No abstract

No abstract

In this study complete BV light curves of the W Ursae Majoris binary V1073 Cygni obtained in 2005 are presented. We have used the spectroscopic data of V1073 Cyg obtained by Ahn et al. (1992) for analysis. The analysis of radial velocity and light curves was made with Wilson program (1998) and the geometric and physical elements of the system were derived. By searching the simultaneous solutions of the system, we have determined the masses and radii of the components: 1.64M , 2.275R for the primary component and 0.55M , 1.397R for the secondary component respectively. The effective temperature of 6494 ± 53 (K) for the secondary component was also estimated.

Abstract. New radial velocity measurements of the Algol-type eclipsing binary BD +52 °2009, based on Reticon observations, are presented. The velocity measures are based on fitting theoretical profiles, generated by a physical model of the binary, to the observed cross-correlation function (ccf). Such profiles match this function very well, much better in fact than Gaussian profiles, which are generally used. Measuring the ccf's with Gaussian profiles yields the following results: m p sin 3 i = 2.55 ± 0.05m @ , m s sin 3 i = 1.14 ± 0.03m @ , (a p + a s ) sin i = 7.34 ± O.O5i? 0 , and m p /m s = 2.23 ± 0.05. However, measuring the ccf's with theoretical profiles yields a mass ratio of 2.33 and following results: m p sin 3 i = 2.84 ± 0.05m®, m s sin 3 i = 1.22 ± O.O3m 0 , (a p + a s ) sin i = 7.56 ± 0.05R @ . The system has a semi-detached configuration. By combining the solution of a previously published light curve with the spectroscopic orbit, one can obtain the following physical parameters: m p = 2.99m @ , m 3 = 1.28m0, < T p >= 9600K, < T s >= 5400K, < R p >= 2.35i? 0 , < R s >= 2.12R®. The system consists of an A0 primary and a G2 secondary.