In the framework of 'microscopic' theory of black holes (J. references therein, we address the 'pre-radiation time' (PRT) of neutrinos from black holes, which implies the lapse of time from black hole's birth till radiation of an extremely high energy neutrinos. For post-PRT lifetime, the black hole no longer holds as a region of spacetime that cannot communicate with the external universe. We study main features of spherical accretion onto central BH and infer a mass accretion rate onto it, and, further, calculate the resulting PRT versus bolometric luminosity due to accretion onto black hole. We estimate the PRTs of AGN black holes, with the well-determined masses and bolometric luminosities, collected from the literature by Woo Jong-Hak and Urry (Astrophys. J. 579, 530, 2002) on which this paper is partially based. The simulations for the black holes of masses M BH (1.1 · 10 6 ÷ 4.2 · 10 9 ) M give the values of PRTs varying in the range of about T BH (4.3 · 10 5 ÷ 5.6 · 10 11 ) yr. The derived PRTs for the 60 AGN black holes are longer than the age of the universe (∼13.7 Gyr) favored today. At present, some of remaining 174 BHs may radiate neutrinos. However, these results G. Ter-Kazarian ( ) · L. Sargsyan would be underestimated if the reservoir of gas for accretion in the galaxy center is quite modest, and no obvious way to feed the BHs with substantial accretion.

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Recently observed rare mighty X-ray coherent pulsations coming from M82X-2 impose a significant challenge in breaking the Eddington limit. Alternative approach to circumvent the obstacles was studied in [1,2] by addressing the M82X-2 as a spinning intermediate mass black hole, resided in final stage of growth. This approach employs the microscopic theory of black hole (MTBH), which explores a spontaneous breaking of gravitation gauge symmetry at huge energies. The preceding developments of this theory are proved to be quite fruitful for addressing the growth and merging phenomena of the black hole seeds. It explains as well the origin of ZeV-neutrinos, which are of vital interest for the source of ultra-high energy particles. In the present work, we further expose the assertions made in previous model via a computation of essential astrophysical corrections introduced by the rotation to the characteristic phase profile of M82X-2.