Finite black hole entropy and string theory

Journal Article · Sat Oct 15 00:00:00 EDT 1994 · Physical Review, D (Particles Fields); (United States)

DOI:https://doi.org/10.1103/PhysRevD.50.5225· OSTI ID:6909994

McGuigan, M ^[1]

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1. Institute for Fundamental Theory, University of Florida, Gainesville, Florida 32611 (United States)

An accelerating observer sees a thermal bath of radiation at the Hawking temperature which is proportional to the acceleration. Also, in string theory there is a Hagedorn temperature beyond which one cannot go without an infinite amount of energy. Several authors have shown that in the context of Hawking radiation a limiting temperature for string theory leads to a limiting acceleration, which for a black hole implies a minimum distance from the horizon for an observer to remain stationary. We argue that this effectively introduces a cutoff in Rindler space or the Schwarzschild geometry inside of which accelerations would exceed this maximum value. Furthermore, this natural cutoff in turn allows one to define a finite entropy for Rindler space or a black hole as all divergences were occurring on the horizon. In all cases if a particular relationship exists between Newton's constant and the string tension then the entropy of the string modes agrees with the Bekenstein-Hawking formula.

• DOE Contract Number: FG05-86ER40272
• OSTI ID: 6909994
• Journal Information: Physical Review, D (Particles Fields); (United States), Vol. 50:8; ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
STRING MODELS
ENTROPY
ACCELERATION
BLACK HOLES
SCHWARZSCHILD METRIC
COMPOSITE MODELS
EXTENDED PARTICLE MODEL
MATHEMATICAL MODELS
METRICS
PARTICLE MODELS
PHYSICAL PROPERTIES
QUARK MODEL
THERMODYNAMIC PROPERTIES
661310* - Relativity & Gravitation- (1992-)