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In this study, a new method is presented to classify flares derived from thephotoelectric photometry of UV Ceti type stars. This method is based onstatistical analyses using an independent samples t-test. The data used inanalyses were obtained from four flare stars observed between 2004 and 2007.The total number of flares obtained in the observations of AD Leo, EV Lac, EQPeg, and V1054 Oph is 321 in the standard Johnson U band. As a result flarescan be separated into two types, slow and fast, depending on the ratio of flaredecay time to flare rise time. The ratio is below 3.5 for all slow flares,while it is above 3.5 for all fast flares. Also, according to the independentsamples t-test, there is a difference of about 157 s between equivalentdurations of slow and fast flares. In addition, there are significantdifferences between amplitudes and rise times of slow and fast flares.

A New Method for Classifying Flares of UV Ceti Type Stars: Differences Between Slow and Fast Flares