Semiclassical Approaches to the Hawking Temperatures of Radiating Kerr - Newman - Vaidya Black Holes Ahmad H. Salimi (a), Triyanta (a,b)
(a) High Energy Theoretical Physics Division,
Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung
Jalan Ganesha no.10, Bandung 40132 Indonesia
(b) Indonesian Center for Theoretical and Mathematical Physics
Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung
Jalan Ganesha no.10, Bandung 40132 Indonesia
Abstract
In this research, the analysis of Hawking radiation on non-stationary black hole Kerr -
Newman - Vaidya was determined through semiclassical approaches. The non-stationary term, that
can be negative or positive, for this black hole corresponds to the change of mass with respect to time
and radial coordinates. The negative value of non-stationary term implies the black hole radiates, but
the positive value implies the black hole absorbs matter around it. Hawking temperature was derived
using two methods, namely, the semiclassical methods and the Bekenstein - Hawking temperature
formulation. The semiclassical methods that were used are radial null geodesic and complex path
analysis. These three calculations gave the same results, meaning these semiclassical approaches can
be used to determine the Hawking temperature of non-stationary black holes. The Hawking temperature
is inversely proportional to the mass and non-stationary term. If the mass of the black hole is getting
bigger, the temperature is getting smaller and vice versa. With these results, we concluded that the
increasing of non-stationary term will cause decreasing radiation probability. Furthermore, the entropy
of Kerr - Newman - Vaidya black hole was given by two formulations, which are the Bekenstein -
Hawking formulation and in dynamical form by the black hole dynamics equation. The entropy
formulations that were calcutated obey generalized second law of black holes.
