The Eddington Luminosity Phase in Quasars: Duration and Implications

Details The Eddington Luminosity Phase in Quasars: Duration and Implications The Eddington Luminosity Phase in Quasars: Duration and Implications

1999-12-08

arxiv.org/abs/astro-ph/9912152v1

Astronomy and Astrophysics

Astrophysics

4 pages, 2 figures, uses aipproc.sty. To appear in "Cosmic Explosions" (Proc. of the 10th Annual October Conference in Marylan

Scientific paper

10.1063/1.1291731

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 in hypotheses about the total duration of such a stage, the latter remains essentially unknown. We calculate the duration of quasar luminous phase in dependence upon the initial mass of a newborn massive black hole (MBH) by comparing the observed luminosity- and redshift distributions of quasars with mass distribution of the central 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 one-to-one corrrespondence through the entire mass range of the inferred MBHs if the accretion efficiency of mass-to-energy transformation $\eta \sim 0.1$.

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