Evaporation of Charged Black Holes Near Extremality

Details Evaporation of Charged Black Holes Near Extremality Evaporation of Charged Black Holes Near Extremality

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002nmgm.meet.1517f&link_type=abstract

"THE NINTH MARCEL GROSSMANN MEETING On Recent Developments in Theoretical and Experimental General Relativity, Gravitation and R

Physics

Scientific paper

The quantum evolution of black holes including back reaction effects is an open problem. One can simplify it by considering the scattering of low-energy neutral particles off extremal Reissner-Nordström black holes 1. If, in addition, we also consider spherically reduced configurations, the theory can be described, in a region very close to the horizon, by a solvable effective model. This model is just the Jackiw-Teitelboim model 2 (for details see 3) I = ∫{d2 x√{-g} [{(R + (4)/({l2 q3)}) ˜ φ - 1/2 ∑ limits iN {|∇ fi |2 } (1) where the two-dimensional fields of (1) are related to the four-dimensional metric by the expression ds_{(4)}(2) = {2l}/{r_0 }ds_{(2)}(2) + (r_0(2) + 4l(2) tilde phi )dOmega (2,) r0 = lq is the extremal radius, and l2 = G is Newton's constant. The fields fi represent null matter. To analyze back reaction effects we have to add to the classical action (1) the Polyakov-Liouville term IPL = -{N hbar}/{96π} ∫{d2 x√ { - g} R□ { - 1} R + {N hbar}/{12π} ∫ {d2 x√ {-g} λ2 (2)

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