Multicolor study of V1009 Per, a close binary system at the beginning of the overcontact phase, and of CRTS J031642.2+332639, a new binary system in the same field

Abstract

The first multicolor observations, and light curve solutions, of the eclipsing binary systems V1009~Per and CRTS~J031642.2+332639 are presented. Using the 2005 version of the Wilson-Devinney code, both systems are found to be W UMa contact binaries. V1009~Per has a mass ratio of $q=0.362\pm 0.002$ and a shallow fill out parameter of $f=11.8\pm 0.6\%$ while CRTS~J031642.2+332639 has a mass ratio of $q=2.507\pm 0.006$ and a fill out of $f=13.6\pm 0.4\%$. High orbital inclinations, $i=85^{\circ }.9$ for V1009 Per and $i=83^{\circ }.2$ for CRTS~J031642.2+332639, implies that both systems are total eclipsing binaries and that the photometric parameters here obtained are reliable. Based on 16 times of minimum, the orbital period variations of V1009~Per are discussed. %The estimated physical parameters of V1009 Per are $M_1=0.874M_{\odot },M_2=0.317M_{\odot },R_1=0.865R_{\odot },R_2=0.474R_{\odot },L_1=0.521L_{\odot },L_2=0.153L_{\odot }$. For CRTS J031642.2+332639, the physical parameters are $M_1=1.037M_{\odot },M_2=0.414M_{\odot },R_1=1.002R_{\odot },R_2=0.661R_{\odot },L_1=0.770L_{\odot },L_2=0.370L_{\odot }$. The absolute dimensions of the systems are estimated and, from the logM-logL diagram, it is found that both components of the systems follow the general pattern of the W subtype W Ursae Majoris systems.

12 pages, 7 figures