Vacuum energy density near static distorted black holes

Details Vacuum energy density near static distorted black holes Vacuum energy density near static distorted black holes

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986phrvd..33.1604f&link_type=abstract

Physical Review D (Particles and Fields), Volume 33, Issue 6, 15 March 1986, pp.1604-1610

Physics

12

Black Holes

Scientific paper

We investigate the contribution of massless fields of spins 0, 1/2, and 1 to the vacuum polarization near the event horizon of static Ricci-flat space-times. We do not assume any particular spatial symmetry. Within the Page-Brown ``ansatz'' we calculate <φ2>ren and ren near static distorted black holes, for both the Hartle-Hawking (||>H) and Boulware (||>B) vacua. Using Israel's description of static space-times, we express these quantities in an invariant geometric way. We obtain that <φ2>renH and renH near the horizon depend only on the two-dimensional geometry of the horizon surface. We find <φ2>renH=(1/48π2 )K0, renH=(7α+12β )K0 2-α(2)ΔK0. $K sub 0- is the Gaussian curvature of the horizon, and α and β are numerical coefficients depending on the spin of a field. The term in (2)K0 is characteristic of the distortion of the black hole. When the event horizon is not distorted, K0 is a constant and this term disappears.

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