scholarly journals Stability analysis of black holes via a catastrophe theory and black hole thermodynamics in generalized theories of gravity

2003 ◽  
Vol 68 (2) ◽  
Author(s):  
Takashi Tamaki ◽  
Takashi Torii ◽  
Kei-ichi Maeda
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Stability Analysis ◽  
Catastrophe Theory ◽  
Black Hole Thermodynamics ◽  
Theories Of Gravity

scholarly journals A CONFORMAL AFFINE TODA MODEL OF 2D BLACK HOLES: A QUANTUM STUDY OF THE EVAPORATION END POINT

1993 ◽  
Vol 08 (27) ◽  
pp. 2593-2605
Author(s):  
F. BELGIORNO ◽  
A.S. CATTANEO ◽  
F. FUCITO ◽  
M. MARTELLINI
Keyword(s):  
Field Theory ◽  
Black Holes ◽  
Black Hole ◽  
Group Analysis ◽  
Black Hole Thermodynamics ◽  
Dilaton Gravity ◽  
Final State ◽  
Renormalization Group Analysis ◽  
Conformal Field ◽  
Toda Model

In this paper we reformulate the dilaton-gravity theory of Callan et al. as a new effective conformal field theory which turns out to be a generalization of the so-called SL 2-conformal affine Toda (CAT) theory studied some time ago by Babelon and Bonora. We quantize this model, thus keeping in account the dilaton-gravity quantum effects. We then implement a Renormalization Group analysis to study the black hole thermodynamics and the final state of the Hawking evaporation.

scholarly journals On the black holes in alternative theories of gravity: The case of nonlinear massive gravity

2015 ◽  
Vol 24 (03) ◽  
pp. 1550022 ◽  
Author(s):  
Ivan Arraut
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Degrees Of Freedom ◽  
Massive Gravity ◽  
Alternative Theories Of Gravity ◽  
De Sitter ◽  
Theories Of Gravity ◽  
Bound Orbits ◽  
Black Hole Temperature ◽  
Alternative Theories

I derive general conditions in order to explain the origin of the Vainshtein radius inside dRGT. The set of equations, which I have called "Vainshtein" conditions are extremal conditions of the dynamical metric (gμν) containing all the degrees of freedom of the theory. The Vainshtein conditions are able to explain the coincidence between the Vainshtein radius in dRGT and the scale [Formula: see text], obtained naturally from the Schwarzschild de-Sitter (S-dS) space inside general relativity (GR). In GR, this scale was interpreted as the maximum distance in order to get bound orbits. The same scale corresponds to the static observer position if we want to define the black hole temperature in an asymptotically de-Sitter space. In dRGT, the scale marks a limit after which the extra degrees of freedom of the theory become relevant.

scholarly journals Black hole thermodynamics in Snyder phase space

2017 ◽  
Vol 14 (11) ◽  
pp. 1750164
Author(s):  
Sara Saghafi ◽  
Kourosh Nozari
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Phase Space ◽  
Symplectic Structure ◽  
Symplectic Manifolds ◽  
Black Hole Thermodynamics ◽  
Schwarzschild Black Hole ◽  
Noncommutative Phase Space ◽  
Physics Of Black Holes ◽  
First Time

By defining a noncommutative symplectic structure, we study thermodynamics of Schwarzschild black hole in a Snyder noncommutative phase space for the first time. Since natural cutoffs are the results of compactness of symplectic manifolds in phase space, the physics of black holes in such a space would be affected mainly by these cutoffs. In this respect, this study provides a basis for more deeper understanding of the black hole thermodynamics in a pure mathematical viewpoint.

scholarly journals Spherically symmetric black holes with electric and magnetic charge in extended gravity: physical properties, causal structure, and stability analysis in Einstein’s and Jordan’s frames

