2003/03/27 by J. A. Sellwood, Sellwood, J. A., Juntai Shen +1
Engineering · Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #Space Technology and Applications #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0303611
16 pages, 6 figures, LaTeX cls and sty files included. To appear in Carnegie Observatories Astrophysics Series, Vol. 1: Coevolution of Black Holes and Galaxies ed. L. C. Ho (Cambridge: Cambridge Univ. Press)
arxiv created 2003/03/27 · openalex publication_date 2003/03/27 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Any connection between central activity and the large-scale dynamics of disk galaxies requires an efficient mechanism to remove angular momentum from the orbiting material. The only viable means of achieving inflow from kiloparsec scales is through gravitational stresses created by bars and/or mergers. The inflow of gas in bars today appears to stall at a radius of few hundred parsec, however, forming a nuclear ring. Here we suggest that bars in the early Universe may have avoided this problem, and propose that the progenitors of central supermassive black holes (SMBHs) are created by gas that is driven deep into the centers of galaxies by bars in the early stages of disk formation. The coincidence of the QSO epoch with galaxy formation, the short lifetimes of QSOs, and the existence of SMBHs in the centers of most bright galaxies are all naturally accounted for by disk dynamics in this model. The progenitor SMBHs are the seeds for brighter QSO flares during galaxy mergers. We present a new study of bar weakening by central mass concentrations, which shows that bars are less easily destroyed than previously thought. An extremely massive and compact central mass can, however, dissolve the bar, which creates a pseudo-bulge component in the center of the disk.