Predicting the length of magnetic cycles in late-type stars
Rosario Lorente (ISO Data Center
ESA Satellite Tracking Station
PO Box 50727
E-28080 Madrid Spain
)
Benjamin Montesinos (LAEFF, ESA Satellite Tracking Station, Madrid, Spain)
The long-term monitoring of the variation of the Ca II H
and K emission lines in late-type stars, carried out at Mount Wilson and Las Campanas since 1966, has allowed the detection of activity cycles, similar to the well-known 11-year solar cycle, in some 30 stars.
Some of the most recent models developed to reproduce the different properties of the solar cycle are the so-called interface dynamo models. The newest assumption is that the poloidal and the toroidal fields are generated in different layers, the former in the convection zone and the later in the overshoot region.
We present an interface dynamo model that attempts to reproduce the length of the observed activity cycles in solar-type stars. The model has been used for predicting trends of the magnetic field intensities in the stellar interiors and linking them to the observed magnetic
fluxes fB in these stars.