|
ИСТИНА |
Войти в систему Регистрация |
ИПМех РАН |
||
Analysis of the ionized-hydrogen motions in the direction of the CYG OB1 and CYG OB3 associationsстатья
Информация о цитировании статьи получена из
Web of Science,
Scopus
Статья опубликована в журнале из списка Web of Science и/или Scopus
Дата последнего поиска статьи во внешних источниках: 8 февраля 2017 г.
- Авторы: Lozinskaya T.A., Pravdikova V.V., Sitnik T.G., Esipov V.F., Mel'nikov V.V.
- Журнал: Astronomy Reports
- Том: 42
- Номер: 4
- Год издания: 1998
- Издательство: Maik Nauka/Interperiodica Publishing
- Местоположение издательства: Russian Federation
- Первая страница: 453
- Последняя страница: 464
- Аннотация: Interferometric H-alpha observations of the system of shells in the region of the Cyg OB1 and Cyg OB3 associations are presented. The ionized-hydrogen radial-velocity field is studied in the region I similar to 725 degrees-79 degrees, b similar to 1 degrees-4 degrees. The main component in the line profile is observed in the radial-velocity interval Delta V-LSR = 2-20 km/s. A decrease in the radial velocity of the main component with longitude is noted, due to the differential rotation of the Galaxy. A comparison of the observed run of mean velocity with that expected for various distances suggests that most of the radiating ionized gas in the direction of Cyg OB1 is at a distance of 1.5-2 kpc. This is consistent with the mean photometric distance to stars in this association. In some regions, a secondary line maximum is observed at high positive or negative velocities, at a level no less than 30-35% of the maximum intensity of the main component. High-velocity motions at negative velocities up to V-LSR = -85 km/s have been observed on multiple occasions, including in interstellar absorption lines in the spectra of the stars of Cyg OB1 and Cyg OB3. The widespread presence of regions with high positive velocities V-LSR = 30-55 km/s is reported here for the first time. The relation between the spatial distributions of the molecular and ionized components of the shell complex is discussed. It is concluded that the multiple-shell system formed as the result of an interaction between the stars of the Cyg OB1 association and a dense molecular complex. At the western edge of the multiple-shell system, there is some contribution from the stars of the Cyg OB3 association, and, at the eastern edge, there is a significant contribution from the stars of Cyg OB9 and from two WR stars at a distance of about 900 pc.
- Добавил в систему: Ситник Татьяна Григорьевна