Open AccessThe physical nature of the short‐period RS CVn system DV Psc
Author(s) -
Zhang X. B.,
Zhang R. X.
Publication year - 2007
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2007.12293.x
Subject(s) - physics , light curve , photometry (optics) , orbital period , astrophysics , ephemeris , mass ratio , radial velocity , contact binary , orbital inclination , binary star , binary number , amplitude , astronomy , stars , optics , satellite , arithmetic , mathematics
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 0.308 536 09 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 2.038 R ⊙ . The masses and radii for the components are determined as 0.70 ± 0.02 M ⊙ , 0.68 ± 0.03 R ⊙ for the primary, and 0.49 ± 0.01 M ⊙ , 0.51 ± 0.02 R ⊙ for the secondary.