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Hα and NaD Line Variability in RY Tauri

Published online by Cambridge University Press:  12 April 2016

P. Petrov  and
O. Vilhu
P. Petrov
Affiliation:
Crimean Astrophysical Observatory, 334413 Crimea, USSR
O. Vilhu
Affiliation:
Observatory and Astrophysics Laboratory, University of Helsinki, SF-00130 Helsinki, Finland

Abstract

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Using high resolution spectroscopy of the T Tau star RY Tau in the regions of Hα and Na D lines, we discovered line profile variability, which is interpreted by a hypothesis of stellar ’prominences’: cool gas clouds are moving inside the stellar wind, ascending and descending on a time scale of a few days. These clouds are supposed to be controlled by the magnetic field of the star. The range of radial velocities of the clouds (−100 to +100 km/s) is twice as large as the rotational velocity (v sin i) of the star. The form of variability of the Hα profile suggests the existence of two components: the (variable) stellar wind and the circumstellar disc.

Type
Part IV Stellar activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 471 - 476
Copyright
Copyright © Springer-Verlag 1991

References

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