Primordial black holes. B. Czerny Copernicus Astronomical Center, Warsaw on behalf of collaboration: D. Cline, B. Czerny, A. Dobrzycki, A. Janiuk, C. Matthey, M. Nikołajuk, S. Otwinowski. Introduction.
Copernicus Astronomical Center, Warsaw
on behalf of collaboration: D. Cline, B. Czerny, A. Dobrzycki, A. Janiuk, C. Matthey, M. Nikołajuk, S. Otwinowski
The existence of the primary black holes is an unproved but a very interesting possibility. Their detection, or their absence, will impose important constraints on the physics of the early Universe, nature of the dark mass constituting the dominant part of the matter, the origin of the high energy radiation and cosmic rays, and finally on the quantum gravity.
Primary black holes were supposed to form during the early stage of the Big Bang. In standard 4-dimensional approach their formation epoch t_0, their expected lifetime, t_1, and the temperature of their Hawking emission are given by the following expressions:
The existence of higher dimensions modify this predictions. Therefore, in our search for primordial black holes we have to allow for a broad range of their properties.
We plan to estimate the density of the more massive black holes at the basis of their X-ray and gamma-ray radiation due to accretion of the interstellar/intergalactic material. Preliminary formula for a total luminosity of the dark halo:
Enhanced number of VSB in BATSE data are comming from the anticenter region, unlike SWIFT/HETE2 events with afterglows (Cline et al. in preparation).
Cline et al. 1999, 2005
V/Vmax test shows that this class of bursts is not located at cosmological distances. Spectral properties are consistent with expectation of the evaporation of PBH. If so, the bursts are located at a distance of about 100 pc, for a 4-d black hole mass. Emission must be slightly beamed to satisfy the occurance frquency of Green et al. (2001). Anisotropy is an interesting aspect, consistent with the results of the Millenium cosmological simulations of the dark matter perturbations which predict significant clumpiness of dark matter.