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QSO formation under coevolution of SMBH and bulge

Published online by Cambridge University Press:  01 December 2004

N. Kawakatu ,
M. Umemura  and
M. Mori
N. Kawakatu
Affiliation:
Center for Computational Physics, University of Tsukuba, Ten-nodai, 1-1-1, Ibaraki 305-8577, Japan email: [email protected], [email protected]
M. Umemura
Affiliation:
Center for Computational Physics, University of Tsukuba, Ten-nodai, 1-1-1, Ibaraki 305-8577, Japan email: [email protected], [email protected]
M. Mori
Affiliation:
Department of Law, Senshu University, Tama-Ku, Kawasaki 214-8580, Japan email: [email protected]
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Abstract

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The formation and growth of supermassive black holes (SMBHs) physically linked with bulges are considered. We focus on the radiation hydrodynamic process for the growth of SMBH in the optically thick starburst phase, where radiation from bulge stars drives the mass accretion on to a galactic center through radiation drag effect. In the present scenario, the AGN luminosity-dominant phase (QSO phase) is preceded by the host luminosity-dominat phase, which is called “proto-QSO phase”. In this phase, there exists the massive dusty disks within younger bulges. Also, the proto-QSO phase is anticipated by an optically-thick ultraluminous infrared galaxy (ULIRG) phase. Furthermore, such radiation hydrodynamic model has been also applied to disk galaxies. It turns out that the mass of a SMBH primarily correlates with a bulge component even in a disk galaxy. Thus, by analogy to proto-QSOs, the BH growing phase in disk galaxies may have massive dusty disks within younger bulges.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
ORAL CONTRIBUTIONS
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS222 , March 2004 , pp. 493 - 496
Copyright
© 2004 International Astronomical Union