  We have derived the criteria for thermal stability of charged rotating black
holes, for horizon areas that are large relative to the Planck area (in these
dimensions). In this paper, we generalized it for black holes with arbitrary
hairs. The derivation uses results of loop quantum gravity and equilibrium
statistical mechanics of the grand canonical ensemble and there is no explicit
use of classical spacetime geometry at all in this analysis. The assumption is
that the mass of the black hole is a function of its horizon area and all the
hairs. Our stability criteria are then tested in detail against some specific
black holes, whose metrics provide us with explicit relations for the
dependence of the mass on the area and other hairs of the black holes. This
enables us to predict which of these black holes are expected to be thermally
unstable under Hawking radiation.
