The Elliptic Orbit of the WR Binary System CV Serpentis

Details The Elliptic Orbit of the WR Binary System CV Serpentis The Elliptic Orbit of the WR Binary System CV Serpentis

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996rmxac...5..100n&link_type=abstract

Workshop on Colliding Winds in Binary Stars to Honor Jorge Sahade, vol. 5, p. 100

Computer Science

5

Elliptical Orbits, Binary Stars, Orbit Calculation, Orbital Position Estimation, Binary Data, Argentina, Charge Coupled Devices, Early Stars, Eccentricity, Emission Spectra, Line Spectra, Radial Velocity, Spectrograms, Spectroscopy

Scientific paper

We have made a new determination of the orbital parameters of the WC8+08-9 binary system CV Serpentis (HD 168206), through the analysis of spectroscopic observations obtained at CTIO (Chile) and CASLEO (Argentina), together with previously published data. The period that best fits the radial velocity variations of both the Wolf-Rayet emission lines and the O-type absorption lines, is 29.704 days. The curve of the radial velocity variations of the absorption lines shows an eccentricity of 0.19 +/- 0.03, not noticed in previous studies of this binary system. In recent echelle CCD spectrograms obtained at CASLEO, the shape of the absorption line profiles appears complex, suggesting that probably more than one early type star might be present in the system.

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