Abstract
ABSTRACT Spectroscopy and photometry are used to show that MR Persei, an object originally classified as a dwarf nova, is in fact a flare star. The automated CCD photometry consists of sequences of exposures within a single night as well as long-term photometry over a 5-month interval. One sequence shows a 30-minute flare, accompanied by post-flare "dips." A 0.2 mag variation with a period of about one-half day is also seen in this sequence. The long-term photometry is used to refine the period to 0.45483d, which we attribute to the rotation of a spotted star. Evidence for membership of MR Per in the young alpha Per cluster is considered, and found to be inconclusive.
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