X-ray Spectroscopy of the Contact Binary VW Cephei

Details X-ray Spectroscopy of the Contact Binary VW Cephei X-ray Spectroscopy of the Contact Binary VW Cephei

2006-06-28

arxiv.org/abs/astro-ph/0606690v1

Astrophys.J.650:1119-1132,2006

Astronomy and Astrophysics

Astrophysics

Accepted for publication in the Astropysical Journal, 23 June 2006; 22 pages, 15 figures

Scientific paper

10.1086/507404

Short-period binaries represent extreme cases in the generation of stellar coronae via a rotational dynamo. Such stars are important for probing the origin and nature of coronae in the regimes of rapid rotation and activity saturation. VW Cep (P=0.28 d) is a relatively bright, partially eclipsing, and very active object. Light curves made from Chandra/HETGS data show flaring and rotational modulation, but no eclipses. Velocity modulation of emission lines indicates that one component dominates the X-ray emission. The emission measure is highly structured, having three peaks. Helium-like triplet lines give electron densities of about 3.0E+10 - 18.0E+10 /cm^3. We conclude that the corona is predominantly on the polar regions of the primary star and compact.

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