Relating stellar cycle periods to dynamo calculations

Stellar magnetic activity in slowly rotating stars is often cyclic, with the period of the magnetic cycle depending critically on the rotation rate and the convective turnover time of the star. Here we show that the interpretation of this law from dynamo models is not a simple task. It is demonstrated that the period is (unsurprisingly) sensitive to the precise type of non‐linearity employed. Moreover the calculation of the wave‐speed of plane‐wave solutions does not (as was previously supposed) give an indication of the magnetic period in a more realistic dynamo model, as the changes in length‐scale of solutions are not easily captured by this approach. Progress can be made, however, by considering a realistic two‐dimensional model, in which the radial length‐scale of waves is included. We show that it is possible in this case to derive a more robust relation between cycle period and dynamo number. For all the non‐linearities considered in the most realistic model, the magnetic cycle period is a decreasing function of | D | (the amplitude of the dynamo number). However, discriminating between different non‐linearities is difficult in this case and care must therefore be taken before advancing explanations for the magnetic periods of stars.