Spatially Homogeneous Rotating Solution in f(R) Gravity and Its Energy Contents

M. Jamil Amir, Saima Naheed

In this paper, the metric approach of f(R) theory of gravity is used to investigate the exact vacuum solutions of spatially homogeneous rotating spacetimes. For this purpose, R is replaced by f(R) in the standard Einstein-Hilbert action and the set of modified Einstein field equations reduce to a single equation. We adopt the assumption of constant Ricci scalar which maybe zero or non-zero. Moreover, the energy density of the non-trivial solution has been evaluated by using the generalized Landau-Lifshitz energy-momentum complex in the perspective of f(R) gravity for some appropriate f(R) model, which turns out to be a constant quantity.

Cite as: arXiv:1312.6684 [gr-qc]
(or arXiv:1312.6684v1 [gr-qc] for this version)

Approximate Black Hole Binary Spacetime via Asymptotic Matching

Bruno C. Mundim, Hiroyuki Nakano, Nicolás Yunes, Manuela Campanelli, Scott C. Noble, Yosef Zlochower

We construct a fully-analytic, general relativistic, non-spinning black hole binary spacetime that approximately solves the vacuum Einstein equations everywhere in space and time for black holes sufficiently well-separated. The metric is constructed by asymptotically matching perturbed Schwarzschild metrics near each black hole to a two-body post-Newtonian metric far from them, and a two-body post-Minkowskian metric farther still. Asymptotic matching is done without linearizing about a particular time slice, and thus it is valid dynamically and for all times, provided the binary is sufficiently well-separated. This approximate global metric can be used for long dynamical evolutions of relativistic magnetohydrodynamical, circumbinary disks around inspiraling supermassive black holes to study a variety of phenomena.

Cite as: arXiv:1312.6731 [gr-qc]
(or arXiv:1312.6731v1 [gr-qc] for this version)

Jebsen-Birkhoff theorem and its stability in f(R) gravity

Anne Marie Nzioki, Rituparno Goswami, Peter K. S. Dunsby

We prove a Jebsen-Birkhoff like theorem for f(R) theories of gravity in order to to find the necessary conditions required for the existence of the Schwarzschild solution in these theories and demonstrate that the rigidity of such solutions of f(R) gravity is valid even in the perturbed scenario.

Cite as: arXiv:1312.6790 [gr-qc]
(or arXiv:1312.6790v1 [gr-qc] for this version)

On the thermodynamic stability of rotating black holes in higher dimensions — a comparison of thermodynamic ensembles

Brian P. Dolan

Thermodynamic potentials relevant to the micro-canonical, the canonical and the grand-canonical ensembles, associated with rotating black holes in D-dimensions, are analysed and compared. Such black holes are known to be thermodynamically unstable, but the instability is a consequence of a subtle interplay between specific heats and the moments of inertia and it manifests itself differently in the different ensembles. A simple relation between the product of the specific heat and the determinant of the moment of inertia in both the canonical and the grand-canonical ensembles is derived. Myers-Perry black holes in arbitrary dimension are studied in detail. All temperature extrema in the micro-canonical ensemble are determined and classified. The specific heat and the moment of inertia tensor are evaluated in both the canonical and the grand-canonical ensembles in any dimension. All zeros and poles of the specific heats, as a function of the angular momenta, are determined and the eigenvalues of the isentropic moment of inertia tensor are also found and classified. It is further shown that many of the thermodynamic properties of a Myers-Perry black hole in D-2 dimensions can be obtained from those of a black hole in D dimensions by sending one of the angular momenta to infinity.

Cite as: arXiv:1312.6810 [gr-qc]
(or arXiv:1312.6810v1 [gr-qc] for this version)

Thermodynamics of the polymeric quantized Schwarzschild black hole

M. A. Gorji, K. Nozari, B. Vakili

Polymer representation of quantum mechanics is an effective approach to loop quantum gravity. In this paper we develop statistical mechanics in the polymer framework. While to obtain energies of microstates one needs usually to solve the polymer-modified Schr\”{o}dinger equation, we have not adopted this strategy here since it is not an easy task due to the complicated form of the Schr\”{o}dinger equation in the polymer picture. Instead, we formulate the ensemble theory in polymer framework in a semi-classical regime through deformed density of states. We show that our results are in good agreement with those arising from quantum mechanical considerations. Applying this method to thermodynamics of quantum Schwarzschild black hole, we obtain corrections to the Bekenstein-Hawking entropy due to loop quantum gravity effects.

