BEHAVIOR OF SECTORIAL INSTABILITIES DEPENDING ON THE PARAMETERS OF THE GENERALIZED MODEL OF A SELF-GRAVITATING DISK
Section: STARS AND THE INTERSTELLAR MEDIUM
Authors:
1.
National University of Uzbekistan named after Mirzo Ulugbek
2.
Ulugh Beg Astronomical Institute of the Uzbek Academy of Sciences
Type:
Сonference article
Published:
27.12.2024
Subject area:
UDK 52 Астрономия. Геодезия
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
Language:
English
Keywords:
galaxies: evolution, formation, kinematics and dynamics, structure
Abstract (English):
In this work we study the problem of gravitational instability in the generalized model of a nonlinearly radially pulsating disk with an anisotropic velocity diagram relative to sectoral perturbation modes. This model is a nonstationary generalization of the equilibrium self-gravitating disk of Bisnovatyi-Kogan and Zeldovich. Nonstationary analogues of dispersion equations (NADE) are obtained on the background of this generalized model for sectoral modes of perturbations. Based on the results of numerical calculations of NADE, graphs comparing the increments of instability as a function of the initial virial ratio of the system for different values of the parameters and , characterizing the difference and the degree of anisotropy of the nonlinearly nonstationary generalized model of the self-gravitating disk, are constructed. In particular, it is found that the development of the bar-like perturbation mode will be the same for all anisotropic models, since the NADE of this mode does not depend on these parameters and .
In this work we study the problem of gravitational instability in the generalized model of a nonlinearly radially pulsating disk with an anisotropic velocity diagram relative to sectoral perturbation modes. This model is a nonstationary generalization of the equilibrium self-gravitating disk of Bisnovatyi-Kogan and Zeldovich. Nonstationary analogues of dispersion equations (NADE) are obtained on the background of this generalized model for sectoral modes of perturbations. Based on the results of numerical calculations of NADE, graphs comparing the increments of instability as a function of the initial virial ratio of the system for different values of the parameters and , characterizing the difference and the degree of anisotropy of the nonlinearly nonstationary generalized model of the self-gravitating disk, are constructed. In particular, it is found that the development of the bar-like perturbation mode will be the same for all anisotropic models, since the NADE of this mode does not depend on these parameters and .
Keywords:
galaxies: evolution, formation, kinematics and dynamics, structure
galaxies: evolution, formation, kinematics and dynamics, structure
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