scholarly journals Area law for black hole entropy in the SU(2) quantum geometry approach

2012 ◽  
Vol 85 (10) ◽  
Author(s):  
P. Mitra
Keyword(s):  
Black Hole ◽  
Black Hole Entropy ◽  
Quantum Geometry ◽  
Area Law

scholarly journals Quantum geometry and microscopic black hole entropy

2006 ◽  
Vol 24 (1) ◽  
pp. 243-251 ◽  
Author(s):  
Alejandro Corichi ◽  
Jacobo Díaz-Polo ◽  
Enrique Fernández-Borja
Keyword(s):  
Black Hole ◽  
Black Hole Entropy ◽  
Quantum Geometry

scholarly journals Quantum geometry of isolated horizons and black hole entropy

2000 ◽  
Vol 4 (1) ◽  
pp. 1-94 ◽  
Author(s):  
Abhay Ashtekar ◽  
John C. Baez ◽  
Kirill Krasnov
Keyword(s):  
Black Hole ◽  
Black Hole Entropy ◽  
Quantum Geometry ◽  
Isolated Horizons

scholarly journals BOUND OF NONCOMMUTATIVITY PARAMETER BASED ON BLACK HOLE ENTROPY

2010 ◽  
Vol 25 (38) ◽  
pp. 3213-3218 ◽  
Author(s):  
WONTAE KIM ◽  
DAEHO LEE
Keyword(s):  
Black Hole ◽  
Gauge Group ◽  
Black Hole Entropy ◽  
Brick Wall ◽  
Statistical Entropy ◽  
Schwarzschild Black Hole ◽  
Cutoff Parameter ◽  
Entropy Satisfying ◽  
Area Law ◽  
Wall Method

We study the bound of the noncommutativity parameter in the noncommutative Schwarzschild black hole which is a solution of the noncommutative ISO(3, 1) Poincaré gauge group. The statistical entropy satisfying the area law in the brick wall method yields a cutoff relation which depends on the noncommutativity parameter. Requiring both the cutoff parameter and the noncommutativity parameter to be real, the noncommutativity parameter can be shown to be bounded as Θ > 8.4 × 10-2lp.

scholarly journals HOLOGRAPHY, GAUGE-GRAVITY CONNECTION AND BLACK HOLE ENTROPY

2009 ◽  
Vol 24 (18n19) ◽  
pp. 3414-3425 ◽  
Author(s):  
PARTHASARATHI MAJUMDAR
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Degrees Of Freedom ◽  
Black Hole Entropy ◽  
Cross Sectional ◽  
Gauge Gravity ◽  
Thermal Stability Of ◽  
Spacetime Fluctuations ◽  
Area Law ◽  
Quantum Spacetime

The issues of holography and possible links with gauge theories in spacetime physics is discussed, in an approach quite distinct from the more restricted AdS-CFT correspondence. A particular notion of holography in the context of black hole thermodynamics is derived (rather than conjectured) from rather elementary considerations, which also leads to a criterion of thermal stability of radiant black holes, without resorting to specific classical metrics. For black holes that obey this criterion, the canonical entropy is expressed in terms of the microcanonical entropy of an Isolated Horizon which is essentially a local generalization of the very global event horizon and is a null inner boundary of spacetime, with marginal outer trapping. It is argued why degrees of freedom on this horizon must be described by a topological gauge theory. Quantizing this boundary theory leads to the microcanonical entropy of the horizon expressed in terms of an infinite series asymptotic in the cross-sectional area, with the leading 'area-law' term followed by finite, unambiguously calculable corrections arising from quantum spacetime fluctuations.

scholarly journals Quantum Geometry and Black Hole Entropy

1998 ◽  
Vol 80 (5) ◽  
pp. 904-907 ◽  
Author(s):  
A. Ashtekar ◽  
J. Baez ◽  
A. Corichi ◽  
K. Krasnov
Keyword(s):  
Black Hole ◽  
Black Hole Entropy ◽  
Quantum Geometry

scholarly journals Non-minimal couplings, quantum geometry and black-hole entropy

2003 ◽  
Vol 20 (20) ◽  
pp. 4473-4484 ◽  
Author(s):  
Abhay Ashtekar ◽  
Alejandro Corichi
Keyword(s):  
Black Hole ◽  
Black Hole Entropy ◽  
Quantum Geometry

scholarly journals Power law corrections to BTZ black hole entropy

2014 ◽  
Vol 24 (01) ◽  
pp. 1550001 ◽  
Author(s):  
Dharm Veer Singh
Keyword(s):  
Black Hole ◽  
Excited State ◽  
Power Law ◽  
Ground State ◽  
Entanglement Entropy ◽  
Black Hole Entropy ◽  
Mixed States ◽  
Btz Black Hole ◽  
First Excited State ◽  
Area Law

We study the quantum scalar field in the background of BTZ black hole and evaluate the entanglement entropy of the nonvacuum states. The entropy is proportional to the area of event horizon for the ground state, but the area law is violated in the case of nonvacuum states (first excited state and mixed states) and the corrections scale as power law.

scholarly journals Where are the degrees of freedom responsible for black-hole entropy?

2008 ◽  
Vol 86 (4) ◽  
pp. 653-658 ◽  
Author(s):  
S Das ◽  
S Shankaranarayanan ◽  
S Sur
Keyword(s):  
Black Hole ◽  
Excited State ◽  
Power Law ◽  
Ground State ◽  
Degrees Of Freedom ◽  
Black Hole Entropy ◽  
Quantum Field ◽  
Hole Area ◽  
Area Law ◽  
03.65 Ud

Considering the entanglement between quantum field degrees of freedom inside and outside the horizon as a plausible source of black-hole entropy, we address the question: where are the degrees of freedom that give rise to this entropy located? When the field is in ground state, the black-hole area law is obeyed and the degrees of freedom near the horizon contribute most to the entropy. However, for excited state, or a superposition of ground state and excited state, power-law corrections to the area law are obtained, and more significant contributions from the degrees of freedom far from the horizon are shown.PACS Nos.: 04.60.–m, 04.62., 04.70.–s, 03.65.Ud

scholarly journals Black Hole Entropy: A Closer Look

Entropy ◽  
2019 ◽  
Vol 22 (1) ◽  
pp. 17 ◽  
Author(s):  
Constantino Tsallis
Keyword(s):  
Complex System ◽  
Black Hole ◽  
Event Horizon ◽  
Black Hole Entropy ◽  
Planck Length ◽  
Horizon Area ◽  
C 73 ◽  
Area Law

In many papers in the literature, author(s) express their perplexity concerning the fact that the ( 3 + 1 ) black-hole ‘thermodynamical’ entropy appears to be proportional to its area and not to its volume, and would therefore seemingly be nonextensive, or, to be more precise, subextensive. To discuss this question on more clear terms, a non-Boltzmannian entropic functional noted S δ was applied [Tsallis and Cirto, Eur. Phys. J. C 73, 2487 (2013)] to this complex system which exhibits the so-called area-law. However, some nontrivial physical points still remain open, which we revisit now. This discussion is also based on the fact that the well known Bekenstein-Hawking entropy can be expressed as being proportional to the event horizon area divided by the square of the Planck length.

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