2005/01/26 by V. Karas, Karas, V., L. Subr +2
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Mechanics and Biomechanics Studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0501578
Poster session paper #2103, XXII Texas Symposium on Relativistic Astrophysics, Stanford University, December 2004; 6 pages (minor revision)
openalex publication_date 2005/01/26 · arxiv created 2005/01/31 · arxiv updated 2009/12/01 · openalex created_date 2020/01/23 · openalex updated_date 2026/07/28
We discuss the structure of a central stellar cluster whose dynamics is\ninfluenced by gravitation of a supermassive black hole and by the dissipative\ninteraction of orbiting stars with an accretion disc. We also take the effect\nof disc self-gravity into account. We show that the cluster properties are\ndetermined predominantly by the radial profile of the disc surface density. To\nthis aim we develop a simple steady-state model of the central cluster and we\nestimate the rate at which stars migrate to the centre.\n This model is relevant for central regions of an active galactic nucleus\n(AGN) containing a rather dense accretion medium. In passing we also briefly\nmention a possibility that a fossil (inactive) disc could exist in the centre\nof our own Galaxy. Such a hypothetical disc could perturb the motion of stars\nand set them on highly elliptic trajectories with small pericentre distances.\nThe required mass of the disc is less than one percent of the central black\nhole mass, i.e. below the upper limit permitted by present accuracy of the\norbital parameters of S-stars in the Galactic Centre.\n