Fundamental parameters of the W Serpentis stars

Details Fundamental parameters of the W Serpentis stars Fundamental parameters of the W Serpentis stars

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ssrv...50..179a&link_type=abstract

(IAU, NSERC, Canadian Institute of Theoretical Astrophysics, et al., Colloquium on Algols, 107th, Sidney, Canada, Aug. 15-19, 19

Astronomy and Astrophysics

Astrophysics

3

Cool Stars, Eclipsing Binary Stars, Light Curve, Radial Velocity, Stellar Spectra, Stellar Spectrophotometry, Cross Correlation, Digital Techniques

Scientific paper

Application of digital cross-correlation spectroscopy to the spectra of the W Serpentis binaries SX Cas and RX Cas has allowed an accurate determination of the orbits and rotations of the (mass-losing) K-subgiant secondary components. The distortion of the primary radial-velocity curves due to the influence of the prominent accretion disks in these systems has been modeled to first order. This makes it possible to estimate K1, and thereby the mass ratio q = 0.30, to within + or - 20 percent. The absolute radii of the secondaries are derived independently from the observed rotations and periods, assuming synchronous rotation. They show that the stars fill their Roche lobes, or at least very nearly so. Rough fits to the available photometry shows both primaries to be unevolved mid-B stars; that in RX Cas appears completely obscured by the disk.

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