New spectral observations of the interacting eclipsing binary V367 Cygni

Details New spectral observations of the interacting eclipsing binary V367 Cygni New spectral observations of the interacting eclipsing binary V367 Cygni

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998arep...42..494t&link_type=abstract

Astronomy Reports, Volume 42, Issue 4, July 1998, pp.494-500

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The results of high-dispersion CCD spectral observations of the interacting eclipsing binary V367 Cyg near the HeI 6678 Angstrom, MgII 4481 Angstrom, SiII 6347 Angstrom, and Hα lines are presented. Faint emission in the HeI 6678 Angstrom line was detected. The radial velocity derived from this emission varies with a half-amplitude of about 180km/s, and is in antiphase with the variations of the MgII 4481 A line, which is formed in the photosphere of the primary star. It is concluded that the He I emission is formed in the accretion disc around the invisible companion. A simultaneous solution for the orbital radial-velocity variability curves (taking into account the inclination angle of the orbit, determined previously from polarimetric observations), results in estimates for the masses of the two components M_1 22 M_solar and M_2 11 M_solar. New orbital elements for the binary are determined. Long-term variability in the radial velocity of the system's center of mass was also discovered. The variability of the HeI 6678 Angstrom, SiII 6347 Angstrom, and Hα line profiles are used to analyze the behavior of gas flows in the system. V367 Cyg appears to be in an initial phase of rapid mass transfer, when matter flows from the more massive onto the less massive component.

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