UV鲸鱼座型星耀斑分类的新方法：慢耀斑和快耀斑的区别
A New Method for Classifying Flares of UV Ceti Type Stars: Differences Between Slow and Fast Flares
摘要：
在这项研究中，提出了一种新的方法来分类耀斑的紫外鲸鱼座型恒星的光电测光。该方法基于使用独立样本t检验的统计分析。分析中使用的数据来自2004年至2007年期间观察到的四颗耀斑星。AD Leo、EV Lac、EQ Peg和V1054 Oph的观测中获得的耀斑总数在标准Johnson U波段为321。因此，耀斑可以分为两种类型，慢和快，这取决于耀斑衰减时间与耀斑上升时间的比值。所有慢耀斑的比率都低于3.5，而所有快耀斑的比率都高于3.5。根据独立样本t检验，慢耀斑和快耀斑的等效持续时间相差约157 s。此外，慢耀斑和快耀斑的振幅和上升时间也有显著差异。
英文摘要：
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.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
