Quasi-classical Hawking Temperatures and Black Hole Thermodynamics

Abstract

The semi-classical derivation of Hawking radiation for axially symmetric, stationary spacetimes with a Killing horizon is examined following the recent quasi-classical tunneling analysis and a simple formula is found for the inverse Hawking temperature $\beta =1/T_H$. The formula is invariant under canonical transformations and is shown to be equivalent to the integral of a closed differential 1-form around the horizon enclosing a pole. The Hawking temperature is then given in terms of the winding number in the first homotopy group of the torus formed from the compactified imaginary parts of the analytically continued radial and time variables.

9 pages, Talk given at Quarks 2008, 15th international seminar on high energy physics, Sergiev Posad, Russia, May 2008

References in corpus (1)

• Comments on anomaly versus WKB/tunneling methods for calculating Unruh radiation

Cited by in corpus (5)

• Corrections to Hawking-like Radiation for a Friedmann-Robertson-Walker Universe
• Information loss and entropy conservation in quantum corrected Hawking radiation
• Corrected Entropy of Friedmann-Robertson-Walker Universe in Tunneling Method
• Invariance of the Hamilton-Jacobi tunneling method for black holes and FRW model
• Hawking radiation of Reissner-Nordstrom-de Sitter black hole by Hamilton-Jacobi method