Accretion efficiency at the Eddington luminous stage in quasars

Details Accretion efficiency at the Eddington luminous stage in quasars Accretion efficiency at the Eddington luminous stage in quasars

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26at...20..271d&link_type=abstract

Astronomical and Astrophysical Transactions, vol. 20, Issue 2, pp.271-274

Astronomy and Astrophysics

Astronomy

Quasars, Accreation, Massive Black Holes

Scientific paper

Non-steady and eruptive phenomena in quasars are thought to be associated with the Eddington or super-Eddington luminous stage. Although there is no lack of hypotheses about the total duration of such a stage, the latter remains essentially unknown. We calculate the duration of the quasar luminous stage as a function of the initial mass of a newborn massive black hole (MBH) by comparing the observed luminosity- and redshift distributions of quasars with the mass distribution of MBHs in normal galactic nuclei. It is assumed that, at the quasar stage, each MBH goes through a single (or recurrent) phase(s) of accretion with, or close to, the Eddington luminosity. The mass distributions of quasars is found to be connected with that of MBHs residing in normal galaxies by a single-valued relationship through the mass range 107-1011 M of the inferred MBHs.

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