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The physical nature of the short-period RS CVn system DV Psc
We present multicolour CCD photometry of the short-period RS CVn-typebinary DV Psc obtained in 2006 September and October. Our observationsindicate that GSC0008-789, the comparison star used by Robb et al. intheir discovery of DV Psc, is a variable with amplitude exceeding 0.08mag. Based on the new data, the orbital period of the eclipsing systemis revised to 0.30853609 d. From the new observations, a set ofcompletely covered B, V and R light curves and a single V-band lightcurve are formed in two epochs. The radial-velocity curves obtained byLu, Rucinski & Ogloza are reformed with the newly determinedephemeris and are analysed along with the light curves using the 2003version of the Wilson-Devinney code. The results show that DV Psc is adetached, near-contact binary system with a mass ratio of 0.693 +/-0.005 and a separation of 2.038Rsolar. The masses and radiifor 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.
| Photometric study of neglected binary DV Psc
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| Photometry of the Eclipsing Binary Star GSC 0008 324 = 1RXS J001309+053550
GSC 0008 324 is a near contact eclipsing binary star with deep eclipsesand an orbital period of 0.30855 days.
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