2020 ◽  
Vol 80 (2) ◽  
Author(s):  
E. Elizalde ◽  
G. G. L. Nashed ◽  
S. Nojiri ◽  
S. D. Odintsov
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Stability Analysis ◽  
Physical Properties ◽  
Causal Structure ◽  
Hawking Temperature ◽  
The Novel ◽  
Extended Gravity ◽  
Static Black Hole ◽  
Black Hole Solutions

Abstract Novel static black hole solutions with electric and magnetic charges are derived for the class of modified gravities: $$f({{{\mathcal {R}}}})={{{\mathcal {R}}}}+2\beta \sqrt{{{\mathcal {R}}}}$$f(R)=R+2βR, with or without a cosmological constant. The new black holes behave asymptotically as flat or (A)dS space-times with a dynamical value of the Ricci scalar given by $$R=\frac{1}{r^2}$$R=1r2 and $$R=\frac{8r^2\Lambda +1}{r^2}$$R=8r2Λ+1r2, respectively. They are characterized by three parameters, namely their mass and electric and magnetic charges, and constitute black hole solutions different from those in Einstein’s general relativity. Their singularities are studied by obtaining the Kretschmann scalar and Ricci tensor, which shows a dependence on the parameter $$\beta $$β that is not permitted to be zero. A conformal transformation is used to display the black holes in Einstein’s frame and check if its physical behavior is changed w.r.t. the Jordan one. To this end, thermodynamical quantities, as the entropy, Hawking temperature, quasi-local energy, and the Gibbs free energy are calculated to investigate the thermal stability of the solutions. Also, the casual structure of the new black holes is studied, and a stability analysis is performed in both frames using the odd perturbations technique and the study of the geodesic deviation. It is concluded that, generically, there is coincidence of the physical properties of the novel black holes in both frames, although this turns not to be the case for the Hawking temperature.

THICK EINSTEIN SHELLS AS “HEAT" BATHS FOR BLACK HOLES

1994 ◽  
Vol 03 (01) ◽  
pp. 171-174 ◽  
Author(s):  
G.L. COMER
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Heat Bath ◽  
Black Hole Thermodynamics

We discuss the significance of the “heat” bath for black hole thermodynamics and how to represent it as a thick Einstein shell.

scholarly journals Black hole event horizons — Teleology and predictivity

2017 ◽  
Vol 32 (34) ◽  
pp. 1750186
Author(s):  
Swastik Bhattacharya ◽  
S. Shankaranarayanan
Keyword(s):  
Boundary Condition ◽  
Black Holes ◽  
Black Hole ◽  
Black Hole Thermodynamics ◽  
Navier Stokes ◽  
Navier Stokes Equation ◽  
Black Hole Evaporation ◽  
Spacetime Manifold ◽  
Statistical Mechanical ◽  
Late Stages

General Relativity predicts the existence of black holes. Access to the complete spacetime manifold is required to describe the black hole. This feature necessitates that black hole dynamics is specified by future or teleological boundary condition. Here, we demonstrate that the statistical mechanical description of black holes, the raison d’être behind the existence of black hole thermodynamics, requires teleological boundary condition. Within the fluid–gravity paradigm — Einstein’s equations when projected on spacetime horizons resemble Navier–Stokes equation of a fluid — we show that the specific heat and the coefficient of bulk viscosity of the horizon fluid are negative only if the teleological boundary condition is taken into account. We argue that in a quantum theory of gravity, the future boundary condition plays a crucial role. We briefly discuss the possible implications of this at late stages of black hole evaporation.

scholarly journals Constructing Higher-Dimensional Exact Black Holes in Einstein-Maxwell-Scalar Theory

Universe ◽  
2020 ◽  
Vol 6 (9) ◽  
pp. 148
Author(s):  
Jianhui Qiu ◽  
Changjun Gao
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Black Hole Thermodynamics ◽  
Spherically Symmetric ◽  
Dilaton Gravity ◽  
Scalar Theory ◽  
First Law Of Thermodynamics ◽  
Higher Dimensional

