Abstract
The results of applying a method developed by us for determining the spottedness parameter A to data on the brightness variation of 34030 objects based on observations with the Kepler space telescope are presented. An approxmate power law dependence of A on Teff is obtained. Assuming that the empirical relationship between A and the lifetime of a spot (the Gnevyshev-Waldmeier relation) is applicable, the dependence of the spot lifetime for stars with different effective temperatures is constructed and examined. The relationship between the maximum magnetic field H and spot size established for the sun is used to estimate H for the objects studied here. The applicability of solar analogs for analyzing the activity of stars in different spectral classes and the possible similarity of the processes responsible for the activity of these objects is discussed. The results are compared with observational data and possible manifestations of spottedness in hot A stars are examined.
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