Dmitry BizyaevА. В. ХоперсковN. Tiurina2026-03-222026-03-22200310.48550/arxiv.astro-ph/0306193https://doi.org/10.48550/arxiv.astro-ph/0306193https://andeanlibrary.org/handle/123456789/83914We present results of numerical modeling made for the galactic stellar disk embedded in the spherical halo. The non-linear dynamics of bending instabilities developed in the disk is studied. The axisymmetrical bending mode is considered as a main factor increasing the disk thickness. The model dependence between the disk thickness and the halo to disk mass ratio $M_h/M_d$ is inferred. The modeling results enable us to estimate the dark halo mass for several edge-on galaxies. The obtained values of $M_h/M_d$ for the galaxies considered are of order 1 - 2.enHaloThick diskAstrophysicsPhysicsGalaxyThin diskGalactic haloDiscDark matter haloComponent (thermodynamics)preprint