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Formation history of supermassive black holes in a viable cosmological window

Published online by Cambridge University Press:  01 August 2006

Carlos H. Coimbra-Araújo  and
Amâncio C. S. Friaça
Carlos H. Coimbra-Araújo
Affiliation:
Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, CP 6165, 13083-970 Campinas, SP, Brazil
Amâncio C. S. Friaça
Affiliation:
Departamento de Astronomia, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, 05508-900 São Paulo, SP, Brazil
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Abstract

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We show, performing a viable cosmological window, that only the magneto hydrodynamic (MHD) disk model is capable to explain how an intermediate mass black hole (IMBH) (with masses ∼ 103M⊙) grows unto a supermassive black hole (SMBH) (with masses ∼ 107M⊙). We still calculate the supermassive stars sequence of stability. Those stars, with synthetized helium or oxygen cores, collapse to form IMBHs. In our calculation we show that the primordial stars must have rapid rotation if they are in the stable part of the sequence.

Keywords

Black holes – quasars – first stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 345 - 346
Copyright
Copyright © International Astronomical Union 2007

References

Bennet, C. L. et al. 2003, ApJS, 148, 97Google Scholar
Fan, X. et al. 2003, AJ, 125, 1649CrossRefGoogle Scholar
McKinney, J. C. & Gammie, C. F. 2004, ApJ, 611, 977CrossRefGoogle Scholar
Spergel, D. N. et al. 2003, ApJS, 148, 175Google Scholar
Yu, Q. & Tremaine, S. 2002, MNRAS, 335, 965Google Scholar