A study of short-period RS Canum Venaticorum and W Ursae Majoris binary systems - The global nature of H-alpha

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Abstract
The author presents the rotation versus emission characteristics of the Hα line for several short-period (P ⪉ 1d) RS CVn and W UMa binary systems. Estimates for the chromospheric emission arising from each component star were obtained by subtraction of "nonactive" model spectra constructed from comparison stars. Enhanced Hα emission compared to the nonactive comparison stars is seen on all components of the short-period RS CVn systems studied, while a similar enhancement is only typically seen on the primary components of the W-type W UMa systems. A possible correlation between LHα/Lbol and the Rossby number (the ratio between the rotational period and the convective time scale) is seen for those components showing emission.

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