scholarly journals BLACK HOLE AS AN INFORMATION ERASER

2010 ◽  
Vol 25 (19) ◽  
pp. 1581-1594 ◽  
Author(s):  
HYEONG-CHAN KIM ◽  
JAE-WEON LEE ◽  
JUNGJAI LEE
Keyword(s):  
Black Hole ◽  
Mass Spectra ◽  
Black Hole Entropy ◽  
Black Hole Thermodynamics ◽  
Black Hole Mass ◽  
Schwarzschild Black Hole ◽  
Efficient Information ◽  
Landauer’S Principle ◽  
Discrete Mass

We discuss the identity of black hole entropy and show that the first law of black hole thermodynamics, in the case of a Schwarzschild black hole, can be derived from Landauer's principle by assuming that the black hole is one of the most efficient information erasers. The term "most efficient" implies that maximal information will be erased for a given amount of work. We calculate the discrete mass spectra and the entropy of a Schwarzschild black hole assuming that the black hole processes information in unit of bits. The black hole entropy acquires a subleading contribution proportional to the logarithm of its mass-squared in addition to the usual mass-squared term without an artificial cutoff. We also argue that the minimum of the black hole mass is [Formula: see text]

scholarly journals Varying Newton Constant and Black Hole to White Hole Quantum Tunneling

2020 ◽  
Author(s):  
Grigory Volovik
Keyword(s):  
Black Hole ◽  
Quantum Tunneling ◽  
Black Hole Thermodynamics ◽  
Black Hole Mass ◽  
Schwarzschild Black Hole ◽  
Dimensionless Quantity ◽  
White Hole ◽  
Thermodynamic Variable ◽  
Euclidean Action ◽  
Thermodynamics Of Black Holes

The thermodynamics of black holes is discussed for the case, when the Newton constant G is not a constant, but is the thermodynamic variable. This gives for the first law of the Schwarzschild black hole thermodynamics: d S BH = − A d K + d M T BH , where the gravitational coupling K = 1 / 4 G , M is the black hole mass, A is the area of horizon, and T BH is Hawking temperature. From this first law it follows that the dimensionless quantity M 2 / K is the adiabatic invariant, which in principle can be quantized if to follow the Bekenstein conjecture. From the Euclidean action for the black hole it follows that K and A serve as dynamically conjugate variables. This allows us to calculate the quantum tunneling from the black hole to the white hole, and determine the temperature and entropy of the white hole.

scholarly journals Varying Newton Constant and Black Hole to White Hole Quantum Tunneling

Universe ◽  
2020 ◽  
Vol 6 (9) ◽  
pp. 133
Author(s):  
Grigory Volovik
Keyword(s):  
Black Hole ◽  
Quantum Tunneling ◽  
Condensed Matter ◽  
Black Hole Thermodynamics ◽  
Black Hole Mass ◽  
Schwarzschild Black Hole ◽  
Dimensionless Quantity ◽  
White Hole ◽  
Euclidean Action ◽  
Thermodynamics Of Black Holes

The thermodynamics of black holes is discussed for the case, when the Newton constant G is not a constant, but it is the thermodynamic variable. This gives for the first law of the Schwarzschild black hole thermodynamics: dSBH=−AdK+dMTBH, where the gravitational coupling K=1/4G, M is the black hole mass, A is the area of horizon, and TBH is Hawking temperature. From this first law, it follows that the dimensionless quantity M2/K is the adiabatic invariant, which, in principle, can be quantized if to follow the Bekenstein conjecture. From the Euclidean action for the black hole it follows that K and A serve as dynamically conjugate variables. Using the Painleve–Gullstrand metric, which in condensed matter is known as acoustic metric, we calculate the quantum tunneling from the black hole to the white hole. The obtained tunneling exponent suggests that the temperature and entropy of the white hole are negative.

scholarly journals BEKENSTEIN-SPECTRUM, TEMPERATURE AND SPECIFIC HEAT OF BLACK HOLES FROM CHAINS

2005 ◽  
Vol 20 (13) ◽  
pp. 2813-2820 ◽  
Author(s):  
AXEL KRAUSE
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Mass Spectrum ◽  
Specific Heat ◽  
Hawking Temperature ◽  
Evaporation Process ◽  
Black Hole Mass ◽  
Schwarzschild Black Hole ◽  
Discrete Mass

We study some consequences of a recently proposed description for a Schwarzschild black hole based on Euclidean [Formula: see text] brane pairs described in terms of chain-like excitations. A discrete mass-spectrum of Bekenstein-type is inferred and upon identification of the black hole mass with the chain's energy the leading corrections to both Hawking-temperature and specific heat of the black hole are obtained. The results indicate that for small black holes the evaporation process might be considerably altered.

