Primordial black holes: pair creation, Lorentzian condition, and evaporation.

Details Primordial black holes: pair creation, Lorentzian condition, and evaporation. Primordial black holes: pair creation, Lorentzian condition, and evaporation.

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ijtp...38.1227b&link_type=abstract

International Journal of Theoretical Physics, Vol. 38, No. 4, p. 1227 - 1252

Physics

3

Black Holes: Cosmology, Black Holes: Evaporation

Scientific paper

The wave function of the universe is usually taken to be a functional of the three-metric on a spacelike section, Σ, which is measured. It is sometimes better, however, to work in the conjugate representation, where the wave function depends on a quantity related to the second fundamental form of Σ. This makes it possible to ensure that Σ is part of a Lorentzian universe by requiring that the argument of the wave function be purely imaginary. The authors demonstrate the advantages of this formalism first in the well-known examples of the nucleation of a de Sitter or a Nariai universe. They then use it to calculate the pair creation rate for submaximal black holes in de Sitter space, which had been thought to vanish semiclassically. They also study the quantum evolution of asymptotically de Sitter black holes. For black holes whose size is comparable to that of the cosmological horizon, this process differs significantly from the evaporation of asymptotically flat black holes. The model includes the one-loop effective action in the s-wave and large-N approximation. Black holes of the maximal mass are in equilibrium. Unexpectedly, the authors find that nearly maximal quantum Schwarzschild-de Sitter black holes antievaporate. However, there is a different perturbative mode that leads to evaporation. They show that this mode will always be excited when a pair of maximal cosmological black holes nucleates.

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