Corrected form of the first law of thermodynamics for regular black holes

Ma, Meng-Sen; Zhao, Ren

doi:10.1088/0264-9381/31/24/245014

Cited by 90 publications

(67 citation statements)

References 46 publications

(90 reference statements)

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“…where M and S are the total energy and entropy of the system, respectively, and T f is the black hole temperature provided by the first law. According to [27], assuming the area law (S = A/4 = πr 2 + ) and M = M 0 , the first law does not provide a correct form for RBHs temperature. Explicitly, Eq.…”

Section: A Temperaturementioning

confidence: 99%

“…According to [27], a corrected first law is necessary to produce coherent values for the temperature and entropy for RBHs. We adopt the corrected first law proposed by the authors in [27] to evaluate the temperature of a class of RBHs in agreement with a first law that incorporates the so-called Bekenstein-Hawking area law [28], which provides a simple relation between both the entropy S and event horizon area A: S = A/4. Then, with the evaluated temperature, according to thermodynamics, the entropy and heat capacity are obtained.…”

Section: Introductionmentioning

confidence: 99%

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Thermodynamics of a class of regular black holes with a generalized uncertainty principle

Maluf

Neves

2018

Phys. Rev. D

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In this article, we present a study on thermodynamics of a class of regular black holes. Such a class includes Bardeen and Hayward regular black holes. We obtained thermodynamic quantities like the Hawking temperature, entropy, and heat capacity for the entire class. As part of an effort to indicate some physical observable to distinguish regular black holes from singular black holes, we suggest that regular black holes are colder than singular black holes. Besides, contrary to the Schwarzschild black hole, that class of regular black holes may be thermodynamically stable. From a generalized uncertainty principle, we also obtained the quantum-corrected thermodynamics for the studied class. Such quantum corrections provide a logarithmic term for the quantum-corrected entropy.

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Section: A Temperaturementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Thermodynamics of a class of regular black holes with a generalized uncertainty principle

Maluf

Neves

2018

Phys. Rev. D

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“…This result is what we expect. After all, the first law, Smarr formula and the Komar charge may be violated for some regular black holes in (3 + 1)-dimensional spacetime [44][45][46][47]. In fact, the two (2 + 1)-dimensional regular black holes also violate the Smarr formula.…”

Section: Thermodynamics Of the Regular Black Holesmentioning

confidence: 99%

(2 + 1)-dimensional regular black holes with nonlinear electrodynamics sources

2017

Physics Letters B

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On the basis of two requirements: the avoidance of the curvature singularity and the Maxwell theory as the weak field limit of the nonlinear electrodynamics, we find two restricted conditions on the metric function of (2 + 1)-dimensional regular black hole in general relativity coupled with nonlinear electrodynamics sources. By the use of the two conditions, we obtain a general approach to construct (2 + 1)-dimensional regular black holes. In this manner, we construct four (2+1)-dimensional regular black holes as examples. We also study the thermodynamic properties of the regular black holes and verify the first law of black hole thermodynamics.

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“…Identifying a black hole mass M with the thermodynamical energy leads also to appearance of inconsistency between the first law of black hole thermodynamics and relation of the black hole entropy with the Bekenstein-Hawking area law ( [53,55] and references therein).…”

Section: Introductionmentioning

confidence: 99%

Generic Features of Thermodynamics of Horizons in Regular Spherical Space-Times of the Kerr-Schild Class

Dymnikova

2018

Universe

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Abstract:We present a systematic review of thermodynamics of horizons in regular spherically symmetric spacetimes of the Kerr-Schild class, ds 2 = g(r)dt 2 − g −1 (r)dr 2 − r 2 dΩ 2 , both asymptotically flat and with a positive background cosmological constant λ. Regular solutions of this class have obligatory de Sitter center. A source term in the Einstein equations satisfies T t t = T r r and represents an anisotropic vacuum dark fluid (p r = −ρ), defined by the algebraic structure of its stress-energy tensor, which describes a time-evolving and spatially inhomogeneous, distributed or clustering, vacuum dark energy intrinsically related to space-time symmetry. In the case of two vacuum scales it connects smoothly two de Sitter vacua, 8πGTIn the range of the mass parameter M cr1 ≤ M ≤ M cr2 it describes a regular cosmological black hole directly related to a vacuum dark energy. Space-time has at most three horizons: a cosmological horizon r c , a black hole horizon r b < r c , and an internal horizon r a < r b , which is the cosmological horizon for an observer in the internal R-region asymptotically de Sitter as r → 0. Asymptotically flat regular black holes (λ = 0) can have at most two horizons, r b and r a . We present the basic generic features of thermodynamics of horizons revealed with using the Padmanabhan approach relevant for a multi-horizon space-time with a non-zero pressure. Quantum evaporation of a regular black hole involves a phase transition in which the specific heat capacity is broken and changes sign while a temperature achieves its maximal value, and leaves behind the thermodynamically stable double-horizon (r a = r b ) remnant with zero temperature and positive specific heat. The mass of objects with the de Sitter center is generically related to vacuum dark energy and to breaking of space-time symmetry. In the cosmological context space-time symmetry provides a mechanism for relaxing cosmological constant to a certain non-zero value. We discuss also observational applications of the presented results.

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Corrected form of the first law of thermodynamics for regular black holes

Cited by 90 publications

References 46 publications

Thermodynamics of a class of regular black holes with a generalized uncertainty principle

Thermodynamics of a class of regular black holes with a generalized uncertainty principle

(2 + 1)-dimensional regular black holes with nonlinear electrodynamics sources

Generic Features of Thermodynamics of Horizons in Regular Spherical Space-Times of the Kerr-Schild Class

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