Evaporation of a Kerr Black Hole by Emission of Scalar and Higher Spin Particles Typeset Using Revt E X 1

We study the evolution of an evaporating rotating black hole, described by the Kerr metric, which is emitting either solely massless scalar particles or a mixture of massless scalar and nonzero spin particles. Allowing the hole to radiate scalar particles increases the mass loss rate and decreases the angular momentum loss rate relative to a black hole which is radiating nonzero spin particles. The presence of scalar radiation can cause the evaporating hole to asymptotically approach a state which is described by a nonzero value of a a=M. This is contrary to the conventional view of black hole evaporation , wherein all black holes spin down more rapidly than they lose mass. A hole emitting solely scalar radiation will approach a nal asymptotic state described by a ' 0:555. A black hole that is emitting scalar particles and a canonical set of nonzero spin particles (3 species of neutrinos, a single photon species, and a single graviton species) will asymptotically approach a nonzero value of a only if there are at least 32 massless scalar elds. We also calculate the lifetime of a primordial black hole that formed with a value of the rotation parameter a , the minimum initial mass of a primordial black hole that is seen today with a rotation parameter a , and the entropy of a black hole that is emitting scalar or higher spin particles.