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Structure and kinematics of the interstellar medium around WR 142a: Searching for traces of the action of stellar windстатья
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: Sitnik T.G., Lozinskaya T.A., Pravdikova V.V.
- Журнал: Astronomy Letters
- Том: 33
- Номер: 12
- Год издания: 2007
- Издательство: Maik Nauka/Interperiodica Publishing
- Местоположение издательства: Russian Federation
- Первая страница: 814
- Последняя страница: 826
- DOI: 10.1134/S1063773707120055
- Аннотация: Based on our H alpha interferometric observations and CO data, we analyze the structure and kinematics of the gas in an extended region of the Cygnus arm around the recently discovered star WR 142a. We have established that WR 142a and the ionized hydrogen in its immediate neighborhood are associated with the complex of molecular clouds observed in a region with l similar to 78 degrees -80 degrees 30', b similar to 2 degrees-3 degrees 20', and V-LSR similar to 4-16 km s(-1). Traces of the action of the stellar wind from WR 142a on the ambient gas have been found to the northeast of the star in a region devoid of dense absorbing foreground clouds. These include very weak thin gas and dust filaments as well as high-velocity components of the H alpha profile, which can be interpreted as a possible expansion of the shell swept up by the wind with a velocity as high as 50-80 km s(-1). Giant regions of reduced CO emission dominated by high-velocity motions of ionized hydrogen have been detected. Stars of the Cyg OB2 association and the cluster NGC 6910 can be responsible for these motions.
- Добавил в систему: Ситник Татьяна Григорьевна