THE BLACK HOLE ENTROPY BOUND AND THE MAXIMUM TEMPERATURE FOR MESON FORMATION IN THE NUCLEAR FIREBALL

1991 ◽  
Vol 06 (33) ◽  
pp. 3039-3045 ◽  
Author(s):  
JISHNU DEY ◽  
MIRA DEY ◽  
MARCELO SCHIFFER ◽  
LAURO TOMIO
Keyword(s):  
Black Hole ◽  
Simple Model ◽  
Black Hole Entropy ◽  
Heavy Ion ◽  
Black Hole Thermodynamics ◽  
Maximum Temperature ◽  
Ion Collisions ◽  
Pion Interferometry ◽  
Entropy Bound ◽  
Confined System

The entropy bound from black hole thermodynamics can be invoked to set limits for temperatures at which hadrons can survive as a confined system. We find that this implies that the pion can be formed in heavy ion collisions, much later than heavier mesons, for example the ρ-meson, when the fireball is cooler. The temperature found in a simple model agree qualitatively with experiment. We also suggest that this may be the reason why in pion interferometry experiments the space-time volume of the pion source seems large.

scholarly journals ENTROPY AND AREA IN LOOP QUANTUM GRAVITY

2005 ◽  
Vol 14 (12) ◽  
pp. 2301-2305
Author(s):  
JOHN SWAIN
Keyword(s):  
Black Hole ◽  
Quantum Gravity ◽  
Maximum Entropy ◽  
Degrees Of Freedom ◽  
Loop Quantum Gravity ◽  
Black Hole Entropy ◽  
Black Hole Thermodynamics ◽  
Three Dimensions ◽  
Spin Network

Black hole thermodynamics suggests that the maximum entropy that can be contained in a region of space is proportional to the area enclosing it rather than its volume. We argue that this follows naturally from loop quantum gravity and a result of Kolmogorov and Bardzin' on the the realizability of networks in three dimensions. This represents an alternative to other approaches in which some sort of correlation between field configurations helps limit the degrees of freedom within a region. It also provides an approach to thinking about black hole entropy in terms of states inside rather than on its surface. Intuitively, a spin network complicated enough to imbue a region with volume only lets that volume grow as quickly as the area bounding it.

scholarly journals Prospecting black hole thermodynamics with fractional quantum mechanics

2021 ◽  
Vol 81 (7) ◽  
Author(s):  
S. Jalalzadeh ◽  
F. Rodrigues da Silva ◽  
P. V. Moniz
Keyword(s):  
Black Hole ◽  
Quantum Mechanics ◽  
Main Tool ◽  
Acta Math ◽  
Black Hole Thermodynamics ◽  
Point Of View ◽  
Black Hole Mass ◽  
Fractional Quantum ◽  
C 73 ◽  
Fractional Parameter

AbstractThis paper investigates whether the framework of fractional quantum mechanics can broaden our perspective of black hole thermodynamics. Concretely, we employ a space-fractional derivative (Riesz in Acta Math 81:1, 1949) as our main tool. Moreover, we restrict our analysis to the case of a Schwarzschild configuration. From a subsequently modified Wheeler–DeWitt equation, we retrieve the corresponding expressions for specific observables. Namely, the black hole mass spectrum, M, its temperature T, and entropy, S. We find that these bear consequential alterations conveyed through a fractional parameter, $$\alpha $$ α . In particular, the standard results are recovered in the specific limit $$\alpha =2$$ α = 2 . Furthermore, we elaborate how generalizations of the entropy-area relation suggested by Tsallis and Cirto (Eur Phys J C 73:2487, 2013) and Barrow (Phys Lett B 808:135643, 2020) acquire a complementary interpretation in terms of a fractional point of view. A thorough discussion of our results is presented.

scholarly journals BLACK HOLE THERMODYNAMICS AND MODIFIED GUP CONSISTENT WITH DOUBLY SPECIAL RELATIVITY

2012 ◽  
Vol 27 (39) ◽  
pp. 1250227 ◽  
Author(s):  
K. ZEYNALI ◽  
F. DARABI ◽  
H. MOTAVALLI
Keyword(s):  
Heat Capacity ◽  
Black Hole ◽  
Special Relativity ◽  
Uncertainty Principle ◽  
Generalized Uncertainty Principle ◽  
Black Hole Thermodynamics ◽  
Schwarzschild Black Hole ◽  
Commutation Relations ◽  
Doubly Special Relativity ◽  
Correction Terms

We study the black hole thermodynamics and obtain the correction terms for temperature, entropy, and heat capacity of the Schwarzschild black hole, resulting from the commutation relations in the framework of Modified Generalized Uncertainty Principle suggested by Doubly Special Relativity.

DE SITTER-SCHWARZSCHILD BLACK HOLE: ITS PARTICLELIKE CORE AND THERMODYNAMICAL PROPERTIES

1996 ◽  
Vol 05 (05) ◽  
pp. 529-540 ◽  
Author(s):  
I.G. DYMNIKOVA
Keyword(s):  
Black Hole ◽  
Lower Limit ◽  
Mass Parameter ◽  
Hawking Temperature ◽  
Einstein Equations ◽  
Black Hole Mass ◽  
De Sitter ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Solution ◽  
Second Order Phase Transition

We analyze the globally regular solution of the Einstein equations describing a black hole whose singularity is replaced by the de Sitter core. The de Sitter—Schwarzschild black hole (SSBH) has two horizons. Inside of it there exists a particlelike structure hidden under the external horizon. The critical value of mass parameter M cr1 exists corresponding to the degenerate horizon. It represents the lower limit for a black-hole mass. Below M cr1 there is no black hole, and the de Sitter-Schwarzschild solution describes a recovered particlelike structure. We calculate the Hawking temperature of SSBH and show that specific heat is broken and changes its sign at the value of mass M cr 2>M cr 1 which means that a second-order phase transition occurs at that point. We show that the Hawking temperature drops to zero when a mass approaches the lower limit M cr1 .

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