We construct higher-dimensional and exact black holes in Einstein-Maxwell-scalar theory. The strategy we adopted is to extend the known, static and spherically symmetric black holes in the Einstein-Maxwell dilaton gravity and Einstein-Maxwell-scalar theory. Then we investigate the black hole thermodynamics. Concretely, the generalized Smarr formula and the first law of thermodynamics are derived.

scholarly journals Black hole thermodynamics and heat engines in conformal gravity

2017 ◽  
Vol 26 (13) ◽  
pp. 1750151 ◽  
Author(s):  
Hao Xu ◽  
Yuan Sun ◽  
Liu Zhao
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Black Hole Thermodynamics ◽  
Spherically Symmetric ◽  
Conformal Gravity ◽  
Extended Phase ◽  
Heat Engines ◽  
Equation Of States ◽  
Symmetric Black Hole ◽  
Black Hole Solutions

The extended phase-space thermodynamics and heat engines for static spherically symmetric black hole solutions of four-dimensional conformal gravity are studied in detail. It is argued that the equation of states (EOS) for such black holes is always branched, any continuous thermodynamical process cannot drive the system from one branch of the EOS into another branch. Meanwhile, the thermodynamical volume is bounded from above, making the black holes always super-entropic in one branch and may also be super-entropic in another branch in certain range of the temperature. The Carnot and Stirling heat engines associated to such black holes are shown to be distinct from each other. For rectangular heat engines, the efficiency always approaches zero when the rectangle becomes extremely narrow, and given the highest and lowest working temperatures fixed, there is always a maximum for the efficiency of such engines.

scholarly journals Mass formulae and staticity condition for dark matter charged black holes

2020 ◽  
Vol 80 (9) ◽  
Author(s):  
Marek Rogatko
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dark Matter ◽  
Black Hole Solution ◽  
Black Hole Thermodynamics ◽  
Stationary Black Hole ◽  
Charged Black Holes ◽  
Hidden Sector ◽  
Killing Horizon ◽  
Interior Boundary

AbstractThe Arnowitt–Deser–Misner formalism is used to derive variations of mass, angular momentum and canonical energy for Einstein–Maxwell dark matter gravity in which the auxiliary gauge field coupled via kinetic mixing term to the ordinary Maxwell one, which mimics properties of hidden sector. Inspection of the initial data for the manifold with an interior boundary, having topology of $$S^2$$ S 2 , enables us to find the generalised first law of black hole thermodynamics in the aforementioned theory. It has been revealed that the stationary black hole solution being subject to the condition of encompassing a bifurcate Killing horizon with a bifurcation sphere, which is non-rotating, must be static and has vanishing magnetic Maxwell and dark matter sector fields, on static slices of the spacetime under consideration.

scholarly journals BLACK HOLES AND THE THIRD LAW OF THERMODYNAMICS

2004 ◽  
Vol 13 (04) ◽  
pp. 739-770 ◽  
Author(s):  
F. BELGIORNO ◽  
M. MARTELLINI
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Second Law Of Thermodynamics ◽  
Temperature Limit ◽  
Black Hole Thermodynamics ◽  
Zero Temperature ◽  
The Third ◽  
Third Law Of Thermodynamics ◽  
Third Law ◽  
Extremal Black Holes

We discuss in the framework of black hole thermodynamics some aspects relative to the third law in the case of black holes of the Kerr–Newman family. In the light of the standard proof of the equivalence between the unattainability of the zero temperature and the entropic version of the third law it is remarked that the unattainability has a special character in black hole thermodynamics. Also the zero temperature limit which obtained in the case of very massive black holes is discussed and it is shown that a violation of the entropic version in the charged case occurs. The violation of the Bekenstein–Hawking law in favour of zero entropy SE=0 in the case of extremal black holes is suggested as a natural solution for a possible violation of the second law of thermodynamics. Thermostatic arguments in support of the unattainability are explored, and SE=0 for extremal black holes is shown to be again a viable solution. The third law of black hole dynamics by W. Israel is then interpreted as a further strong corroboration to the picture of a discontinuity between extremal states and non-extremal ones.

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