Can we know about black hole thermodynamics through shadows?

Cai, X.; Miao, Yan-Gang

doi:10.48550/arxiv.2107.08352

Cited by 15 publications

(21 citation statements)

References 177 publications

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“…Following Ref. [22][23][24][25], the light ray send from a static observer at position r O transmits into the past with an angle β relative to the radial direction, that is…”

Section: The Shadow Of the Bardeen-ads Bhmentioning

confidence: 99%

“…By investigating the relations between the shadow and critical behavior of the charged AdS BH, Belhaj et al obtained the critical exponent that perfectly matched the vdW system [23]. Cai et al studied the relationship between shadow radius and microstructure of the charged AdS BH, founding that the shadow can provide the dynamic characteristics of BHs [24]. By constructing the connection between the shadow and Ruppeiner geometry, Wang et al believed the BH shadow can provide information about the small/large phase transition of the charged AdS BH and obtained the normalized curvature scalar at the critical point has a constant value of −3/2 [25].…”

Section: Introductionmentioning

confidence: 99%

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Shadow thermodynamics of AdS black hole in regular spacetime

Guo,

Li,

2022

Preprint

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The dependence of the black hole (BH) shadow and thermodynamics may be structured in the regular spacetime. Taking the regular Bardeen-AdS BH as an example, the relationship between the shadow radius and the event horizon radius is derived. It is found that these two radii display a positive correlation, implying that the BH temperature can be rewritten as a function of shadow radius in the regular spacetime. By analyzing the phase transition curves under the shadow context, we found that the shadow radius can replace the event horizon radius to present the BH phase transition process, and the phase transition grade can also be revealed by the shadow radius, indicating that the shadow radius may serve as a probe for the phase structure in the regular spacetime. Utilizing the temperature-shadow radius function, the thermal profile of the Bardeen-AdS BH is established. We obtained that the temperature shows an N-type change trend in P < P c situation. These results suggest that the phase transition process of the regular AdS BH can be completely presented in the thermal profile, and the relationship between the BH shadow and thermodynamics can also be established in the regular spacetime.

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“…Following Ref. [22][23][24][25], the light ray send from a static observer at position r O transmits into the past with an angle β relative to the radial direction, that is…”

Section: The Shadow Of the Bardeen-ads Bhmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Shadow thermodynamics of AdS black hole in regular spacetime

Guo,

Li,

2022

Preprint

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“…Motivated by the investigations on these spacetimes, interplays between the black hole thermodynamics and the optical properties have been established. It has been shown that the shadow size can provide information on the HP phase transitions, the critical behaviors and the microstructure states of the black holes living in AdS geometries [44][45][46]. And the relation between the shadow and the thermodynamics of the black hole has been also developed for regular space-times [47].…”

Section: Introductionmentioning

confidence: 99%

Shadow thermodynamics of non-linear charged Anti-de Sitter black holes

Du,

Li,

Zhou

et al. 2022

Preprint

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Non-linear interaction between the electromagnetic fields (EMF) are occurred when vacuum polarization in quantum electrodynamics (QED) happens. The field of non-linear electrodynamics which may be resulting from this interaction could have important effects on black hole physics. In this work, we investigate the relationship between the observable quantity, the shadow radius and the first-order phase transition for the non-linear charged AdS black hole in the frame of the Einstein-power-Yang-Mills (EPYM) gravity. Through the analysis, we find with a certain condition there exist the non-monotonic behaviors between the shadow radius, the horizon radius, and temperature (or pressure). And from the viewpoint of the shadow radius, the phase transition temperature is higher than that from the viewpoint of the horizon radius with the same condition. These indicate that the shadow radius can be regarded a probe to reveal the thermodynamic phase transition information of black holes. When the system is undergoing the phase transition in two cases of the different non-linear YM charge parameter values: γ = 1, 1.5, the thermal profiles of the coexistent big and small black hole phases with the temperature are presented. Furthermore, the effects of non-linear YM charge parameter on the shadow radius and the thermal profile are also investigated.

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“…In addition, we can define a "force" by taking the ratio F 2 := J 2 /S 2 , where J is the angular momentum and S the Bekenstein-Hawking entropy of the black hole. These two thermodynamical variables can be used to define the so-called Ruppeiner geometry [13] -a two-dimensional Riemannian metric in thermodynamic phase space -which has recently gained some attention in the context of black hole microstructure [14][15][16][17][18][19][20][21] and applications to black hole shadows [22][23][24]. Interestingly, the region in the thermodynamic phase space with positive Ruppeiner scalar curvature is marked by the boundary F 2 = 1 As pointed out by Emparan and Myers, at this point the temperature of the black hole starts to behave like a black brane instead of a Kerr-type black hole.…”

Section: Introduction: the Maximum Force Conjecture And Thermodynamicsmentioning

confidence: 99%

The Hookean Law of Black Holes and Fragmentation: Insights from Maximum Force Conjecture and Ruppeiner Geometry

Di Gennaro,

Good,

Ong

2021

Preprint

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We show that the notion of the maximum force conjecture F 1/4 in general relativity, when applied to asymptotically flat singly spinning Myer-Perry black holes in any dimension, reveals the underlying thermodynamic instability in a number of ways. In particular, the "Hookean force law" F1 = kx, suitably defined, is bounded by the conjectured limit, but in d 6 it is further bounded by a dimensional dependent value less than 1/4, which remarkably corresponds to the Emparan-Myers fragmentation (splitting of a black hole into two becomes thermodynamically preferable). Furthermore, we define another "force" as the square of the angular momentum to entropy ratio (F2 = J 2 /S 2 ). In dimensions d 6, the positive Ruppeiner scalar curvature region in the thermodynamic phase space is marked by the upper boundary F2 = 1 12 d−3 d−5 and the lower boundary F2 = 1 4 d−3 d−5, the latter corresponds to a black hole that suffers from Gregory-Laflamme instability. Surprisingly, the upper and lower boundaries correspond to F = 1/4 when d = 6 and d → ∞, respectively. We discuss how the maximum force may be relevant to the underlying black hole microstructure and its relationship to cosmic censorship.

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Can we know about black hole thermodynamics through shadows?

Cited by 15 publications

References 177 publications

Shadow thermodynamics of AdS black hole in regular spacetime

Shadow thermodynamics of AdS black hole in regular spacetime

Shadow thermodynamics of non-linear charged Anti-de Sitter black holes

The Hookean Law of Black Holes and Fragmentation: Insights from Maximum Force Conjecture and Ruppeiner Geometry

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