Abstract
A study of the relationship between soft X-ray luminosity and Hei 10830 equivalent width in RS CVn binaries and very active late-type Main-Sequence stars is made. Long-period RS CVns and very active F and G Main-Sequence stars show strong dependence on their X-ray luminosities. This is attributed to the dominance of coronal excitation of the line in these stars. Short-period RS CVn binaries have lower Hei 10830 absorption compared to their X-ray emission. This phenomenon is explained by the presence of Hei emission region also in their chromospheres.
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