMT",
"version": "v1"
},
{
"created": "Thu, 24 Apr 2014 17:31:16 GMT",
"version": "v2"
},
{
"created": "Wed, 2 Jul 2014 16:33:54 GMT",
"version": "v3"
},
{
"created": "Wed, 1 Apr 2015 23:28:35 GMT",
"version": "v4"
},
{
"created": "Sun, 2 Aug 2015 21:58:52 GMT",
"version": "v5"
}
] |
2015-09-02
|
[
[
"Brihaye",
"Yves",
"",
"Universite de Mons, Belgium"
],
[
"Hartmann",
"Betti",
"",
"IFSC,\n Universidade de São Paulo, Brazil"
],
[
"Riedel",
"Jürgen",
"",
"LABORES Paris, France"
]
] |
We construct rotating boson stars in (4+1)-dimensional asymptotically Anti-de Sitter space-time (aAdS) with two equal angular momenta that are composed out of a massive and self-interacting scalar field. These solutions possess a single Killing vector field. We construct explicit solutions of the equations in the case of a fixed AdS background and vanishing self-coupling of the scalar field. These are the generalizations of the oscillons discussed in the literature previously now taking the mass of the scalar field into account. We study the evolution of the spectrum of massive oscillons when taking backreaction and/or the self-coupling into account numerically. We observe that very compact boson stars possess an ergoregion.
|
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