SMBH Luminosity in the Starburst Environment

Abstract

We claim that in the starburst environment there is no accretion of the ISM onto the BH and thus, in such cases, the BH luminosity is regulated by the mass-loss rate from massive stars in the star forming region. We calculate the accretion rate and show that it is usually small during the superwind stage and grows at the post-starburst stage, when the matter reinserted by intermediate-mass stars remains gravitationally bound and fuels the central BH. Figure 1 presents the results from hydrodynamic calculations of gas accretion onto a central SMBH embedded in a massive star-forming region. An exponentially decaying starburst with an initial intensity SF R 0 and an e-folding time τSF is assumed. During the SNe stage, the superwind removes most of the matter reinserted by massive stars (see Silich et al. 2008), which results into negligible accretion rates. The accretion rate grows rapidly when the superwind stage decays and is replaced by a gravitationally bound regime that is dominated by intermediate-mass stars. This leads to a time delay (Davies et al. 2007) between the beginning of a starburst and the emergence of the AGN. The value of the lag time depends on the characteristic timescale τ S F of the starburst phase.

Gemini 3D spectroscopy of BAL+IR+Fe ii QSOs - II. IRAS 04505−2958, an explosive QSO with hypershells and a new scenario for galaxy formation and galaxy end phase

“…Tenorio‐Tagle et al (1999), Tenorio‐Tagle et al (2003a), Tenorio‐Tagle, Silich & Munoz‐Tunon (2003b), Tenorio‐Tagle et al (2005), Tenorio‐Tagle et al (2006), Silich et al (2004), Silich, Tenorio‐Tagle & Anorve Zeferino (2005), Silich, Hueyot‐Zahuantitla & Tenorio‐Tagle (2008), Tenorio‐Tagle & Bodenheimer (1988) and Heiles (1987) give further details and references of theoretical and observational studies of giant shells, bubbles and rings, associated with multiple explosion of Type II SNe/HyNe.…”