Development of a theory of the origin of galaxy subsystems: results of calculation of high-degree oscillation modes
Abstract
In this paper, the instability of three high-order oscillation modes is studied. The origin of galaxies and their subsystems is discussed. Possible models for the formation and evolution of globular clusters and their host galaxies are presented. Nonlinear models for a collapsing protogalaxy are constructed, and nonstationary dispersion equations for high-order modes are derived. The stability of the model with respect to three high-order bulk perturbation modes is investigated. Nonstationary dispersion equations are derived for each mode. The critical dependence of the initial virial ratio on the rotation parameter is constructed. The dependences of the instability increments on the physical parameters of the model are found. The instability increments of the oscillation modes for fixed values of the rotation parameter are compared. It is shown that among the oscillation modes studied, for all values of the rotation parameter, the (4,2) mode is the leading one. It is proven that with increasing degree of the oscillation mode, the instability increments gradually decrease. The article also utilizes methods for integrating systems of differential equations containing free parameters using the stability method for periodic solutions, standard integration programs, and numerical calculations of instability increments for model problems. The study focused on self-gravitating systems, their theoretical models, and observed, theoretically unstudied, large-scale structural formations in disk galaxies. The subject of the study was the formation of structural formations in self-gravitating subsystems of galaxies and the mechanisms of gravitational instabilities against the backdrop of non-stationary models