Computer Science
Scientific paper
Feb 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..672k&link_type=abstract
COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.
Computer Science
Chromosomes, Histones, Stellar Rotation, Stellar Activity
Scientific paper
We analyze the long-term variability of the chromospheric radiation of 20 stars monitored in the course of HK Project. We apply the modified wavelet algorithm for this set of gapped data. Besides the rotational periods for all these stars, we find reliable changes of the periods from year to year for a few stars. Epochs of the slower rotation occur when the activity level of the star is high, and they come again during the next maximum of a cycle. Such an effect is traced in two ``Good'' stars, whose cycles are not quite regular, but they are more active than the Sun. So, the mean period of rotation of the star HD 115404 is 18.5 days, and sometimes it does increase up to 21.5 days. The sign of the differential rotation is the same as one for the Sun, and ΔΩ/<Ω> = -0.14. For the star HD 149661, this ratio is -0.074. Characteristic changes of rotational periods occur over around three years when the amplitude of the rotational modulation is large. These changes can be transformed into the butterfly diagrams without a priori assumptions. We compare these results with those for the Sun as a star and conclude that epochs when surface inhomogeneities rotate slower are synchronous with reversal of the global magnetic dipole.
Katsova M. M.
Livshits Moisey A.
Sokoloff Dimitry
Soon Willie
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