Abstract
An equation for determining the magnetic activity cycle for the lower main-sequence stars is derived on the basis of the results of an analysis of magnetic structure drift with the solar activity cycle. The equation correlates the star activity cycle with the period of its rotation Trot, the B−V color index, and the average chromospheric emission level 〈R′HK>. The activity cycles for 30 stars (14 young and 16 old) entering the Wilson sample are calculated. The calculated magnetic activity cycles are found to be in good agreement with the observed ones.
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