Explicit microstates at the Schwarzschild horizon

Giveon, Amit

doi:10.1007/jhep11(2021)001

Cited by 9 publications

(11 citation statements)

References 15 publications

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“…As originally suggested by Dabholkar [15], recent papers [16,17], argued that the winding condensate accounts for the entire Bekenstein-Hawking entropy of the black holes, specifically when taking into account the back reaction it induces [18]. However, the result seemed too good to be true for several reasons.…”

Section: Jhep10(2022)112mentioning

confidence: 99%

On the entropy of strings and branes

Brustein

Zigdon

2022

J. High Energ. Phys.

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We show that the entropy of strings that wind around the Euclidean time circle is proportional to the Noether charge associated with translations along the T-dual time direction. We consider an effective target-space field theory which includes a large class of terms in the action with various modes, interactions and α′ corrections. The entropy and the Noether charge are shown to depend only on the values of fields at the boundary of space. The classical entropy, which is proportional to the inverse of Newton’s constant, is then calculated by evaluating the appropriate boundary term for various geometries with and without a horizon. We verify, in our framework, that for higher-curvature pure gravity theories, the Wald entropy of static neutral black hole solutions is equal to the entropy derived from the Gibbons-Hawking boundary term. We then proceed to discuss horizonless geometries which contain, due to the back-reaction of the strings and branes, a second boundary in addition to the asymptotic boundary. Near this “punctured” boundary, the time-time component of the metric and the derivatives of its logarithm approach zero. Assuming that there are such non-singular solutions, we identify the entropy of the strings and branes in this geometry with the entropy of the solution to all orders in α′. If the asymptotic region of an α′-corrected neutral black hole is connected through the bulk to a puncture, then the black hole entropy is equal to the entropy of the strings and branes. Later, we discuss configurations similar to the charged black p-brane solutions of Horowitz and Strominger, with the second boundary, and show that, to leading order in the α′ expansion, the classical entropy of the strings and branes is equal exactly to the Bekenstein-Hawking entropy. This result is extended to a configuration that asymptotes to AdS.

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Section: Jhep10(2022)112mentioning

confidence: 99%

On the entropy of strings and branes

Brustein

Zigdon

2022

J. High Energ. Phys.

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“…Starting with the HP action in (d+1)-dimensions and taking a β derivative on the integrand before setting the fields on-shell implies that the entropy is given by [13,14,19,20]:…”

Section: Jhep04(2022)021 5 Winding Entropy and Black Hole Entropymentioning

confidence: 99%

“…It is widely accepted that χ plays a key role for small black holes near the Hagedorn temperature (see, e.g., [9][10][11][12][13][14]). It was also claimed that this stringy mode is crucial for a microscopic understanding of large black holes (see, e.g., [15][16][17][18][19][20]). To explore this systematically, one needs to know the details of χ(ρ) and its coupling to the background.…”

Section: Introductionmentioning

confidence: 99%

A puncture in the Euclidean black hole

Brustein

Giveon

Itzhaki

et al. 2022

J. High Energ. Phys.

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We consider the backreaction of the winding condensate on the cigar background. We focus on the case of the SL(2, ℝ)k/U(1) cigar associated with, e.g., the near-horizon limit of k NS5 black-branes. We solve the equations of motion numerically in the large k limit as a function of the amplitude, A, of the winding mode at infinity. We find that there is a critical amplitude, Ac = exp(−γ/2), that admits a critical solution. In string theory, the exact SL(2, ℝ)k/U(1) cigar CFT fixes completely the winding amplitude, As, at infinity. We find that in the large k limit there is an exact agreement, Ac = As. The critical solution is a cigar with a puncture at its tip; consequently, the black-hole entropy is carried entirely by the winding condensate. We argue that, in the Lorentzian case, the information escapes the black hole through this puncture.

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“…However, black holes are fascinating compact objects where the spacetime surrounded them is severely curved in such a way that an observer, being outside their event horizons, cannot observe anything inside the black hole event horizons. Therefore, the statistical origin of the black hole entropy is hidden from the rest of the universe, which leads to some important open questions on counting black hole microstates and calculating its corresponding entropy from the first principle [4][5][6][7][8][9][10][11].…”

Section: Introduction and Motivationsmentioning

confidence: 99%

Emergent Phase, Thermodynamic Geometry and Criticality of Charged Black Holes from Rényi Statistics

Hirunsirisawat¹,

Nakarachinda²,

Promsiri³

2022

Preprint

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Recently, a novel emergent phase can occur from thermodynamic consideration of the asymptotically flat Reissner-Nordström black hole (RN-AF) using Rényi statistics. We present an analysis of the thermodynamical and mechanical stabilities of the RN-AF in both the Gibbs-Boltzmann (GB) and the alternative Rényi statistics when charge q and electrostatic potential φ are treated as pressure and volume, respectively. Interestingly, the emergent phase of the RN-AF can be both thermodynamically and mechanically stable in some range of parameters in the framework of Rényi thermodynamics. With the construction of the Maxwell equal area law in q − φ plane, the coexistence line between the near-extremal black hole phase and the emergent phase can be found in some values of charge which can be associated as the vapor pressure at which the liquid and gas phases coexist. In the aspect of thermodynamic geometry, the microscopic interaction between the black hole microstructures can be repulsive in the Rényi description. This implies that a novel correlation between the microstates of a self-gravitating system could be emerged via the nonextensive nature of long-range interaction systems. Finally, we also investigate the critical phenomena of the RN-AF in Rényi statistics compared to that of the van der Waals (vdW) fluid and find that the critical exponents of the relevant physical quantities of both systems are identical. This implies that both systems are in the same universality class of the phase transition.

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Explicit microstates at the Schwarzschild horizon

Abstract: The claim that the microstates of Schwarzschild black holes in perturbative string theory amount to the modes of long folded strings in the vicinity of its horizon is supported by more evidence.

Cited by 9 publications

References 15 publications

On the entropy of strings and branes

On the entropy of strings and branes

A puncture in the Euclidean black hole

Emergent Phase, Thermodynamic Geometry and Criticality of Charged Black Holes from Rényi Statistics

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