Evaporation of a Kerr black hole by emission of scalar and higher spin particles

Details Evaporation of a Kerr black hole by emission of scalar and higher spin particles Evaporation of a Kerr black hole by emission of scalar and higher spin particles

1998-01-13

arxiv.org/abs/gr-qc/9801044v2

Phys.Rev.D58:044012,1998

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

22 pages, 13 figures, RevTeX format; added clearer descriptions for variables, added journal reference

Scientific paper

10.1103/PhysRevD.58.044012

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 $a_* \equiv a / M$. 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 final asymptotic state described by $a_* \simeq 0.555$. 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 fields. 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.

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