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

Michel, Raul; Acerbi, Francesco; Barani, Carlo; Martignoni, Massimiliano
eprint arXiv:1902.04158


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 $q=2.507 \pm0.006$ and a fill out of $f= 13.6 \pm0.4\%$. 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.