Predicting the length of magnetic cycles in late-type stars

In this paper we present a modification of a local approximation of the so-called interface dynamo in an attempt to reproduce the length of the magnetic cycles for a sample of late-type stars. The sample consists of 25 stars, observed during the MountWilson and Las Campanas long-term monitoring campaigns, for which well-defined cycles have been detected. We have focused our efforts on reproducing general trends observed, namely, the dependence of the cycle length, P-cyc, on the stellar rotation period, Prot, rather than attempting to infer from the dynamo model individual cycle lengths for each star. In spite of the simplicity of the model, the results are promising. The trend of increasing cycle length with increasing rotation period is reproduced with a minimum of assumptions.