HEAD 2003 Meeting
Session 12. Protostars, Stars and Instrumentation III
Poster, Sunday-Wednesday, March 23, 2003, Duration of Meeting

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[12.05] X-ray Doppler Imaging of Rapidly Rotating Stellar Coronae

R. Hoogerwerf, N. S. Brickhouse, A. K. Dupree (Harvard-Smithsonian Center for Astrophysics)

Chandra HETG observations of the bright eclipsing contact binary 44i Boo and Chandra LETG observations for the eclipsing binary VW Cep show X-ray line profiles that are Doppler-shifted by orbital motion. After careful analysis of the spectrum of each binary, a composite line-profile is constructed by adding the individual spectral lines. This high signal-to-noise ratio composite line-profile yields orbital velocities for these binaries that are accurate to 30 km/sec and allows their orbital motion to be studied at higher time resolutions. In conjunction with X-ray lightcurves, the phase-binned composite line-profiles constrain coronal structures to be small and located at high latitudes.

These observations and techniques show the power of the Doppler Imaging Technique applied to X-ray line emission. Differences in localization of the X-ray and far UV emission are also discussed.

This work is supported in part by NASA grant GO2-3018X to the Smithsonian Astrophysical Observatory. N. S. Brickhouse acknowledges the support of the Chandra X-ray Observatory Center (NAS8-39073).

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Bulletin of the American Astronomical Society, 35#2
© 2003. The American Astronomical Soceity.