The low mass ratio contact binary system V728 Herculis

Abstract

We present the orbital period study and the photometric analys of the contact binary system V728 Her. Our orbital period analysis shows that the period of the system increases (dP/dt=1.92x10^-7dyr^-1) and the mass transfer rate from the less massive component to more massive one is 2.51x10^-8M_suny^-1. In addition, an advanced sinusoidal variation in period can be attributed to the light-time effect by a tertiary component or the Applegate mechanism triggered by the secondary component. The simultaneous multicolor BVR light and radial velocity curves solution indicates that the physical parameters of the system are M1=1.8M_sun, M2=0.28M_sun, R1=1.87R_sun, R2=0.82R_sun, L1=5.9L_sun, and L2=1.2L_sun. We discuss the evolutionary status and conclude that V728 Her is a deep (f=81%), low mass ratio (q=0.16) contact binary system.

21 pages, 4 figures, 4 tables

References in corpus (3)

• On the origin of W UMa type Contact binaries - a new method for computation of initial masses
• Period changes in six contact binaries: WZ And, V803 Aql, DF Hya, PY Lyr, FZ Ori, and AH Tau
• On the minimum mass ratio of W UMa binaries

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• New low mass ratio contact binaries in the Catalina Sky Survey
• TY Pup: a low-mass-ratio and deep contact binary as a progenitor candidate of luminous red novae
• NSVS 2569022: a peculiar binary among the W UMa stars with extremely small mass ratios