2004/05/07 by N. V. Tyurina, N. Tyurina, А. В. Хоперсков +5
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0405142
17 pages including 20 PostScript figures. Oral talk presented in International Workshop "Progress in Study of Astrophysical Disks: Collective and Stochastic Phenomena and Computational Tools", Volgograd, September 9-11, 2003
arxiv created 2004/05/07 · openalex publication_date 2004/05/07 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present results of numerical N-body simulations of a galactic stellar disk embedded into a spherical dark halo. The non-linear dynamics of bending instabilities developing in the disk is studied. The bending modes, axisymmetric and not, are considered as main factors increasing the disk thickness. The relation between the disk vertical scale height and the halo+bulge-to-disk mass ratio is inferred. The method of estimation of the spherical-to-disk mass ratio for edge-on spiral galaxies based on this relation is studied and applied to constrain the spherical subsystem mass and the mass of dark halos (Mh/Md) in seven edge-on galaxies. The values of Mh/Md are of order 1 for our galaxies.