The spottedness of two stars characterized by significant photometric variability is studied using published data: the recently discovered variable ASAS 063656-0521.0, whose V variability reaches 0.8 (m) , and XXTri (HD12545), which is among the most active RSCVn stars (in 1997-1998, the amplitude of its V variability was 0.63 (m) ). The spots cover up to 44% of the total visible surface S of ASAS 063656-0521.0. The mean estimated spottedness of XX Tri was 32%, and varied from29% to 36%. An analysis of the dependence of the spottedness on the properties of spotted stars, primarily their effective temperatures, is also presented. A modification of a simplifiedmethod for estimating the spottedness S, i.e., the fractional surface area of the spots, is applied to a sample of 48 late-type stars. The dependences of the spottedness on the effective temperature of the stars and the rotational velocity projected onto the line of sight are derived. Two groups of objects can be distinguished. The first contains stars displaying the typical dependence of S on the effective temperature (their maximum value of S is 20-25% for stars with temperatures 4500-5000 K, and S decreases for solar-type stars and cool M dwarfs). The second group is formed of the most active stars, which have temperatures of 3700-5200 K and S values from 25% to 50%. Our preliminary conclusion is that spottedness is not related to the period of the stellar rotation. The previously studied variable V410 Tau is used to consider the shortcomings of the method applied compared to the results of light-curve modeling.
