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The relation between stellar rotation rate and activity cycle periods
Noyes, R. W.; Weiss, N. O.; Vaughan, A. H.
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AC(Mount Wilson and Las Campanas Observatoires, Washington, DC; Perkin-Elmer Corp., Garden Grove, CA)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 287, Dec. 15, 1984, p. 769-773. Research supported by the National Geographic Society. (ApJ Homepage)
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NASA/STI Keywords:
Angular Velocity, Dynamo Theory, Main Sequence Stars, Periodic Variations, Stellar Activity, Stellar Rotation, Stellar Spectra, Chromosphere, Data Correlation, Stellar Atmospheres, Stellar Magnetic Fields, Stellar Models
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The empirical relation between rotation period, spectral type, and cycle activity period in 13 slowly rotating main-sequence stars is investigated, on the basis of available spectrometric data. It is shown that for slowly rotating stars with similar spectral types, the cycle period P(cyc), and rotation period P(rot) were related such that P(cyc) varies as P(rot) to the nth, where n equals 1.25. In a group of stars with individual spectral types from G2 to K7, the cycle periods were consistent with the relation P(cyc) is approximately equal to (P rot/tauc) exp n, where tauc is the convective turnover time near the bottom of the convection zone. On the basis of the above relations, it is suggested that an increase of P(cyc) with increasing P(rot) does not agree with conventional estimates from nonlinear dynamo models, and is limited by two factors: the quenching of the alpha effect; and differential rotation.

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