Abstract
Theoretical chromospheric models described in the two previous papers of this series are used to study the relationship between the chromospheric emission and the lling factor. This theoretically determined rela- tionship shows that the chromospheric emission flux in Ca II (H+K) is approximately proportional to the square root of the magnetic lling factor at the stellar surface. To relate the lling factor to stellar rotation rate, we compare the theoretical fluxes with observations of stars with known rotation period. The comparison shows that the Rossby number is probably a more appropriate measure of the rotation influence on activity of main-sequence stars than the rotation period. Our theoretical Mg II (h+k) and Ca II (H+K) emission fluxes are also found to be well correlated, which is in a good agreement with the observational data.
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