In this talk, we focus on the corrections to Bekenstein-Hawking entropy by associating it with the entanglement between degrees of freedom inside and outside the horizon. Using numerical techniques, we show that the corrections proportional to fractional power of area result when the field is in a superposition of ground and excited states. We explain this result by identifying that the degrees of freedom contributing to such corrections are different from those contributing to Bekenstein-Hawking entropy.
In this paper, we successfully derive the Bekenstein-Hawking entropy for Schwarzschild black holes in various dimensions by using a non-trivial phase space. It is appealing to notice that the thermodynamics of a Schwarzschild black hole actually behaves like that of a $1$-dimensional quantum mechanical system. Our result suggests that black hole should be viewed as a system with the equation of state $P=ρ$, and it also suggests that a holographic stage should exist in the early universe.
This paper comprehensively explores Stephen Hawking's interaction with Jacob Bekenstein. Both Hawking and Bekenstein benefited from the interaction with each other. It is shown that Hawking's interaction with Bekenstein drove him to solve the problems in Bekenstein's black hole thermodynamics in terms of a new thermal radiation mechanism. Hawking derived the thermal radiation using a semiclassical approximation in which the matter fields are treated quantum mechanically on a classical spacetime background. Hawking's semiclassical approximation yielded a simple formula for the entropy of the bl…
Leading Log Corrections to Bekenstein-Hawking Entropy
我们表明，与任何黑洞相关的贝肯斯坦-霍金熵进行对数修正时，小的热力学波动平衡考虑在内。因此，黑洞熵的校正表达式由$S= A/4 - k \ln(A)$给出，其中$A$是视界面积，$k$是取决于特定黑洞的常数。我们把我们的结果应用到BTZ黑洞，其中$k=3/2$，如前所述，以及反德西特-史瓦西和Reissner-Nordstrom黑洞在任意时空维。最后，我们考察了共形场论在黑洞熵及其修正中的作用。
Black hole entropy is a robust prediction of quantum gravity with no established phenomenological consequences to date. We use the Bekenstein-Hawking entropy formula and general-relativistic statistical mechanics to determine the probability distribution of random geometries uniformly sampled in phase space. We show that this statistics (in the limit $\hbar\to 0$) is relevant to large curvature perturbations, resulting in a population of primordial black holes with zero natal spin. In principle, the identification of such a population at LIGO, Virgo, and future gravitational wave observatories…
In this paper, we derive the Bekenstein-Hawking entropy by considering a Non-Commuting two dimensional quantized space, and we will show that the Bekenstein-Hawking entropy is valid for the system (black hole) in an equilibrium state. Also, by using the entropy was obtained, we derive the Einstein and Newton gravity equation, and finally, we get an equation that is consistent with the previous results. In other words, we want to show that by using the statistical mechanics and quantization of space and the excitation of space quanta, can be obtained the Einstein and Newton gravity equation. In…
Black holes and bits: A simple path to Bekenstein-Hawking entropy
Facultad de Ciencias Básicas, Departamento de Física（基础科学学院物理系）；Centro de Desarrollo de Investigación CEDI-UMCE（CEDI-UMCE研究发展中心）；Universidad Metropolitana de Ciencias de la Educación（教育科学都会大学）
The black-hole information puzzle has attracted much attention over the years from both physicists and mathematicians. One of the most intriguing suggestions to resolve the information paradox is due to Bekenstein, who has stressed the fact that the low-energy part of the semi-classical black-hole emission spectrum is partly blocked by the curvature potential that surrounds the black hole. As explicitly shown by Bekenstein, this fact implies that the grey-body emission spectrum of a (3+1)-dimensional black hole is considerably less entropic than the corresponding radiation spectrum of a perfec…
Gravitational wave constraints on corrections to Bekenstein-Hawking Area Formula in classical F(R) gravity and quantum GR : implications for theory parameters
Indian Association for the Cultivation of Science（印度科学文化研究所）
Bekenstein-Hawking temperature from the Schwarzian
Istituto per le Applicazioni del Calcolo “M. Picone”, CNR（意大利国家研究委员会计算应用研究所）；Dipartimento di Fisica “Ettore Pancini”, Complesso Universitario di Monte S. Angelo（恩托雷·潘奇尼物理系）；Istituto Nazionale di Fisica Nucleare, Sezione di Napoli（意大利国家核物理研究所那不勒斯分部）
The Rényi and Tsallis entropies are discussed as possible alternatives to the Bekenstein-Hawking area-law entropy. It is pointed out how replacing the entropy notion, but not the Hawking temperature and the thermodynamical energy may render the whole black hole thermodynamics inconsistent. The possibility to relate the Rényi and Tsallis entropies with the quantum gravity corrected Bekenstein-Hawking entropy is discussed.
We introduce a new microscopic quantity $\varepsilon $ that describes the contribution of a single black hole molecule to black hole entropy and give a key relation that this microscopic quantity is proportional to the macroscopic quantity -- entropy surface density $σ_{S}$, thus connecting a microscopic quantity to a macroscopic quantity of black holes. Such a connection provides a new probe for understanding the black hole microstructure from the macroscopic perspective. We also classify black holes in terms of entropy surface density. When its entropy surface density is larger (smaller) tha…
Primordial spectra from modified Bekenstein-Hawking entropy law
Scuola Superiore Meridionale（南方高等学院）；INFN, Sezione di Napoli（意大利国家核物理研究所那不勒斯分部）；Dipartimento di Fisica “Ettore Pancini”, Università di Napoli “Federico II”（那不勒斯费德里科二世大学埃托雷·潘奇尼物理系）；Faculty of Physics, Ludwig-Maximilians-Universität（慕尼黑路德维希-马克西米利安大学物理学院）