Cite as: arXiv:1312.6835 [gr-qc]
(or arXiv:1312.6835v1 [gr-qc] for this version)

A perturbative and gauge invariant treatment of gravitational wave memory

Lydia Bieri, David Garfinkle

We present a perturbative treatment of gravitational wave memory. The coordinate invariance of Einstein’s equations leads to a type of gauge invariance in perturbation theory. As with any gauge invariant theory, results are more clear when expressed in terms of manifestly gauge invariant quantities. Therefore we derive all our results from the perturbed Weyl tensor rather than the perturbed metric. We derive gravitational wave memory for the Einstein equations coupled to a general energy-momentum tensor that reaches null infinity.

Cite as: arXiv:1312.6871 [gr-qc]
(or arXiv:1312.6871v1 [gr-qc] for this version)

Higher Spin Resolution of a Toy Big Bang

Chethan Krishnan, Shubho Roy

Diffeomorphisms preserve spacetime singularities, whereas higher spin symmetries need not. Since three dimensional de Sitter space has quotients that have big-bang/big-crunch singularities and since dS_3-gravity can be written as an SL(2,C) Chern-Simons theory, we investigate SL(3,C) Chern-Simons theory as a higher-spin context in which these singularities might get resolved. As in the case of higher spin black holes in AdS_3, the solutions are invariantly characterized by their holonomies. We show that the dS_3 quotient singularity can be de-singularized by an SL(3,C) gauge transformation that preserves the holonomy: this is a higher spin resolution the cosmological singularity. Our work deals exclusively with the bulk theory, and is independent of the subtleties involved in defining a CFT_2 dual to dS_3 in the sense of dS/CFT.

DOI: 10.1103/PhysRevD.88.044049
Cite as: arXiv:1305.1277 [hep-th]
(or arXiv:1305.1277v4 [hep-th] for this version)

Perihelion precession and starlight deflection in the general spherical symmetry spacetime

Ya-Peng Hu, Hong-Sheng Zhang, Jun-Peng Hou, Liang-Zun Tang

Perihelion precession of Mercury and starlight deflection in the solar system are two well-known phenomenons. Since they can give the evidences to show the correctness of general relativity in the history, these two phenomenons become important. In this paper, we first generalize the perihelion precession and starlight deflection to the general spherical symmetry spacetime, and hence obtain the main equation. Then, we choose the Schwarzchild-AdS solution and Reissner-Nordstorm solution as two special spherical symmetry spacetimes to discuss the probable effects from the cosmological constant and electric charge on the perihelion precession and starlight deflection. Our results show that the cosmological constant can affect the precession angle of perihelion, while it does not affect the deflection angle of starlight. For the electric charge, it can both affect the two angles. Furthermore, we also give some discussions according to the experiment data.

Cite as: arXiv:1312.7419 [gr-qc]
(or arXiv:1312.7419v1 [gr-qc] for this version)

Gravitational energy, gravitational pressure, and the thermodynamics of a charged black hole in teleparallel gravity

K. H. C. Castello-Branco, J. F. da Rocha-Neto

We investigate, in the case of a Reissner-Nordstr\”om black hole, the definitions of gravitational energy and gravitational pressure that naturally arise in the framework of the Teleparallel Equivalent of General Relativity. In particular, we calculate the gravitational energy enclosed by the event horizon of the black hole, E, and the radial pressure over it, p. With these quantities we then analyse the thermodynamic relation dE + pdV (as p turns out to be a density, dV is actually given by dV = dr d\theta d\phi, in spherically-type coordinates). We compare the latter with the standard first law of black hole dynamics. Also, by identifying TdS = dE + pdV, we comment on a possible modification of the standard, Bekenstein-Hawking entropy-area relation due to gravitational energy and gravitational pressure of the black hole. The infinitesimal variations in question refer to the Penrose process for a Reissner-Nordstr\”om black hole.

DOI: 10.1103/PhysRevD.88.024045
Cite as: arXiv:1312.7478 [gr-qc]
(or arXiv:1312.7478v1 [gr-qc] for this version)

Configurations of a new atomic interferometer for gravitational wave detection

Biao Tang, Baocheng Zhang, Lin Zhou, Jin Wang, Mingsheng Zhan

Recently, the configuration using atomic interferometers (AIs) had been suggested for the detection of gravitational waves. A new AI with some additional laser pulses for implementing large momentum transfer was also put forward, in order to improve the influence of shot noise and laser frequency noise. In the paper, we use the sensitivity function to analyze all possible configurations of the new AI and to distinguish how many momenta are transferred in a specific configuration. With the analysis for the new configuration, we explore the detection scheme of gravitational wave further, in particular, for the amelioration of the laser frequency noise. We find that the amelioration is definite in such scheme, but novelly, in some cases the frequency noise can be canceled completely by using a proper data processing method.

Cite as: arXiv:1312.7652 [gr-qc]
(or arXiv:1312.7652v1 [gr-qc] for this version)