Forming supermassive black holes by accreting dark and baryon matter

摘要: Given a large-scale mixture of self-interacting dark matter (SIDM) particles and baryon distributed in the early Universe, we advance here two-phase accretion scenario for forming supermassive black holes (SMBHs) with masses around ∼10 9 M ○. at high redshifts z(≥6). The first phase is conceived to involve rapid quasi-spherical quasi-steady Bondi mainly SIDM embedded on seed (BHs) created z ≤ 30 by generation massive Population III stars; this earlier rapidly gives birth significantly enlarged BH BH,t1 ≃ 1.4 x 10 6 σ 0 /(1 cm 2 g -1 )(C s /30 kms ) 4 during ∼ 20-15, where cross-section per unit mass C velocity dispersion halo referred as an effective 'sound speed'. second growth envisaged proceed primarily via accretion, eventually leading SMBH ; such SMBHs may form either sustained Eddington limit or later lower sub-Eddington mean rates. In between these two phases, there transitional yet diffusively limited which eventual steady state would be much than rates main phases. We intend account reported detections few epochs, e.g. Sloan Digital Sky Survey (SDSS) 1148+5251 so forth, without necessarily resorting super-Eddington very frequent merging processes. Only extremely haloes associated rare peaks density fluctuations Universe harbour quasars. Observational consequences are discussed. During final stage accumulating mass, violent feedback circumnuclear environs galactic nucleus leads central bulge formation rise familiar empirical - b correlation inferred nearby normal galaxies being stellar bulge; our scenario, precedes that bulge.