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Title: Hawking radiation from the Garfinkle-Horowitz-Strominger black hole, effective action, and covariant boundary condition

Abstract

We exploit the expression for the anomalous (chiral) effective action to obtain the Hawking radiation from a Garfinkle-Horowitz-Strominger (stringy) black hole falling in the class of the most general spherically symmetric black holes ({radical}(-g){ne}1), using only covariant boundary conditions at the event horizon. The connection between the anomalous and the normal energy-momentum tensors is also established from the effective action approach.

Authors:
 [1]
  1. S. N. Bose National Centre for Basic Sciences, JD Block, Sector III, Salt Lake, Kolkata-700098 (India)
Publication Date:
OSTI Identifier:
21249845
Resource Type:
Journal Article
Resource Relation:
Journal Name: Physical Review. D, Particles Fields; Journal Volume: 77; Journal Issue: 6; Other Information: DOI: 10.1103/PhysRevD.77.064027; (c) 2008 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BLACK HOLES; BOUNDARY CONDITIONS; CHIRALITY; ENERGY-MOMENTUM TENSOR; SPHERICAL CONFIGURATION; SYMMETRY

Citation Formats

Gangopadhyay, Sunandan. Hawking radiation from the Garfinkle-Horowitz-Strominger black hole, effective action, and covariant boundary condition. United States: N. p., 2008. Web. doi:10.1103/PHYSREVD.77.064027.
Gangopadhyay, Sunandan. Hawking radiation from the Garfinkle-Horowitz-Strominger black hole, effective action, and covariant boundary condition. United States. doi:10.1103/PHYSREVD.77.064027.
Gangopadhyay, Sunandan. 2008. "Hawking radiation from the Garfinkle-Horowitz-Strominger black hole, effective action, and covariant boundary condition". United States. doi:10.1103/PHYSREVD.77.064027.
@article{osti_21249845,
title = {Hawking radiation from the Garfinkle-Horowitz-Strominger black hole, effective action, and covariant boundary condition},
author = {Gangopadhyay, Sunandan},
abstractNote = {We exploit the expression for the anomalous (chiral) effective action to obtain the Hawking radiation from a Garfinkle-Horowitz-Strominger (stringy) black hole falling in the class of the most general spherically symmetric black holes ({radical}(-g){ne}1), using only covariant boundary conditions at the event horizon. The connection between the anomalous and the normal energy-momentum tensors is also established from the effective action approach.},
doi = {10.1103/PHYSREVD.77.064027},
journal = {Physical Review. D, Particles Fields},
number = 6,
volume = 77,
place = {United States},
year = 2008,
month = 3
}
  • We apply the method of Banerjee and Kulkarni [R. Banerjee and S. Kulkarni, Phys. Rev. D 77, 024018 (2008).] to provide a derivation of Hawking radiation from the Garfinkle-Horowitz-Strominger (stringy) black hole which falls in the class of the most general spherically symmetric black holes ({radical}(-g){ne}1) and also the nonextremal D1-D5 black hole using only covariant gravitational anomalies.
  • We study the order [alpha][prime] correction to the string black hole found by Garfinkle, Horowitz, and Strominger (GHS). We include all operators of dimension up to four in the Lagrangian, and use the field redefinition technique which facilitates the analysis. A mass correction, which is implied by the work of Giddings, Polchinski, and Strominger, is found for the extremal GHS black hole.
  • We adopt the covariant anomaly cancellation method as well as the effective action approach to obtain the Hawking radiation from the Reissner-Nordstroem blackhole with a global monopole falling in the class of the most general spherically symmetric charged blackhole ({radical}(-g){ne}1), using only covariant boundary conditions at the event horizon.
  • We consider quantum fields around uniformly accelerated black holes in the eternal Ernst geometry. At a particular value of the acceleration, the Bogoliubov transformation, which would be responsible for the late-time Hawking radiation, is found to be trivial. When this happens, Hawking`s thermal radiation, Doppler shifted or not, is absent to the asymptotic inertial observers despite the nonzero Hawking temperature, while the comoving observers find the black hole radiance exactly balanced by the acceleration heat bath. We close with a few comments.
  • Charged Dirac particles' Hawking radiation from a Kerr-Newman black hole is calculated using Damour-Ruffini's method. When energy conservation and the backreaction of particles to the space-time are considered, the emission spectrum is not purely thermal anymore. The leading term is exactly the Boltzman factor, and the deviation from the purely thermal spectrum can bring some information out, which can be treated as an explanation to the information loss paradox. The result can also be treated as a quantum-corrected radiation temperature, which is dependent on the black hole background and the radiation particle's energy, angular momentum, and charge.