A spectroscopic study of the eclipsing binaries SV Camelopardalis and XY Ursae Majoris

High-resolution spectroscopic observations of the eclipsing RS CVn-type act ive close binaries SV Camelopardalis and XY Ursae Majoris reveal excess emi ssion components in the Ha and Ha lines. We have used the spectral subtract ion technique to separate the excess emission from the photospheric backgro und and find that in both stars the excess emission is associated with the secondary, cooler component. Analysis of the EWH alpha/EWH beta ratio indic ates that in both cases the emission is probably associated with surface pl age regions or prominences viewed against the stellar disks. We find no evi dence of excess absorption features associated with extended prominence-lik e material in these systems.