An Orbital Period Investigation of the Semi-Detached Near-Contact Binary DD Monocerotis

Details An Orbital Period Investigation of the Semi-Detached Near-Contact Binary DD Monocerotis An Orbital Period Investigation of the Semi-Detached Near-Contact Binary DD Monocerotis

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009pasj...61..333q&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.61, No.2, pp.333--337

Astronomy and Astrophysics

Astronomy

4

Stars: Binaries: Close, Stars: Binaries: Eclipsing, Stars: Individual (Dd Monocerotis), Stars: Stellar Evolution

Scientific paper

The variations of the orbital period of the near-contact binary system DD Monocerotis were analyzed based on three new CCD times of light minimum together with others compiled from the literature. The general trend of the (O - C)1 curve indicates a continuous period increase at a rate of dP/dt = +1.40 × 10-7dyr-1. Meanwhile, by using all available photoelectric and CCD data, a small-amplitude period oscillation (A = 0.0039d; T = 18.8yr) was found to be superimposed on the period increase. The continuous period increase is explained by mass transfer from the less-massive component to the more-massive one (dM2/dt = +6.99 × 10-8Modotyr-1), which is consistent with the semi-detached configuration of the binary with a lobe-filling secondary discovered by Qian et al. (1997, A&AS, 125, 475). We showed that the timescale of the period change is close to the thermal time scale of the secondary, suggesting that DD Monocerotis is undergoing a case A mass transfer. The small-amplitude period oscillation reveals the presence of an extremely cool stellar companion (M3sin i' = 0.13Modot) in the system. Accumulation of photoelectric and CCD data will discover small-amplitude cyclic changes in many close binary stars in the future.

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