Abstract
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.
