Universal criterion for black hole stability
arXiv:gr-qc/0504064 · doi:10.1103/PhysRevD.72.044005
Abstract
It is shown that a non-rotating macroscopic black hole with very large horizon area can remain in stable thermal equilibrium with Hawking radiation provided {\it its mass, as a function of horizon area, exceeds its microcanonical entropy, i.e., its entropy when isolated, without thermal radiation or accretion, and having a constant horizon area} (in appropriate units). The analysis does not use properties of specific classical spacetimes, but depends only on the plausible assumption that the mass is a function of the horizon area for large areas.
6 pages Latex, no figures; an equation added
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- Holography, Gauge-Gravity Connection and Black Hole Entropy
- Thermodynamics of Quantum Isolated Horizons with model Hamiltonians
- Black holes and entropy in loop quantum gravity: An overview
- Thermal stability of radiant black holes
- Thermodynamic partition function from quantum theory for black hole horizons in loop quantum gravity
- Stability of Quantum Isolated Horizon : A Local Observer's View