The stellar wind in the BO V-type eclipsing binary Y Cygni

Details The stellar wind in the BO V-type eclipsing binary Y Cygni The stellar wind in the BO V-type eclipsing binary Y Cygni

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2349..373m&link_type=abstract

In NASA. Goddard Space Flight Center Future of Ultraviolet Astronomy Based on Six Years of IUE Res. p 373-376 (SEE N85-20961 1

Astronomy and Astrophysics

Astronomy

3

Apsides, Celestial Sphere, Eclipsing Binary Stars, Iue, Stellar Winds, Ultraviolet Spectra, Binary Stars, Cygnus Constellation, Elliptical Orbits, Ultraviolet Astronomy

Scientific paper

The double lined eclipsing binary system Y Cygni (HD 198846) has well determined orbital elements, absolute dimensions, and rate of apsidal motion. In several high-dispersion short wavelength primary camera (SWP) images taken near eclipse and in one at quadrature, the profiles of the resonance lines of Si IV, C IV, and N V were studied. The C IV is very broad, and the absorption minima are shortward shifted by 160 km/s with respect to Si IV. The N V is weak but is shortward shifted by a similar amount and has a broad shortward wing. In general, the spectrum is similar to that of the single BO V-type star tau Scorpii. In the spectrum obtained at quadrature, the C IV profile is shifted in accordance with the orbital motion of the hotter, less massive star. It is likely that the wind-borne C IV absorption originates in this star. By fitting the C IV and N V lines with synthetic profiles computed from the program written by Oslon, a terminal velocity of 1500 km/s was obtained.

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