Black holes and Boyle's law — The thermodynamics of the cosmological constant

Dolan, Brian P.

doi:10.1142/s0217732315400027

Cited by 75 publications

(59 citation statements)

References 200 publications

(255 reference statements)

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“…Using now ∞ 0 dp p −1±ix = 2π δ(x), |Γ(1 + ix)| 2 = πx sinh πx (28) and recalling C 0 is negative and real it is easy to show that…”

Section: The Bogoliubov Coefficients and The Particle Spectramentioning

confidence: 99%

Particle creation by de Sitter black holes revisited

Bhattacharya

2018

Phys. Rev. D

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Creation of thermal distribution of particles by a black hole is independent of the detail of gravitational collapse, making the construction of the eternal horizons suffice to address the problem in asymptotically flat spacetimes. For eternal de Sitter black holes however, earlier studies have shown the existence of both thermal and non-thermal particle creation, originating from the non-trivial causal structure of these spacetimes. Keeping this in mind we consider this problem in the context of a quasistationary gravitational collapse occurring in a (3 + 1)-dimensional eternal de Sitter, settling down to a Schwarzschild-or Kerr-de Sitter spacetime and consider a massless minimally coupled scalar field. There is a unique choice of physically meaningful 'in' vacuum here, defined with respect to the positive frequency cosmological Kruskal modes localised on the past cosmological horizon C − , at the onset of the collapse. We define our 'out' vacuum at a fixed radial coordinate 'close' to the future cosmological horizon, C + , with respect to positive frequency outgoing modes written in terms of the ordinary retarded null coordinate, u. We trace such modes back to C − along past directed null geodesics through the collapsing body. Some part of the wave will be reflected back without entering it due to the greybody effect. We show that these two kind of traced back modes yield the two temperature spectra and fluxes subject to the aforementioned 'in' vacuum. Since the coordinate u used in the 'out' modes is not well defined on a horizon, estimate on how 'close' we might be to C + is given by estimating backreaction. We argue no other reasonable choice of the 'out' vacuum would give rise to any thermal spectra. Our conclusions remain valid for all non-Nariai class black holes, irrespective of the relative sizes of the two horizons.

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“…Using now ∞ 0 dp p −1±ix = 2π δ(x), |Γ(1 + ix)| 2 = πx sinh πx (28) and recalling C 0 is negative and real it is easy to show that…”

Section: The Bogoliubov Coefficients and The Particle Spectramentioning

confidence: 99%

Particle creation by de Sitter black holes revisited

Bhattacharya

2018

Phys. Rev. D

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“…However, in our analysis we will consider an extended phase space. According to the first law of black hole thermodynamics and the interpretation of M (total mass of black hole) [21,56] as H (the black hole enthalpy) [56,57], the Gibbs free energy of the black hole can be written as…”

Section: Phase Equilibrium and Maxwell's Equal Area Lawmentioning

confidence: 99%

Q– $$\Phi $$ Φ criticality in the extended phase space of $$(n+1)$$ ( n + 1 ) -dimensional RN-AdS black holes

Zhao

Cao

2016

Eur. Phys. J. C

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In order to achieve a deeper understanding of gravity theories, i.e., the quantum properties of gravity theories and the statistical explanation of gravitational entropy, it is important to further investigate the thermodynamic properties of a black hole at the critical point, besides the phase transition and critical behaviors. In this paper, by using Maxwell's equal area law, we choose T, Q, as the state parameters and study the phase equilibrium problem of a general (n + 1)-dimensional RN-AdS black holes thermodynamic system. The boundary of the two-phase coexistence region and its isotherm and isopotential lines are presented, which may provide a theoretical foundation for studying the phase transition and phase structure of black hole systems.

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“…However, an identification between RN-AdS black hole and Van der Waals system was recently realized in [13], where the negative cosmological constant plays the role as pressure, while its conjugate acts as thermodynamic volume of the black hole in the so-called extended phase space [14,15] (for a recent review, see [16]). Recently, thermodynamics and phase transition in the extended phase space for black holes in AdS space have been extensively studied in the literature (for an incomplete list see .…”

Section: Jhep02(2015)143mentioning

confidence: 99%

Phase transition and thermodynamical geometry for Schwarzschild AdS black hole in AdS5 × S5 spacetime

Zhang

Cai

2015

J. High Energ. Phys.

112

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Abstract:We study the thermodynamics and thermodynamic geometry of a five-dimensional Schwarzschild AdS black hole in AdS 5 × S 5 spacetime by treating the cosmological constant as the number of colors in the boundary gauge theory and its conjugate quantity as the associated chemical potential. It is found that the chemical potential is always negative in the stable branch of black hole thermodynamics and it has a chance to be positive, but appears in the unstable branch. We calculate the scalar curvatures of the thermodynamical Weinhold metric, Ruppeiner metric and Quevedo metric, respectively and we find that the scalar curvature in the Weinhold metric is always vanishing, while in the Ruppeiner metric the divergence of the scalar curvature is related to the divergence of the heat capacity with fixed chemical potential, and in the Quevedo metric the divergence of the scalar curvature is related to the divergence of the heat capacity with fixed number of colors and to the vanishing of the heat capacity with fixed chemical potential.

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Black holes and Boyle's law — The thermodynamics of the cosmological constant

Cited by 75 publications

References 200 publications

Particle creation by de Sitter black holes revisited

Particle creation by de Sitter black holes revisited

Q– $$\Phi $$ Φ criticality in the extended phase space of $$(n+1)$$ ( n + 1 ) -dimensional RN-AdS black holes

Phase transition and thermodynamical geometry for Schwarzschild AdS black hole in AdS5 × S5 spacetime

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