A study of the MgII 2796.34 Å emission line in late-type normal and RS CVn stars

We carry out an analysis of the Mg II 2796.34 Angstrom emission line in RS CVn stars and make a comparison with the normal stars studied in a previous paper ( Paper I). The sample of RS CVn stars consists of 34 objects with known HIPPARCOS parallaxes and observed at high resolution with IUE. We confirm that RS CVn stars tend to possess wider Mg II. lines than normal stars having the same absolute visual magnitude. However, we could not find any correlation between the logarithmic line width log W-o and the absolute visual magnitude M-V (the Wilson-Bappu relationship) for these active stars, contrary to the case of normal stars addressed in Paper I. On the contrary, we find that a strong correlation exists in the (M-V, log L-MgII) plane (L-MgII is the absolute flux in the line). In this plane, normal and RS CVn stars are distributed along two nearly parallel straight lines with RS CVn stars being systematically brighter by approximate to1 dex. Such a diagram provides an interesting tool to discriminate active from normal stars. We finally analyse the distribution of RS CVn and of normal stars in the (log L-MgII, log W-o) plane, and find a strong linear correlation for normal stars, which can be used for distance determinations.