Analysis and solution of the light and radial velocity curves of the contact binary TY Bootis

Modern comprehensive study of the W UMa system TY Boo

“…A non continuous period variation was announced by Milone et al (1991). They recorded a rapid developing Ca II flares in the system.…”

“…Rainger et al 1990, Milone et al 1991, and Christopoulou et al 2012 showed that the less massive, but hotter, star is eclipsed at the primary minimum. Although the light curve solution by Carr (1972) has a limited accuracy, it suggested that the system TY Boo belong to A-type systems and consists of two mainsequence components with spectral types G3 and G7 and W UMa characteristic with mass ratio of 0.88.…”

“…They confirmed the orbital period change of the system, and calculated the first radial velocities for the system. Photometric and spectroscopic observations were carried out for the system TY Boo by Milone et al (1991) in three observing seasons. They calculated the mass ratio of the system (q = Mh/Mc = 0.465) which is consistent with the value derived using light curve analysis (q = 0.481).…”

Possible Light-Time Effect in the Eclipsing Binary System TY Boo

“…He also determined the spectral types of both components as G3 and G7, and comfirmed the W UMa type variability. Subsequent photometric observations of TY Boo were obtained by Samec and Bookmyer (1987), Samec et al (1989), Rainger et al (1990) and Milone et al (1991). Samec et al (1989) analyzed the Samec and Bookmyer's (1986) light curves using the Wilson-Devinney code and determined the photometric mass ratio as 0.447.…”

“…of Astronomy and Space Sciences, TR-06100, Tandogan, Ankara, Turkey spectroscopic mass ratio of q = 0.437. Milone et al (1991) performed a simultaneous analysis of their new light and radial velocity curves using Wilson-Devinney code and derived the following parameters for the system; M 1 = 1.14 M , M 2 = 0.53 M , i = 77 • .5. Their analysis yielded two spotted regions on the larger component and they noted that the system may contain a chromospherically active star due to the CaII flare observed in the spectrum.…”