The Structured Chromosphere and Wind of TW Hya

Details The Structured Chromosphere and Wind of TW Hya The Structured Chromosphere and Wind of TW Hya

2007-02-14

arxiv.org/abs/astro-ph/0702395v1

Astronomy and Astrophysics

Astrophysics

7 pages, 6 figures. To appear in the 'Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, (Cool Stars 14)', ASP Con

Scientific paper

A continuous set of echelle spectra of TW Hya, taken with the MIKE spectrograph on the Magellan2/Clay telescope at Las Campanas Observatory in April 2006 reveals systematic variations in the flux, velocity, and profile of the H-alpha emission line which appear to be consistent with the photometric period of 2.8 days. Absorption features recur at high outflow velocities in the wind. This behavior suggests that: (a) accretion is not uniformly distributed over the stellar hemisphere in view; (b) stable structures are present in the chromosphere, most likely due to the stellar magnetic field configuration. Semi-empirical models of the atmosphere are constructed to reproduce line profiles of H-alpha and He I, 10830A and to define the wind structure. These preliminary calculations suggest the mass loss rate is variable and comparable to H-alpha mass accretion rates in the literature, requiring a very efficient mechanism if the wind is powered only by accretion.

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