How Reissner-Nordström black holes behave part2(Astrophysics)
- Curved space and particle physics effects on the formation of Bose-Einstein condensation around a Reissner-Nordström black hole(arXiv)
Author : Recai Erdem, Betül Demirkaya, Kemal Gültekin
Abstract : We consider two scalar fields interacting through a χ∗χφ∗φ term in the presence of a Reissner-Nordstrom black hole. Initially, only χ particles are present. We find that the produced φ particles are localized in a region around the black hole and have a tendency towards condensation provided that φ particles are much heavier than the χ particles. We also find that such a configuration is phenomenologically viable only if the scalars and the black hole have dark electric charges
2. Effect of the inner horizon on the black hole thermodynamics: Reissner-Nordström black holeand Kerr black hole(arXiv)
Author : G. E. Volovik
Abstract : For the Schwarzschild black hole the Bekenstein-Hawking entropy is proportional to the area of the event horizon. For the black holes with two horizons the thermodynamics is not very clear, since the role of the inner horizons is not well established. Here we calculate the entropy of the Reissner-Nordström black hole and of the Kerr black hole, which have two horizons. For the spherically symmetric Reissner-Nordström black hole we used several different approaches. All of them give the same result for the entropy and for the corresponding temperature of the thermal Hawking radiation. The entropy is not determined by the area of the outer horizon, and it is not equal to the sum of the entropies of two horizons. It is determined by the correlations between the two horizons, due to which the total entropy of the black hole and the temperature of Hawking radiation depend only on mass M of the black hole and do not depend on the black hole charge Q. For the Kerr and Kerr-Newman black holes it is shown that their entropy has the similar property: it depends only on mass M of the black hole and does not depend on the angular momentum J and charge Q.
3. Hawking radiation received at infinity in higher dimensional Reissner-Nordström black holespacetimes(arXiv)
Author : Kai Lin, Wei-Liang Qian, Xilong Fan, Bin Wang, Elcio Abdalla
Abstract : In this work, we investigate the Hawking radiation in higher dimensional Reissner-Nordström black holes as received by an observer, resides at infinity. The frequency-dependent transmission rates, which deform the thermal radiation emitted in the vicinity of the black hole horizon, are evaluated numerically. Apart from the case of four-dimensional spacetime, the calculations are extended to higher dimensional Reissner-Nordström metrics, and the results are found to be somewhat sensitive to the spacetime dimension. In general, it is observed that the transmission coefficients practically vanishes when the frequency of the emitted particle approaches zero. It increases with increasing frequency and eventually saturates to some value. For four-dimensional spacetime, the above result is shown to be mostly independent of the metric’s parameter, neither of the orbital quantum number of the particle, once the location of the event horizon, rh, and the product of the charges of the black hole and the particle qQ are given. For higher-dimensional cases, on the other hand, the convergence becomes more slowly. Moreover, the difference between states with different orbital quantum numbers is found to be more significant. As the magnitude of the product of charges qQ becomes more significant, the transmission coefficient exceeds one. In other words, the resultant spectral flux is amplified, which results in an accelerated process of black hole evaporation. The relation between the calculated outgoing transmission coefficient with existing results on the greybody factor is discussed
