Hawking temperatures for the Vaidya and the Reissner-Nordstrom-Vaidya black holes

Abstract

Abstract. We derive the Hawking temperature for both the Vaidya and the Reissner-Nordstrom-Vaidya black holes in two methods, the radial null geodesic method and the complex path method. Both black holes differ in some ways including the charge content and the number of horizons: the Vaidya black hole is charge-less and it has a single horizon while the Reissner-Nordstrom-Vaidya black hole is charged and it has two horizons. We obtain that the Hawking temperature for both black holes depends on their masses and on the radial change of their masses. Black hole with greater mass has a lesser Hawking temperature. We also obtain that there is a condition that should be fulfilled in order to guaranty positive values of the Hawking temperature. Some special cases for the Reissner-Nordstrom-Vaidya black hole are also discussed.

Dirac Particles Emission from An Elliptical Black Hole

“…This correlation is in a good agreement with previous calculations (Triyanta & Bowaire, 2013). In other words, for spherically symmetric case, the variable ξ is constant, (i.e.…”

“…The calculation of black hole temperature is a topic that has been widely studied in a recent decade (Tiandho, 2016;Ding & Liu, 2011;Triyanta & Bowaire, 2013;Kai & Shu-Zheng, 2009). However, mostly calculations just focused on the spherical symmetric black holes.…”

Massive Charged Fermion Emissions from Kerr – Newman – Vaidya Black Holes

“…Equation (24) show that the relation between Θ action and θ coordinate. The solutions of ( 20) and ( 21) for region around event horizon would be obtained by Hamilton -Jacobi method explained in the next sections.…”

“…Several works in [18][19][20][21][22] provide tunnelling for several types of particle tunnelling from various types of black holes. Other works provide semiclassical methods for Hawking radiation on Vaidya type black holes [23][24][25][26], which are non-stationary black holes that their mass and charge depend on time and radius.…”

The Semiclassical Methods for Hawking Radiations on the Kerr – Newman – Vaidya Black Holes

“…Several works in [13][14] provided massive fermions particle tunnelling on several type of black holes. Other works in [16][17][18] provided semiclassical methods for Hawking radiation on Vaidya type black holes [15], which are non-stationary black holes that their mass and charge depend on time and radius.…”