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Non-LTE modeling of narrow emission components of He and Ca lines in optical spectra of classical T Tauri starsстатья
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: 18 июля 2013 г.
- Авторы: Dodin A.V., Lamzin S.A., Sitnova T.M.
- Журнал: Astronomy Letters
- Том: 39
- Номер: 5
- Год издания: 2013
- Издательство: Maik Nauka/Interperiodica Publishing
- Местоположение издательства: Russian Federation
- Первая страница: 315
- Последняя страница: 335
- DOI: 10.1134/S1063773713050010
- Аннотация: Using LTE calculations of the structure of T Tauri stellar atmospheres heated by radiation from an accretion shock (Dodin and Lamzin 2012), we have calculated the spectrum of the hot spot emerging on the stellar surface by taking into account non-LTE effects for He I, He II, Ca I, and Ca II. Assuming the pre-shock gas density N (0) and velocity V (0) to be the same at all points of the accretion stream cross section, we have calculated the spectrum of the star+circular spot system at various N (0), V (0), and parameters characterizing the star and the spot. Using nine stars as an example, we show that the theoretical optical spectra reproduce well the observed veiling of photospheric absorption lines as well as the profiles and intensities of the so-called narrow components of He II and Ca I emission lines with an appropriate choice of parameters. The accreted gas density in all of the investigated stars except DK Tau has been found to be N (0) > 10(12) cm(-3). We have managed to choose the parameters for eight stars at a calcium abundance in the accreted gas xi (Ca) equal to the solar one, but we have been able to achieve agreement between the calculations and observations for TW Hya only by assuming xi (Ca) to be approximately a factor of 3 lower than the solar one. The estimated parameters do not depend on interstellar extinction, because they have been determined from the spectra normalized to the continuum level. The calculated intensity of Ca II lines has turned out to be lower than the observed one, but this contradiction can be eliminated by assuming that, in addition to the accreted gas with a high density N (0), a more rarefied gas also falls onto the star. The theoretical equivalent widths and relative intensities of the subordinate He I lines disagree significantly with the observations. This is apparently because non-LTE effects should be taken into account when calculating the structure of the upper layers of the hot spot, the accuracy of the cross sections for collisional processes from upper levels is insufficient, and the spot inhomogeneity should probably be taken into account.
- Добавил в систему: Ламзин Сергей Анатольевич