Abstract
To study the influence of the central black hole on the formation of the bulge of spiral galaxies, we analyzed the relationship between the masses of supermassive black holes (SMBHs) and the parameters of their bulges. Unlike other authors, we consider only spiral galaxies. In this paper, we present empirical formulas derived from observations of 54 spiral galaxies, establishing connections between the mass of the central black hole (MBH), the bulge stellar mass (Mbulge), and the velocity dispersion (σ) of stars in it. A non-linear non-stationary disk model with an anisotropic velocity diagram is constructed. Within this model, the instabilities of individual perturbation modes are studied. The increments of instability are calculated depending on the physical parameters of the model. These values are compared across three perturbation modes. The paper is partly based on the report presented at the conference “Modern Stellar Astronomy-2022,” held at the Caucasian Mountain Observatory of the Sternberg Astronomical Institute of Lomonosov Moscow State University, on November 8–10, 2022.