Other
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.1001s&link_type=abstract
American Astronomical Society, SPD Meeting #31, #10.01; Bulletin of the American Astronomical Society, Vol. 32, p.842
Other
Scientific paper
I explore relationships between the magnetic activity cycle frequency ωcyc, the rotational frequency Ω , and other stellar properties in a large sample of dwarfs, evolved stars, active binaries, and the secondaries of CV systems. The cycles are derived from various sources, including periodicities in Ca ii, photometry, and orbital period changes. Dimensional (ωcyc vs. Ω ) and non-dimensional (ωcyc/Ω vs. Ro-1; where Ro is the Rossby number) parameterizations give similar results. Stars are concentrated on three main ``branches" with different relationships between ωcyc and Ω ; the branches may converge at very short Ω . The oldest, lowest activity stars tend to occupy the branch with the highest ωcyc. Some stars have additional secondary ωcyc (perhaps analogous to the Sun's ``Gleissberg" cycle) lying on other branches; the preferred branch of the primary ωcyc may be mass and Ω dependent. The density of stars along each branch also depends on Ω and hence age, indicating ωcyc evolves in time, but in a complex, sometimes multi-valued fashion. I discuss some possible implications for dynamo theory and evolution. This work is supported by NSF grant AST-9528563.
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