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S. Redfield (McDonald Observatory, University of Texas), J.L. Linsky (JILA, University of Colorado and NIST), T.R. Ayres, A. Brown (CASA, University of Colorado), G.J. Herczeg (JILA, University of Colorado and NIST)
RS CVn systems are detached late-type binaries that are very active as a result of their tidally-enforced rapid rotation. They are actively studied and bright at X-ray and ultraviolet (UV) wavelengths, but very few have been observed in the far-UV. We present multiple orbital phase observations of RS CVn systems taken by the Far Ultraviolet Spectroscopic Explorer (FUSE). Located in the FUSE spectral range are emission lines formed in plasma at 50,000-300,000 K (e.g., C III and O VI). We present an analysis of the strong emission line profiles. By monitoring the change in the profile shape over the course of an orbital period we can measure the fractional contributions of each star in the RS CVn binary system at different plasma temperatures. In addition, the spectral resolution and wavelength scale of FUSE permit us to measure the width and velocity shift of the O VI and C III lines, providing a new window on stellar atmospheric dynamics and structure.
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The author(s) of this abstract have provided an email address for comments about the abstract: sredfield@astro.as.utexas.edu
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.