Hawking radiation in string theory and the string phase of black holes

Details Hawking radiation in string theory and the string phase of black holes Hawking radiation in string theory and the string phase of black holes

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000phrvd..61h4030r&link_type=abstract

Physical Review D (Particles, Fields, Gravitation, and Cosmology), Volume 61, Issue 8, 15 April 2000, id.084030

Physics

9

Quantum Aspects Of Black Holes, Evaporation, Thermodynamics, Quantum Field Theory In Curved Spacetime, Strings And Branes

Scientific paper

The quantum string emission by black holes is computed in the framework of the ``string analog model'' (or thermodynamical approach), which is well suited to combine quantum-field theory (QFT) and string theory in curved backgrounds (particularly here, as black holes and strings possess intrinsic thermal features and temperatures). The QFT-Hawking temperature TH is upper bounded by the string temperature TS in the black hole background. The black hole emission spectrum is an incomplete gamma function of (TH-TS). For TH<TS, it shows that highly massive string states dominate the emission and undergo a typical string phase transition to a microscopic ``minimal'' black hole of mass Mmin or radius rmin (inversely proportional to TS) and string temperature TS. The string back reaction effect [self-consistent black hole solution of the semiclassical Einstein equations with mass M+ (radius r+) and temperature T+] is computed. Both the QFT and string black hole regimes are well defined and bounded: rmin<=r+<=rS, Mmin<=M+<=M, TH<=T+<=TS. The string ``minimal'' black hole has a life time τmin~=(kBc/Għ) T-3S.

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