Precession of Stellar Rings in the Center of Galaxy

Kondratyev, B.P.; Klyuchinsky, K.A.

Авторы: Kondratyev B.P., Klyuchinsky K.A.
Журнал: Moscow University Physics Bulletin
Том: 79
Номер: 5
Год издания: 2024
Издательство: Allerton Press
Местоположение издательства: New York, N.Y., United States
Первая страница: 627
Последняя страница: 633
DOI: 10.3103/S0027134924701911
Аннотация: Abstract—The dynamics of two interacting concentric wide star rings located around a supermassive black hole in the central parsec of the Galaxy is investigated. The most massive of them, the ring with the retrograde motion of stars (known in the literature as a “clockwise” disk) is modeled as R-disk with a small cutout in the center. Another ring with a direct motion of stars (“counter-clockwise” disk) is represented by a thin circular ring with an inclination α ≈ 62◦ to the plane of the R-disk. The masses of these rings M1, M2 (M1/M2 ≈ 60), their geometric parameters and spatial orientation are known from observations. The mutual gravitational energy Wmut and the angular moment of force M between therings have been found, and graphs of these quantities depending on the angle of inclination have been constructed. The angular momenta of the rings L(1) and L(2), whose ratio L(1)/L(2) ≈ 23.4 have also been calculated. For the system of rings, the Laplace plane and the angles of its orientation are determined. It has been established that the mutual perturbation of the rotating rings leads to precession of the nodes with a period of TΩ ≈ 3.53 × 105 years. The lines of the nodes of both rings in the Laplace plane move with the same angular velocity but in opposite directions. This explains the large angle of divergence of the lines of nodes known from observations.
Добавил в систему: Кондратьев Борис Петрович

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