2000/12/15 by A. V. Zasov, A. V. Khoperskov, N. V. Tyurina
Physics and Astronomy · #astro-ph
published as Paper presented at conference "Stellar Dynamics: from classic to modern", Sobolev institute, Saint Petersburg State University, Russia, August 2000 · 8 pages including 4 PostScript figures
arxiv created 2000/12/15 · arxiv updated 2009/12/01
Different ways of the determination of masses of galactic disks, based on the kinematic data, are briefly discussed. The analysis of the rotation curves which reach maximum inside of a disk, and N-body modeling, reproducing the rotation curves and stellar velocity dispersion of real galaxies, enable to conclude that the mass of a disk is usually significantly less than the total mass of spherical components (bulge + dark halo) inside of optical borders of a galaxy, although the exceptions also exist.