Evidence for accretion activity and obscured hot component stars in W Serpentis type binaries

Details Evidence for accretion activity and obscured hot component stars in W Serpentis type binaries Evidence for accretion activity and obscured hot component stars in W Serpentis type binaries

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...262..269y&link_type=abstract

Astrophysical Journal, Part 1, vol. 262, Nov. 1, 1982, p. 269-281.

Astronomy and Astrophysics

Astrophysics

18

Eclipsing Binary Stars, Hot Stars, Stellar Mass Accretion, Accretion Disks, Astronomical Photometry, Emission Spectra, Far Ultraviolet Radiation, Iue, Line Spectra, Stellar Color

Scientific paper

Recent studies of a number of peculiar Beta Lyrae type (or W Ser type) eclipsing binaries have been made by Plavec and Koch (1978), utilizing the International Ultraviolet Explorer (IUE) satellite. Results of these studies show two prominent features in the far-ultraviolet spectra of these long-period binaries. According to Plavec (1980), the obtained results indicate that the optical and hotter ultraviolet continua are associated with the accreting primary, which must have a structure more complicated than an ordinary star. As a mechanism for the ultraviolet excess, Plavec has suggested that the mass-gaining primary is surrounded by an optically and geometrically thick disk which creates a false photosphere. The present investigation is concerned with an observational test of this model. Five peculiar binary systems W Ser, V367 Cyg, SX Cas, RX Cas, and RW Per were observed photometrically during the times of primary eclipse, specifically to determine the behavior of the ultraviolet color as a function of phase.

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