Long-Term Cyclic Variability of YZ CMi in the Context of Solar and Stellar Physics

Abstract

Manifestations of activity on the YZ CMi (M4.5Ve) flare star which has a rotation period of 2.77 days and belongs to a group of activity-saturated stars, are considered from long-term photometric data together with photographic measurements from 1926 to 2009. Long-term changes in yearly mean brightness of the star are found on a time scale of 27.5 years with an amplitude of $0.2-0.3^m$ that indicate variations in development of surface inhomogeneities and a large degree of surface spottedness in the maximum activity. Spots are distributed unevenly over the surface, their concentration is higher at certain longitudes spaced by intervals equal to 0.6 phases of the rotation period. The recovery of active longitude (a possible "flip-flop" effect) occurs over a period of about 6 years. We note differences in activity of this star from typical for the Sun and solar-like stars, which are associated with its dynamic characteristics $P_{cyc}$ and $P_{rot}$ and its inner structure.

Corrected version. 8 pages, 5 color figures

References in corpus (6)

• The First Direct Measurements of Magnetic Fields on Very Low-Mass Stars
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