Bending instability in galaxies: the stellar disk thickness and the mass of spheroidal component
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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 (M_h/M_d) in seven edge-on galaxies. The values of M_h/M_d are of order 1 for our galaxies.
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
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