Abstract
The coevolution of a supermassive black hole (SMBH) and a bulge is considered based on a novel mechanism for BH formation, where the BH growth is promoted by the mass accretion driven by radiation drag which is exerted on dusty interstellar gas in radiation fields generated by bulge stars. It turns out that the resultant mass of a SMBH is predicted to be in proportion to the bulge mass, and the mass ratio is basically determined by the nuclear energy conversion efficiency from hydrogen to helium, e =0 .007. In the present scenario, the bulge luminosity overwhelms the BH accretion luminosity in the growing phase of SMBH. This phase corresponds to a “proto-QSO”, thereafter evolving to a QSO. Also, the proto-QSO phase is preceded by an optically-thick ultraluminous infrared galaxy (ULIRG) phase.
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