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O. Y. Gnedin (Institute of Astronomy, Cambridge)
The collapse and dissipation of gas during the early stages of galaxy formation leads inevitably to the formation of a seed black hole at the center. Using the two-phase description of the interstellar media enclosed in the virialized dark matter halo, I present an analytical model of the gas collapse and fragmentation into cold clouds within the inner kpc. During the first 107 yr, before the supernovae feedback may affect the thermal balance, a substantial amount of gas is unable to fragment and form stars, and therefore it is destined to become a black hole ~106 solar masses. I discuss the effects of a possible protogalactic magnetic field acting to prevent fragmentation of clouds into stars. The resulting black hole provides a seed for further growth of the supermassive black hole by accretion of stellar ejecta or the tidally-disrupted stars.
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The author(s) of this abstract have provided an email address for comments about the abstract: ognedin@ast.cam.ac.uk