ANALYSIS OF COROTATION RADII IN SPIRAL GALAXIES
Авторы:
1.
Sternberg Astronomical Institute, Lomonosov Moscow State University
г. Санкт-Петербург и Ленинградская область, Россия
г. Санкт-Петербург и Ленинградская область, Россия
2.
Pulkovo Astronomical Observatory, Russian Academy of Sciences
St. Petersburg State University
St. Petersburg State University
3.
Sternberg Astronomical Institute, Lomonosov Moscow State University
Тип:
Статья конференции
Опубликовано:
27.12.2024
Классификаторы:
УДК 52 Астрономия. Геодезия
УДК 53 Физика
УДК 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
УДК 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
УДК 523 Солнечная система
УДК 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
УДК 52-1 Метод изучения
УДК 52-6 Излучение и связанные с ним процессы
ГРНТИ 41.00 АСТРОНОМИЯ
ГРНТИ 29.35 Радиофизика. Физические основы электроники
ГРНТИ 29.31 Оптика
ГРНТИ 29.33 Лазерная физика
ГРНТИ 29.27 Физика плазмы
ГРНТИ 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
ОКСО 03.06.01 Физика и астрономия
ОКСО 03.05.01 Астрономия
ОКСО 03.04.03 Радиофизика
ББК 2 ЕСТЕСТВЕННЫЕ НАУКИ
ББК 223 Физика
ТБК 614 Астрономия
ТБК 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
УДК 53 Физика
УДК 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
УДК 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
УДК 523 Солнечная система
УДК 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
УДК 52-1 Метод изучения
УДК 52-6 Излучение и связанные с ним процессы
ГРНТИ 41.00 АСТРОНОМИЯ
ГРНТИ 29.35 Радиофизика. Физические основы электроники
ГРНТИ 29.31 Оптика
ГРНТИ 29.33 Лазерная физика
ГРНТИ 29.27 Физика плазмы
ГРНТИ 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
ОКСО 03.06.01 Физика и астрономия
ОКСО 03.05.01 Астрономия
ОКСО 03.04.03 Радиофизика
ББК 2 ЕСТЕСТВЕННЫЕ НАУКИ
ББК 223 Физика
ТБК 614 Астрономия
ТБК 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
Язык материала:
английский
Ключевые слова:
galaxies: spiral, kinematics and dynamics
Аннотация (русский):
The corotation radius is one of the key parameters of a galaxy, since it not only influences the course of the dynamical processes, but also allows to determine the nature of the spiral structure. A clearly defined corotation radius indicates the presence of a spiral density wave, while an uneven distribution of positions suggests a transient nature to the spiral structure. In this study, we collected measurements of the corotation radius from the literature for 547 galaxies, obtained using 12 different methods. After analyzing the collected data, we found that only a quarter of the galaxies had consistent measurements of the resonance positions within the error limits when at least two different methods were used. As an indicator of the consistency of the collected measurements, we considered two values for each galaxy: the fraction of total error coverage and a dimensionless parameter related to the separation of average values. These quantities were found to be independent of the number of measurements taken, the methods used, and the values of the rotation radius with large uncertainties. In addition, no relationship was found between our results and the distance to the galaxy or its morphological type. Furthermore, we have shown that the consistency measure between the corotation radii does not depend on the type of spiral structure or the presence of a bar. Therefore, the obtained results can be explained by the different nature of the spiral arms in galaxies from the collected sample, where a dominant number of objects have a transient structure. As an example, we have examined in detail three galaxies to which several methods for estimating the corotation radius were applied. After a detailed analysis, we found that all three galaxies may have different nature of spiral arms. NGC 3686 shows a density wave, while NGC 4321 has dynamic (transient) spirals. The spiral structure of NGC 2403, on the other hand, most likely consists of several different spiral modes.
The corotation radius is one of the key parameters of a galaxy, since it not only influences the course of the dynamical processes, but also allows to determine the nature of the spiral structure. A clearly defined corotation radius indicates the presence of a spiral density wave, while an uneven distribution of positions suggests a transient nature to the spiral structure. In this study, we collected measurements of the corotation radius from the literature for 547 galaxies, obtained using 12 different methods. After analyzing the collected data, we found that only a quarter of the galaxies had consistent measurements of the resonance positions within the error limits when at least two different methods were used. As an indicator of the consistency of the collected measurements, we considered two values for each galaxy: the fraction of total error coverage and a dimensionless parameter related to the separation of average values. These quantities were found to be independent of the number of measurements taken, the methods used, and the values of the rotation radius with large uncertainties. In addition, no relationship was found between our results and the distance to the galaxy or its morphological type. Furthermore, we have shown that the consistency measure between the corotation radii does not depend on the type of spiral structure or the presence of a bar. Therefore, the obtained results can be explained by the different nature of the spiral arms in galaxies from the collected sample, where a dominant number of objects have a transient structure. As an example, we have examined in detail three galaxies to which several methods for estimating the corotation radius were applied. After a detailed analysis, we found that all three galaxies may have different nature of spiral arms. NGC 3686 shows a density wave, while NGC 4321 has dynamic (transient) spirals. The spiral structure of NGC 2403, on the other hand, most likely consists of several different spiral modes.
Ключевые слова:
galaxies: spiral, kinematics and dynamics
galaxies: spiral, kinematics and dynamics
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