Spectral investigation of the eclipsing binary star V 367 Cygni

Details Spectral investigation of the eclipsing binary star V 367 Cygni Spectral investigation of the eclipsing binary star V 367 Cygni

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985azh....62..542k&link_type=abstract

(Astronomicheskii Zhurnal, vol. 62, May-June 1985, p. 542-551) Soviet Astronomy (ISSN 0038-5301), vol. 29, May-June 1985, p. 314

Astronomy and Astrophysics

Astronomy

5

Eclipsing Binary Stars, H Lines, Stellar Envelopes, Stellar Spectra, Variable Stars, Electron Density (Concentration), H Gamma Line, Stellar Luminosity, Stellar Models, Stellar Winds

Scientific paper

Spectral observations of the eclipsing binary star V 367 Cygni are reported. The structure of the spectrum is found to be of the envelope type having emission in the N alpha-H gamma lines. The Mg II line at 4481 A, as well as the wings of the hydrogen lines were found exclusively in the primary star. The structure and velocity of the motion of the gaseous medium in V 367 Cygni were studied on the basis of the mission components of the H gamma line. A gas stream from the secondary component was observed passing through the Lagrangian point L(1). No variation in the equivalent line widths and electron densities were detected in relation to the period of revolution of the star. The average electron densities were n(e) m = 13.26 + or - 0.35 and log n(e) H delta = 14.36 + or - 0.21. The outflow of material from V 367 Cygni was estimated near 0.0000323 solar mass/yr. A line drawing showing the structure of the stellar envelope is provided.

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