Thermal Radiation of Reissner-Nordström Black Hole

Abstract

By the entropy density near the event horizon, the result has been obtained that the thermal radiation of the black hole satisfies the generalized Stenfan-Boltzmann law. The derived generalized Stenfan-Boltzmann coefficient is no longer a constant, but a proportional coefficient related to the black hole mass, the black hole charge, the average radial effusion velocity of the radiation particles near the event horizon, the cut-off distance and the thin film thickness. For an extreme Reissner-Nordström black hole, radiation energy flux and radiation power are all equal to zero. Then, the generalized Stenfan-Boltzmann law will lead to a black hole remnant. In this paper, we have put forward a thermal particle model in curved space-time. By this model, the thermal radiation of the Reissner-Nordström black hole has been studied. The result shows that when the thin film thickness and the cut-off distance are both fixed for the Reissner-Nordström black hole, the radiation energy flux received by observer far away from the Reissner-Nordström black hole is proportional to the average radial effusion velocity of the radiation particles, and inversely proportional to the square of the distance between the observer and the black hole.

Thermodynamics and Stability of Five Dimensional AdS Reissner-Nordstrom Black Hole

“…If the sign of specific heat be positive, then the black hole is in unstable phase, and vise versa. Therefore we should specify sign of specific heat (10). Again we consider the relation (10) and analyze nominator and denominator of this equation separately.…”

“…Therefore we should specify sign of specific heat (10). Again we consider the relation (10) and analyze nominator and denominator of this equation separately. First of all we assume that the nominator is positive, in that case the denominator of (1) is also positive for 6πr 6 + + 16GML 2 r 2 + ≥ 3πQ 2 L 2 ≥ 3 5 (6πr 6 + + 16GML 2 r 2 + ).…”

“…[10], and found that the thermal radiation of the RN black hole satisfies the generalized Stefan-Boltzmann law [11][12][13]. Instead of RN AdS black hole, the RN de Sitter (dS) black hole considered in Ref.…”