On the nature of the candidate T-Tauri star V501 Aurigae

Vaňko, M.; Torres, G.; Hambálek, L.; Pribulla, T.; Buchhave, L.A.; Budaj, J.; Dubovský, P.; Garai, Z.; Ginski, C.; Grankin, K.; Komžík, R.; Krushevska, V.; Kundra, E.; Marka, C.; Mugrauer, M.; Neuhäuser, R.; Ohlert, J.; Parimucha, Š.; Perdelwitz, V.; Raetz, S.; Shugarov, S.Y.

Авторы: Vaňko M., Torres G., Hambálek L., Pribulla T., Buchhave L.A., Budaj J., Dubovský P., Garai Z., Ginski C., Grankin K., Komžík R., Krushevska V., Kundra E., Marka C., Mugrauer M., Neuhäuser R., Ohlert J., Parimucha Š., Perdelwitz V., Raetz S., Shugarov S.Y.
Журнал: Monthly Notices of the Royal Astronomical Society
Том: 467
Номер: 4
Год издания: 2017
Издательство: Oxford Journals, Oxford University Press
Местоположение издательства: Oxford, UK, England
Первая страница: 4902
Последняя страница: 4913
DOI: 10.1093/mnras/stx407
Аннотация: We report new multi-colour photometry and high-resolution spectroscopic observations of the long-period variable V501 Aur, previously considered to be a weak-lined T-Tauri star belonging to the Taurus-Auriga star-forming region. The spectroscopic observations reveal that V501 Aur is a single-lined spectroscopic binary system with a 68.8-day orbital period, a slightly eccentric orbit (e ~ 0.03), and a systemic velocity discrepant from the mean of Taurus-Auriga. The photometry shows quasi-periodic variations on a different, ~55-day timescale that we attribute to rotational modulation by spots. No eclipses are seen. The visible object is a rapidly rotating (vsini ~ 25 km/s) early K star, which along with the rotation period implies it must be large (R > 26.3 Rsun), as suggested also by spectroscopic estimates indicating a low surface gravity. The parallax from the Gaia mission and other independent estimates imply a distance much greater than the Taurus-Auriga region, consistent with the giant interpretation. Taken together, this evidence together with a re-evaluation of the LiI~$\lambda$6707 and H$\alpha$ lines shows that V501 Aur is not a T-Tauri star, but is instead a field binary with a giant primary far behind the Taurus-Auriga star-forming region. The large mass function from the spectroscopic orbit and a comparison with stellar evolution models suggest the secondary may be an early-type main-sequence star.
Добавил в систему: Шугаров Сергей Юрьевич

	ИСТИНА	Войти в систему Регистрация
	ИСТИНА ЦЭМИ РАН
	Главная Поиск Статистика О проекте Помощь

ИСТИНА

ИСТИНА ЦЭМИ РАН

On the nature of the candidate T-Tauri star V501 Aurigaeстатья

Прикрепленные файлы