Abstract
The faint RS CVn system SS Bootis was observed over two seasons, and the most prominent surface activity indicators in this spectroscopically understudied object were examined. The first two Balmer lines are consistently strong in emission, as are the Ca II infrared triplet and Ca II H line; there is no significant modulation with phase in any of these lines. No excess emission is evident in He I D3. The ratio of energy emitted in H-alpha to that in H-beta is typically between three and six for the more active subgiant primary, and between two and five for the dwarf secondary. Of special interest is an excess absorption feature in the Balmer lines near primary eclipse in both seasons. The feature lies near the velocity of the secondary, and as there is no similar feature in secondary eclipse, it is suggested that it arises from obscuring material associated with the primary. From the extent of the feature and the system's geometry, limits were placed on the parameters of such material.