S.-B. Qian

TL;DR: In this article, the authors used the century-long historical record of the times of light minimum to analyze the cyclic period change in the Algol binary WW Dra and found that the orbital period of the binary shows a similar to 112.2-yr cyclic variation with an amplitude of similar to 0.1977 d. The cyclic oscillation can be attributed to the LTTE by means of a third body with a mass no less than 6.43M.

TL;DR: In this paper, the spectral properties of 5363 EW-type binary stars were determined based on good spectroscopic observations and their properties were analyzed and the correlations between the orbital period and the effect temperature, the gravitational acceleration and the metallicity are presented and their scatters are mainly caused by (i) the presence of the third bodies and (ii) the wrong determined periods sometimes.

TL;DR: In this paper, a charge-coupled device photometric observations of the W UMa-type binary star UX Eridani were presented, which confirmed that UX Eri is a marginal W-type overcontact binary system with a very low degree of overcontact, f 44.5 circle dot.

TL;DR: In this article, the authors analyzed the orbital period variations of two O-type overcontact binary stars, V382 Cyg and TU Mus, and found that the periods of both binaries show cyclic oscillations with periods of 47.70 and 47.73 yr, respectively.

TL;DR: In this paper, a detailed O-C analysis for both CVs inside the period gap is made, showing that the observed cyclical period changes in UZ Fornacis, both mechanisms of magnetic activity cycles in the late-type secondary and the light travel-time effect are two probable causes.