Bose instability in Kerr black holes.

Details Bose instability in Kerr black holes. Bose instability in Kerr black holes.

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996babel.153...29g&link_type=abstract

Bulletin Astronomique de Belgrade, No. 153, p. 29 - 34

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Kerr Black Holes: Instabilities

Scientific paper

Bose instability in rotating (Kerr) black holes (BH's) consists in exponential increase in time of small perturbations of Bose mass fields, corresponding to superradiative, quasi bound levels. The minimal time of dumping of the angular momentum on the 2P envelope is much less than the time of dumping of the angular momentum by superradiation for primordial BH's when the mass of the particles m ≪ M2Pl/M. Very fast dumping of the angular momentum occurs when 0.46 ≥ mM/M2Pl ≥ 0.203 (for π0), 0.353(η), .0.065(D0). Electrically charged particles cannot develop Bose instability due to the ionization of bound levels by electromagnetic radiation emitted by the BH itself. The neutral particles produce γ-bursts of energies 67.5, 274.5, 932 MeV correspondingly. The duration of bursts is 1.26×10-17s(π0), 2.99×10-18s(η), 8.55×10-19s(D0). The radiated energies are 1.20×1035erg, 8.67×1034erg, 8.55×1033erg, corresponding to powers of the order of magnitude 1052erg/s. Other consequences for BH's evaporation are discussed.

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