The growth history of giant black holes and the radio dichotomy of quasars

Details The growth history of giant black holes and the radio dichotomy of quasars The growth history of giant black holes and the radio dichotomy of quasars

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003newar..47..193c&link_type=abstract

New Astronomy Reviews, Volume 47, Issue 4-5, p. 193-197.

Astronomy and Astrophysics

Astronomy

Scientific paper

The radio jets' energy source is still controversial. Blandford and Znajek [MNRAS 179 (1977) 433] proposed that this source is the rotational kinetic energy of a supermassive black hole (SMBH). This proposal begs the question of whether SMBHs have the appropriate spin distribution to account for the observed radio property distribution. If the BZ process is the correct model for the radio-loud/quiet dichotomy and if SMBHs only acquire spin through gas accretion, then it is very difficult to reproduce a bimodal radio property distribution. Instead, a bimodal radio property distribution can be reproduced, if BHs also grow by coalescing with other SMBHs. The attractive point of this model is that it links the radio properties of quasars to SMBHs' merging histories, and therefore to the host galaxy's environment and morphology. I have used semi-analytic simulations of galaxy formation to investigate the growth histories of SMBHs and their environmental dependence. I present a scenario in which mergers of late type galaxies form radio-quiet quasars (RQQs) and mergers of early-type galaxies, which already contain SMBHs, are more likely to produce radio-loud quasars (RLQs). This scenario predicts that RLQs have a longer clustering length than RQQs.

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