Abstract
Stellar magnetic activity can be characterized by a chaotic, multiple or single cycle behavior. Sometimes cyclic activity can be interrupted by a flat behavior. The mechanism that produce such a diverse behavior in stellar atmosphere is a matter of debate. We decided to address this issue by investigating the properties of a sample of 40 stars with high quality cycles, selected from the original data provided by the Mount Wilson Observatory. This sample contains stars with single and secondary cycles, whose secondary periods are longer or shorter than the primary cycle.
Highlights
Long term observations of solar type stars [1] has revealed a pattern of correlated changes between rotation rates and chromospheric activity
The role played by the different component of the magnetic dynamo configuration has been suggested recently as a possible mechanism to explain the presence of the quasi-biennial periodicity (QBP) in helioseismic and solar activity proxies [5]
We have shown that stars showing secondary cycles mainly are younger than the ones showing only strict cycles
Summary
Long term observations of solar type stars [1] has revealed a pattern of correlated changes between rotation rates and chromospheric activity. Young stars shows high rotation rates, high activity levels and chaotic behavior in their stellar magnetic activity. Shows instead moderate levels of activity and rotation rates, and sometimes smooth cycles. Stars as old as the Sun shows slow rotation rates, low activity levels and cycles interrupted by flat behavior. The role played by the different component of the magnetic dynamo configuration has been suggested recently as a possible mechanism to explain the presence of the quasi-biennial periodicity (QBP) in helioseismic and solar activity proxies [5]. Wonder if this mechanism might be at the origin of the observed multiple magnetic cycles in some stars
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