Spectroscopic Orbits for Two White Dwarf Binaries Identified in X-ray, EUV, and UV Surveys by ROSAT and IUE

Details Spectroscopic Orbits for Two White Dwarf Binaries Identified in X-ray, EUV, and UV Surveys by ROSAT and IUE Spectroscopic Orbits for Two White Dwarf Binaries Identified in X-ray, EUV, and UV Surveys by ROSAT and IUE

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.7903e&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #79.03; Bulletin of the American Astronomical Society, Vol. 28, p.1380

Astronomy and Astrophysics

Astronomy

Scientific paper

We present spectroscopic orbits for two binaries with main sequence primaries and white dwarf companions. These systems were originally identified because they showed more X-ray emission than expected for main sequence stars. The presence of each white dwarf companion was subsequently confirmed by the detection of its spectrum in the ultraviolet using IUE. Velocity variations of the primary stars in both systems were monitored using the CfA Digital Speedometers. The orbital periods are 21(d) .7217 and 2(d) .9934 for HR 8210 and HD 33959C, respectively. The minimum mass for the white dwarf companion of HR 8210 is 1.171 M_sun, which suggests an unusually massive progenitor. HD 33959C is a candidate for a system that has undergone a common-envelope phase.

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