Streaming Media

Document Type

Article

Publication Date

2002

Abstract

The red dwarf + white dwarf eclipsing binary V471 Tau shows a variable Hα feature that varies from absorption during eclipse to maximum emission during white dwarf transit. In 1998 we obtained simultaneous BVRI photometry and Hα spectroscopy, with thorough phase coverage of the 12.5 hour orbital period. A binary star model was used with our light curve, radial velocity, and Hα data to refine stellar and orbital parameters. Combined absorption-emission profiles were generated by the model and fit to the observations, yielding a red star radius of 0.94⊙. Orbital inclination 78° is required with this size and other known parameters. The model includes three spots 1,000 K cooler than the surrounding photosphere. The variable Hα profile was modeled as a chromospheric region (essentially on the surface of the red star) centered at the substellar point. Additional emission seen outside our modeled profiles may be large co-rotating prominences that complicate the picture.

Comments

Note: This article was originally published as:

Vaccaro, Todd R., and Robert E. Wilson (2002). "Fluorescence and Chromospheric Activity of V471 Tau" in Astronomical Society of the Pacific Conference Series No. 279, Exotic Stars as Challenges to Evolution, IAU Colloquium 187, edited by Christopher A. Tout and Walter van Hamme,

The article was subsequently made available through the SAO/NASA Astrophysics Data System.

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