V1010 Oph
Leung1974 - Leung1974B (Johnson B)
This system has a confusing analytical history, and its true nature is uncertain. It has been modeled as both an overcontact system (Leung & Wilson (1977)) and a near contact system (Cocoran, Siah & Guinan (1991)). The obviously large temperature difference between the two stars lends much more credence to the near contact scenario, although I would argue that it is just as likely to be in a contact configuration (fillout = 0.00). The consistently higher maximum following primary eclipse is most likely due to an impact stream and hence a hot spot rather than a cool spot. Most cool spots (likely magnetic in origin) come and go, whereas the various light curves of V1010 Oph (Leung (1974), Guinan (1970) and Cocoran Siah & Guinan (1991)) all have the higher maximum following primary eclipse.
The model presented is a near contact configuration with most of the parameters taken from Cocoran, Siah & Guinan (1991). However, since their data was unavailable, I used the B&V light curves from Leung (1974). The resulting fit involves a slightly larger mass ratio and somewhat different hot spot than in Cocoran, Siah & Guinan, but not drastically different. Hopefully the data in that paper can be located someday for comparison with that of Leung…
Radial velocity measurements are from Guinan & Koch (1977), B & V light curves from Leung (1974).