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

Abstract

In this study, a new method is presented to classify flares derived from the photoelectric photometry of UV Ceti type stars. This method is based on statistical analyses using an independent samples t-test. The data used in analyses 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, EQ Peg, and V1054 Oph is 321 in the standard Johnson U band. As a result flares can be separated into two types, slow and fast, depending on the ratio of flare decay 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 independent samples t-test, there is a difference of about 157 s between equivalent durations of slow and fast flares. In addition, there are significant differences between amplitudes and rise times of slow and fast flares.

46 pages, 7 figures, 4 tabels, 2010AJ....140..483D

References in corpus (4)

• Late-type stars members of young stellar kinematic groups - I. Single stars
• Analysis and modeling of high temporal resolution spectroscopic observations of flares on AD Leo
• Studies of multiple stellar systems - IV. The triple-lined spectroscopic system Gliese 644
• Spatially resolved X-ray emission of EQ Pegasi

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