Evolution of charged evaporating black holes

Details Evolution of charged evaporating black holes Evolution of charged evaporating black holes

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990phrvd..41.1142h&link_type=abstract

Physical Review D (Particles and Fields), Volume 41, Issue 4, 15 February 1990, pp.1142-1151

Physics

31

Scientific paper

The evaporative evolution of charged nonrotating black holes is studied by numerically integrating a set of coupled differential equations describing the charge and mass as functions of time. We find that large charged black holes will evolve through a region (in the black-hole configuration space) of positive specific heat, undergoing two phase transitions as they evaporate. The region is approximately bounded by 3/4<(Q/M)2<1 and M>~2.03×107Msolar. Unlik rotating black holes (which always evolve toward the Schwarzschild limit), sufficiently large charged black holes will initially evolve toward the extreme Reissner-Nordström limit; their lifetime may be many orders of magnitude larger than the lifetime of a Schwarzschild black hole with the same initial mass.

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