Abstract
The problem of the detection or discovery of RS CVn-type close binary systems with the aid of the magnesium emission doublet 2800 Mgii is discussed. On the example of a star, HD 102077, the possibility of such an approach is shown. The determining factor is the magnitude of the measureless parameterR(Mgii), that is, the relative power of the magnesium doublet emission. For the normal Main-Sequence stars the magnesium emission has a purely chromospheric origin andR(Mgii) ∼ 1 (in units of 10−5). However, in the case of close binary systems of RS CVn-typeR(Mgii) ∼ 100. Wit the help of IUE it is foundR(Mgii) ∼ 100 for the star HD 102077 and, therefore, it is identified with RS CVn-type objects in which the magnesium doublet emission is generated in the intercomponent medium by gaseous matter and is transferred from one component of the system to the other. The basic physical parameters of the intercomponent medium in the case of HD 102077 are obtained.
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