The Doppler images were produced using maximum entropy regularisation, fitting geometrical and orbital parameters of the contact binary at the same time as spots using both the spectroscopic and photometric data to constrain the models. Spots were modeled as being 3500 K in temperature, fractionally covering each surface element of the system to different amounts. These models fitted the observational data very well.
The Doppler images indicated the presence of large polar spots on both components. The polar spot on the primary was about 50° in diameter, and was slightly off-centre, while that on the secondary was 30° in diameter and somewhat tenuous. A number of lower latitude features were also present. Spots on the primary were found to migrate around in the direction of the orbital motion in the system. Differential rotation of the primary component was observed, with spots at higher latitudes moving at higher angular rates. The spot distribution on the secondary appeared to be quite stable, with spots congregating at active longitudes, and no organised pattern of migration was observed.
The spot coverage on both components was extremely high. Spots covered 66% of the surface area of the primary and 55% of the secondary. The spot model was modeled after the Mullan (1975) starspot model, but was in agreement with the hot secondary model, since the bolometric flux weighted mean surface temperature of the primary was less than that of the secondary, due to the large numbers of spots.
Page current as of Dec. 16, 1996. Not to be updated.