RZ Dra
Kreiner1994 - Kreiner1994V (Johnson V)
The spectroscopic mass ratio used is that of Rucinski et al. (2000). The initial parameters and light curves were taken from Kreiner et al. (1994) but I changed the system into a contact system in order to fit the shape of the light curves. The only way to fit the eclipse depths was to increase the limb darkenings of both stars in both bandpasses. For the larger, hotter star (star #1) the values of the limb darkening went from 0.661 to 0.88 in B and from 0.538 to 0.78 in V. For the smaller, cooler star (star #2) the values of the limb darkening went from 0.891 to 0.93 in B and from 0.734 to 0.87 in V. The fits were done by eye and not by differential corrections.