The Structured Chromosphere and Wind of TW Hya

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dc.creatorDupree, A. K.
dc.creatorAvrett, E. H.
dc.creatorBrickhouse, N. S.
dc.creatorCranmer, S. R.
dc.creatorSzalai, T.
dc.date2007-02-14
dc.date.accessioned2026-07-07T07:46:58Z
dc.date.available2026-07-07T07:46:58Z
dc.descriptionA 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.
dc.description7 pages, 6 figures. To appear in the 'Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, (Cool Stars 14)', ASP Conf. Series
dc.identifierhttps://arxiv.org/abs/astro-ph/0702395
dc.identifierhttp://arxiv.org/abs/astro-ph/0702395
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/124007
dc.subjectAstrophysics
dc.titleThe Structured Chromosphere and Wind of TW Hya
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