2003/01/16 by Amr El‐Zant, Amr El-Zant, Isaac Shlosman +3 · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/375150
published as Astrophys.J.590:641-653,2003 · 20 pp, 10 postscript figures, submitted to the Astrophysical Journal
arxiv created 2003/01/16 · openalex publication_date 2003/06/20 · arxiv updated 2009/12/01 · openalex created_date 2020/11/23 · openalex updated_date 2026/08/01
The masses of supermassive black holes (SBHs) show correlations with bulge properties in disk and elliptical galaxies. We study the formation of galactic structure within flat-core, mildly triaxial halos and show that these correlations can be understood within the framework of a baryonic component modifying the orbital structure in the underlying potential. In particular, we find that terminal properties of bulges and their central SBHs are constrained by the destruction of box orbits in the harmonic cores of dark halos and the emergence of progressively less eccentric loop orbits there. SBH masses, M • , should exhibit a tighter correlation with bulge velocity dispersions, σ B , than with bulge masses, M B , in accord with observations, if there is a significant scatter in the M H -σ H relation for the halo. In the context of this model the observed M • -σ B relation implies that halos should exhibit a Faber-Jackson type relationship between their masses and velocity dispersions. The most important prediction of our model is that halo properties determine the bulge and SBH parameters. The model also has important implications for galactic morphology and the process of disk formation.