Reentrant phase transitions in Einstein-Maxwell-scalar black holes

Astefanesei, Dumitru; Cabrera, Paulina; Mann, Robert B.; Rojas, Raúl

doi:10.1103/physrevd.105.046021

“…In this paper we have derived a Smarr formula and a first law for the extended thermodynamics of the black-hole solutions of the theories described by the action equation (2.1) using Wald's formalism and the results of [13,45]. Our results coincide with those of [34] except for the inclusion of the term proportional to the scalar charge and the variation of the asymptotic value of the scalar. This term is somewhat mysterious since there are no asymptotically flat blackhole solutions for asymptotic values of the scalar other than zero, but it may make sense in a wider class of not asymptotically-flat solutions.…”

Section: Discussionmentioning

confidence: 57%

“…The mechanical stability of black holes with scalar hair has been studied in[31] while the thermodynamical stability has been studied in[32,33] 10. in[34] the extended thermodynamics of some of these solutions has been studied, but not from the point of view of their scalar charges.…”

mentioning

confidence: 99%

Hairy black holes, scalar charges and extended thermodynamics

Ballesteros,

Ortín

2024

Class. Quantum Grav.

3

0

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We explore the use of the recently deﬁned scalar charge which satisﬁes a Gauss law in stationary spacetimes, in the context of theories with a scalar potential. We ﬁnd new conditions that this potential has to satisfy in order to allow for static, asymptotically-ﬂat black-hole solutions with regular horizons and non-trivial scalar ﬁeld. These conditions are equivalent to some of the known “no-hair” theorems (such as Bekenstein’s). We study the extended thermodynamics of these systems, deriving a ﬁrst law and a Smarr formula. As an example, we study the Anabalón-Oliva hairy black hole.

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“…However, some differences exist, such as phase structures of Born-Infeld black holes [16][17][18]. For example, a large/small/large black hole reentrant phase transition [19][20][21] could be observed for Born-Infeld AdS black holes, while it can't occur for any Born-Infeld black hole in a cavity. Between black holes in a cavity and with the AdS boundary, the similarity or difference of phase structures may have interesting implications for black hole thermodynamics and holography [22].…”

Section: Introductionmentioning

confidence: 99%

Thermodynamics and Microstructures of Euler-Heisenberg Black Hole in a Cavity

Yu¹,

Xu²,

Teishima³

2023

Preprint

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The Euler-Heisenberg black holes with quantum electrodynamics (QED) correction are embraced by a cavity in this paper, which serves as a boundary of the black hole spacetime and contributes to the equilibrium of the system. We explore the thermodynamic properties of the black hole, including the phase transitions and phase structures. The small/large black hole phase transition occurs for a negative QED parameter, while the reentrant phase transition can be observed for a small positive QED parameter. Then the thermodynamic geometry is investigated to diagnose microscopic interactions of black hole thermodynamic systems. For the reentrant phase transition, the small black holes are dominated by repulsion for the first-order coexistence curve, while the interaction between the small black hole molecules could be attractive or repulsive for the small/large black hole phase transition.

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“…However, some differences exist, such as phase structures of Born-Infeld black holes [16][17][18]. For example, a large/small/large black hole reentrant phase transition [19][20][21] could be observed for Born-Infeld-AdS black holes, while it can not occur for any Born-Infeld black hole in a cavity. For black holes in a cavity and with the AdS boundary, the similarity or difference of phase structures may have interesting implications for black hole thermodynamics and holography [22].…”

Section: Introductionmentioning

confidence: 99%

Thermodynamics and microstructures of Euler–Heisenberg black hole in a cavity

Yu

¹

,

Xu

²

,

Tao

³

2023

Commun. Theor. Phys.

2

0

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The Euler-Heisenberg black holes with quantum electrodynamics (QED) correction are embraced by a cavity in this paper, which serves as a boundary of the black hole spacetime and contributes to the equilibrium of the system. We explore the thermodynamic properties of the black hole, including the phase transitions and phase structures. The small/large black hole phase transition occurs for a negative QED parameter, while the reentrant phase transition can be observed for a small positive QED parameter. Then the thermodynamic geometry is investigated to diagnose microscopic interactions of black hole thermodynamic systems. For the reentrant phase transition, the small black holes are dominated by repulsion for the first-order coexistence curve, while the interaction between the small black hole molecules could be attractive or repulsive for the small/large black hole phase transition.

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Reentrant phase transitions in Einstein-Maxwell-scalar black holes

Cited by 10 publications

References 42 publications

Hairy black holes, scalar charges and extended thermodynamics

Hairy black holes, scalar charges and extended thermodynamics

Thermodynamics and Microstructures of Euler-Heisenberg Black Hole in a Cavity

Thermodynamics and microstructures of Euler–Heisenberg black hole in a cavity

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