双星与变星研究组知识库

New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f similar to 11% and a high mass ratio q similar to 1.587 (1/q = 0.63), where the hotter component is the less massive one (M-1 similar to 0.52 M-circle dot and M-2 similar to 0.82 M-circle dot). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O - C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = -9.61 x 10(-9) d yr(-1) is superimposed on a cyclic variation (A(3) = 0.0054 d and P-3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deeper normal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.