Formation history of supermassive black holes in a viable cosmological window

Details Formation history of supermassive black holes in a viable cosmological window Formation history of supermassive black holes in a viable cosmological window

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..238..345c&link_type=abstract

Black Holes from Stars to Galaxies -- Across the Range of Masses. Edited by V. Karas and G. Matt. Proceedings of IAU Symposium #

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Scientific paper

In this work we study the formation history of supermassive black holes in the centre of quasars and galaxies, from one scenario where supermassive stars, in the primitive universe (z ˜ 30-40) collapse to intermediate mass black holes (IMBHs). As a form to obtain the black hole growth, our calculations include the accretion mechanism, using a magneto-hydrodynamics (MHD) disk model. We show, performing a viable cosmological window, that only the MHD disk model is capable to transform intermediate mass black holes (IMBHs) (with masses ˜ 103 Msun) in supermassive black holes (SMBHs) with masses ˜ 107 Msun. We still calculate the supermassive stars sequence of stability. Those stars, with synthetized helium or oxygen cores, originated the IMBHs. In this calculation we show that the primordial stars must have rapid rotation if necessarily they are in the stable part of the sequence. In the limit of stability, such stars expel their hydrogen envelope, and by radial instabilities, their core collapses to form IMBHs. As a necessary revision, we explain, in the initial part of this dissertation, some energetical and dynamical properties of quasars and galaxies, focusing the conjugated evolution of those objects with their central black holes. As a consequence of first stars and quasars emergence, we explain yet the reionization of the universe, the moment where the universe becomes transparent, ilustrating then the cosmological impact due to the presence of such objects.

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