scholarly journals Higher derivative corrections to Kerr black hole thermodynamics

2019 ◽  
Vol 2019 (4) ◽  
Author(s):  
Harvey S. Reall ◽  
Jorge E. Santos
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Black Hole Thermodynamics ◽  
Higher Derivative

The influence of the generalized uncertainty principle on Kerr black hole thermodynamics

2018 ◽  
Vol 48 (5) ◽  
pp. 050401 ◽  
Author(s):  
ShanPing WU ◽  
ChengZhou LIU ◽  
QiaoJun CAO ◽  
Sheng WANG ◽  
RuYa REN ◽  
...  
Keyword(s):  
Black Hole ◽  
Uncertainty Principle ◽  
Generalized Uncertainty Principle ◽  
Kerr Black Hole ◽  
Black Hole Thermodynamics

scholarly journals A Zeroth Law Compatible Model to Kerr Black Hole Thermodynamics

Universe ◽  
2017 ◽  
Vol 3 (1) ◽  
pp. 14 ◽  
Author(s):  
Viktor Czinner ◽  
Hideo Iguchi
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Black Hole Thermodynamics

Black hole spectroscopy from a class of Plebański and Demiański space–times

2014 ◽  
Vol 92 (1) ◽  
pp. 46-50
Author(s):  
De-Jiang Qi
Keyword(s):  
Black Hole ◽  
Normal Modes ◽  
Kerr Black Hole ◽  
Black Hole Thermodynamics ◽  
Area Spectrum ◽  
Spherically Symmetric ◽  
Adiabatic Invariance ◽  
Schwarzschild Black Hole ◽  
Gravity System ◽  
Area Spectra

Recently, via adiabatic invariance, Majhi and Vagenas quantized the horizon area of the general class of a static spherically symmetric space–time. Very recently, applying the period of the gravity system with respect to the Euclidean time, Zeng and Liu derived area spectra of a Schwarzschild black hole and a Kerr black hole. It is noteworthy that the preceding methods are not useful for the quasi-normal modes. In this paper, based on those works, and as a further study, adopting near horizon approximation, applying the laws of black hole thermodynamics, we would like to investigate the black hole spectroscopy from a class of Plebański and Demiański space–times by using two different methods. The result shows that the area spectrum of the black hole is [Formula: see text], which confirms the initial proposal of Bekenstein, and the result is consistent with that already obtained by Maggiore with quasi-normal modes.

scholarly journals Duality and supersymmetry constraints on the weak gravity conjecture

2020 ◽  
Vol 2020 (11) ◽  
Author(s):  
Gregory J. Loges ◽  
Toshifumi Noumi ◽  
Gary Shiu
Keyword(s):  
Black Hole ◽  
Scattering Amplitudes ◽  
Energy Condition ◽  
Null Energy Condition ◽  
Black Hole Thermodynamics ◽  
Simple Condition ◽  
Mass Ratio ◽  
Higher Derivative ◽  
Bps States ◽  
Weak Gravity

Abstract Positivity bounds coming from consistency of UV scattering amplitudes are not always sufficient to prove the weak gravity conjecture for theories beyond Einstein-Maxwell. Additional ingredients about the UV may be necessary to exclude those regions of parameter space which are naïvely in conflict with the predictions of the weak gravity conjecture. In this paper we explore the consequences of imposing additional symmetries inherited from the UV theory on higher-derivative operators for Einstein-Maxwell-dilaton-axion theory. Using black hole thermodynamics, for a preserved SL(2, ℝ) symmetry we find that the weak gravity conjecture then does follow from positivity bounds. For a preserved O(d, d; ℝ) symmetry we find a simple condition on the two Wilson coefficients which ensures the positivity of corrections to the charge-to-mass ratio and that follows from the null energy condition alone. We find that imposing supersymmetry on top of either of these symmetries gives corrections which vanish identically, as expected for BPS states.

THOUGHTS ON THE AREA THEOREM

2009 ◽  
Vol 24 (16n17) ◽  
pp. 3111-3135 ◽  
Author(s):  
MU-IN PARK
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Three Dimensional ◽  
Kerr Black Hole ◽  
Second Law Of Thermodynamics ◽  
Positive Energy ◽  
Btz Black Hole ◽  
Area Theorem ◽  
Four Dimensions ◽  
Higher Derivative

Hawking's area theorem can be understood from a quasistationary process in which a black hole accretes positive energy matter, independent of the details of the gravity action. I use this process to study the dynamics of the inner as well as the outer horizons for various black holes which include the recently discovered exotic black holes and three-dimensional black holes in higher derivative gravities as well as the usual Banados–Teitelboim–Zanelli (BTZ) black hole and the Kerr black hole in four dimensions. I find that the area for the inner horizon "can decrease," rather than increase, with the quasistationary process. However, I find that the area for the outer horizon "never decrease" such as the usual area theorem still works in our examples, though this is quite nontrivial in general. I also find that the recently proposed new entropy formulae for the above mentioned, recently discovered black holes satisfy the second law of thermodynamics.

scholarly journals Effect of the inner horizon on the black hole thermodynamics: Reissner–Nordström black hole and Kerr black hole

2021 ◽  
pp. 2150177
Author(s):  
G. E. Volovik
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Radiation ◽  
Kerr Black Hole ◽  
Black Hole Thermodynamics ◽  
Spherically Symmetric ◽  
Schwarzschild Black Hole ◽  
Inner Horizon ◽  
Hole Charge

For the Schwarzschild black hole, the Bekenstein–Hawking entropy is proportional to the area of the event horizon. For the black holes with two horizons, the thermodynamics is not very clear, since the role of the inner horizons is not well established. Here we calculate the entropy of the Reissner–Nordström black hole and of the Kerr black hole, which have two horizons. For the spherically symmetric Reissner–Nordström black hole, we used several different approaches. All of them give the same result for the entropy and for the corresponding temperature of the thermal Hawking radiation. The entropy is not determined by the area of the outer horizon, and it is not equal to the sum of the entropies of two horizons. It is determined by the correlations between the two horizons, due to which the total entropy of the black hole and the temperature of Hawking radiation depend only on mass M of the black hole and do not depend on the black hole charge Q. For the Kerr and Kerr–Newman black holes, it is shown that their entropy has the similar property: it depends only on mass M of the black hole and does not depend on the angular momentum J and charge Q.

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