Abstract
SV Centauri is an early-type contact binary for which detailed physical data have been obtained from observations (Wilson and Starr 1976). The orbital period is p = 1.659 days and the separation is a = 16.1 R⊙. The radii of component Stars A and B are, respectively, R = 7.2 and 6.9 R⊙ so that they are in overcontact. The masses and the luminosities are M = 11.1 and 9.3 M⊙, and L = 2830 and 10900 L⊙ for Stars A and B, respectively. The more massive Star A is called the primary star but its luminosity is fainter than Star B. This implies that it is in the phase of rapid mass transfer and mass is outflowing from Star A. Indeed one of the most interesting and important points of this system is that the rate of period change is measured to be dP/dt = −9.4 × 10−8 (Irwin and Landolt 1972) which corresponds to the mass transfer rate of dMA/dt = −4 × 10−4 M⊙ yr−1.
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