The physical nature of the short-period RS CVn system DV Psc
Abstract
We present multicolour CCD photometry of the short-period RS CVn-type binary DV Psc obtained in 2006 September and October. Our observations indicate that GSC0008-789, the comparison star used by Robb et al. in their discovery of DV Psc, is a variable with amplitude exceeding 0.08 mag. Based on the new data, the orbital period of the eclipsing system is revised to 0.30853609 d. From the new observations, a set of completely covered B, V and R light curves and a single V-band light curve are formed in two epochs. The radial-velocity curves obtained by Lu, Rucinski & Ogloza are reformed with the newly determined ephemeris and are analysed along with the light curves using the 2003 version of the Wilson-Devinney code. The results show that DV Psc is a detached, near-contact binary system with a mass ratio of 0.693 +/- 0.005 and a separation of 2.038Rsolar. The masses and radii for the components are determined as 0.70 +/- 0.02Msolar, 0.68 +/- 0.03Rsolar for the primary, and 0.49 +/- 0.01Msolar, 0.51 +/- 0.02Rsolar for the secondary.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- December 2007
- DOI:
- 10.1111/j.1365-2966.2007.12293.x
- Bibcode:
- 2007MNRAS.382.1133Z
- Keywords:
-
- stars: activity;
- binaries: eclipsing;
- stars: individual: DV Psc;
- stars: late-type