The physical nature of the short-period RS CVn system DV Psc

Details The physical nature of the short-period RS CVn system DV Psc The physical nature of the short-period RS CVn system DV Psc

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007mnras.382.1133z&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 382, Issue 3, pp. 1133-1138.

Astronomy and Astrophysics

Astronomy

4

Stars: Activity, Binaries: Eclipsing, Stars: Individual: Dv Psc, Stars: Late-Type

Scientific paper

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.

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