Entropy of thin shells in a (<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mn>2</mml:mn><mml:mo>+</mml:mo><mml:mn>1</mml:mn></mml:mrow></mml:math>)-dimensional asymptotically AdS spacetime and the BTZ black hole limit

Lemos, José P. S.; Quinta, Gonçalo M.

doi:10.1103/physrevd.89.084051

Cited by 20 publications

(28 citation statements)

References 28 publications

(62 reference statements)

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“…It is surely interesting to see if the thermodynamic properties for black holes and self-gravitating matter are reproduced in dimensions different from four and in spacetimes with a cosmological constant. In three dimensions, thermodynamic properties of thin shells in BTZ non-rotating and rotating spacetimes have been studied [22][23][24][25] with results that, even in one lower dimension and with the inclusion of a cosmological constant and rotation, somehow repeat the four-dimensional results, confirming that the BTZ spacetime is a good bed test for four-dimensional general relativity. On the other hand, the study of higher d-dimensional self-gravitating shells has not been performed.…”

Section: Introductionmentioning

confidence: 71%

“…(19), both the shell's rest mass M and pressure p go to zero, as one can check in Eqs. (21) and (22). Because k → 1, the temperature is T = 1/b and its behavior at the large d limit depends on the sign of the equation of state exponent a, as can be seen in Eq.…”

Section: Entropy Of the Shell For Large Dmentioning

confidence: 99%

“…(65), p + is the redshifted pressure p + = pk with p given in Eq. (22), and A + the horizon area given in Eq. (10).…”

Section: Smarr Relationmentioning

confidence: 99%

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Thermodynamics and entropy of self-gravitating matter shells and black holes in d dimensions

2019

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The thermodynamic properties of self-gravitating spherical thin matter shells an black holes in d > 4 dimensions are studied, extending previous analysis for d = 4. The shell joins a Minkowski interior to a Tangherlini exterior, i.e., a Schwarzschild exterior in d dimensions, with d 4, The junction conditions alone together with the first law of thermodynamics enable one to establish that the entropy of the thin shell depends only on its own gravitational radius. Endowing the shell with a well-defined power-law temperature equation of state allows to establish a precise form for the entropy and to perform a thermodynamic stability analysis for the shell. A particularly interesting case is when the shell's temperature has the Hawking form, i.e., it is inversely proportional to the shell's gravitational radius. It is shown in this case that the shell's heat capacity is positive, and thus the shell is stable, for shells with radii in-between their own gravitational radius and the photonic radius, i.e., the radius of circular photon orbits, reproducing unexpectedly York's thermodynamic stability criterion for a d = 4 black hole in the canonical ensemble. Additionally, the Euler equation for the matter shell is derived, the Bekenstein and holographic entropy bounds are studied, and the large d limit is analyzed. Within this formalism the thermodynamic properties of black holes can be studied too. Putting the shell at its own gravitational radius, i.e., in the black hole situation, obliges one to choose precisely the Hawking temperature for the shell which in turn yields a black hole with the Bekenstein-Hawking entropy. The stability analysis implies that the black hole is thermodynamically stable substantiating that in this configuration our system and York's canonical ensemble black hole are indeed the same system. Also relevant is the derivation in a surprising way of the Smarr formula for black holes in d dimensions.

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Section: Introductionmentioning

confidence: 71%

Section: Entropy Of the Shell For Large Dmentioning

confidence: 99%

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Thermodynamics and entropy of self-gravitating matter shells and black holes in d dimensions

2019

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“…Indeed, thin shells, besides giving instances of static and dynamic spacetimes, allow themselves to be scrutinized in relation to their entropic and thermodynamic matter and gravitational properties, and even from those properties to pick up the corresponding black hole properties. For static and rotating circularly symmetric thin shells, i.e., thin rings, in (2+1)-dimensional Bañados-Teitelbom-Zanelli (BTZ) spacetimes their entropic and thermodynamic properties have been worked out in general and in the limit where the ring is taken to its own gravitational, or horizon, radius, i.e., in the black hole limit [1][2][3][4]. For static electric charged spherically symmetric thin shells in (3+1)-dimensional Reissner-Nordström spacetimes these properties have also been worked out in detail in general and in the black hole limit [5][6][7], see also [8] for neutral thin shells in Schwarzschild spacetimes.…”

