Quasi stable black holes and their implications

We had already derived the criteria for thermal stability of charged rotating quantum black holes, for horizon areas that are large relative to the Planck area. We also had extended it for black holes with arbitrary number of hairs in arbitrary dimensional spacetime. We found that most of the criteria for thermal stability are satisfied even by some unstable black holes, although they do not satisfy all the criteria. These black holes are called 'Quasi Stable' black holes. We have already calculated thermal fluctuations and correlations among hairs of a stable quantum black hole. In this paper, we extend this work for quasi stable quantum black holes. We get the interesting result that quasi stable black holes have finite fluctuations and correlations for some of its hairs, although the black hole will ultimately radiate away due to Hawking radiation. We have also shown that quasi stable black holes may decay in a slower rate in comparision to unstable black holes.