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In this study, new observations and some results of statistical analyses arepresented. The largest flare data set of DO Cep in the literature has beenobtained with 89 flares detected in 67.61 hours of U-band flare patrol. Firstof all, the observations demonstrated that the star is one of the most activeflare stars in respect to the computed flare frequency. Secondly, using theindependent samples t-test, the detected flares were classified into twosubtypes, and then they were modelled. Analysing the models demonstrated thatthe fast and slow flares occurring on the star can be separated with a criticalvalue of the ratio of their decay time to rise time. The critical value wascomputed as 3.40. According to this value, the fast flare rate is 20.22%, whilethe slow flare rate is 79.78%. Besides, there is a 39.282 times differencebetween the energies of these two types of flares. However, the flareequivalent durations versus the flare rise times increase in similar ways forboth groups. In addition, all all the flares were modelled with the one-phaseexponential association function. Analysing this model, the plateau value wasfound to be 2.810. Moreover, the half-life value was computed as 433.1s fromthe model. The maximum flare rise time was found to be 1164s, while the maximumflare total duration was found to be 3472s. The results of the flare timescalesindicate that the geometry of the flaring loop on the surface of the star mightbe similar to those seen on analogues of DO Cep. Consequently, considering boththe half-life value and flare timescales, the flares detected on the surface ofDO Cep get maximum energy in longer times, while the geometries of the flaringloops or areas get smaller.

Statistical Analysis and the OPEA Model of the White-Light Flares Occurring on Kr\"uger 60B (DO Cep)