Section: Introductionmentioning

confidence: 99%

“…Related studies, where the entropy of black holes can be studied through systems with matter, involve quasiblack holes for which matter is spread over a 3-dimensional spatial region rather than on a 2-dimensional thin shell [9,10], or are connected to a quasistatic collapse of matter [11]. These works [1][2][3][4][5][6][7][8][9][10][11] stem from the fact that the concept of entropy is originally based on quantum properties of matter, and so it is very important to study whether and how black hole thermodynamics could emerge from thermodynamics of collapsing matter, when matter is compressed within its own gravitational radius. Conversely, it is through black hole entropy that we can grasp the microscopic aspects of a spacetime and hence of quantum gravity, and the fact that thermodynamics of a thin shell reflects thermodynamic properties of a black hole formed after quasistatic collapse of the shell indicates some connection between matter and gravitational degrees of freedom.…”

Section: Introductionmentioning

confidence: 99%

Unified approach to the entropy of an extremal rotating BTZ black hole: Thin shells and horizon limits

2017

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Using a thin shell, the first law of thermodynamics, and a unified approach, we study the thermodymanics and find the entropy of a (2+1)-dimensional extremal rotating Bañados-TeitelbomZanelli (BTZ) black hole. The shell in (2+1) dimensions, i.e., a ring, is taken to be circularly symmetric and rotating, with the inner region being a ground state of the anti-de Sitter (AdS) spacetime and the outer region being the rotating BTZ spacetime. The extremal BTZ rotating black hole can be obtained in three different ways depending on the way the shell approaches its own gravitational or horizon radius. These ways are explicitly worked out. The resulting three cases give that the BTZ black hole entropy is either the Bekenstein-Hawking entropy, S =, or it is an arbitrary function of A+, S = S(A+), where A+ = 2πr+ is the area, i.e., the perimeter, of the event horizon in (2+1) dimensions. We speculate that the entropy of an extremal black hole should obey 0 ≤ S(A+) ≤. We also show that the contributions from the various thermodynamic quantities, namely, the mass, the circular velocity, and the temperature, for the entropy in all three cases are distinct. This study complements the previous studies in thin shell thermodynamics and entropy for BTZ black holes. It also corroborates the results found for a (3+1)-dimensional extremal electrically charged Reissner-Nordström black hole.

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Information recovery from pure state geometries in 3D

Hulík

Raeymaekers

Vasilakis

2020

J. High Energ. Phys.

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It is a well-studied phenomenon in AdS 3 /CFT 2 that pure states often appear 'too thermal' in the classical gravity limit, leading to a version of the information puzzle. One example is the case of a heavy scalar primary state, whose associated classical geometry is the BTZ black hole. Another example is provided by a heavy left-moving primary, which displays late time decay in chiral correlators. In this paper we study a special class of pure state geometries which do not display such information loss. They describe heavy CFT states created by a collection of chiral operators at various positions on the complex plane. In the bulk, these take the form of multi-centered solutions from the backreaction of a collection of spinning particles, which we construct for circular distributions of particles. We compute the two-point function of probe operators in these backgrounds and show that information is retrieved. We observe that the states for which our geometric picture is reliable are highly extended star-like objects in the bulk description. This may point to limitations of semiclassical microstate geometries for understanding the information puzzle and to the need for including quantum effects.

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Entropy of thin shells in a (2+1)-dimensional asymptotically AdS spacetime and the BTZ black hole limit

Cited by 20 publications

References 28 publications

Thermodynamics and entropy of self-gravitating matter shells and black holes in d dimensions

Thermodynamics and entropy of self-gravitating matter shells and black holes in d dimensions

Unified approach to the entropy of an extremal rotating BTZ black hole: Thin shells and horizon limits

Information recovery from pure state geometries in 3D

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