Rossby numbers of convective stars

The problem is that the canonical place where {tau}_c_ is usually determined (half a mixing length above the base of the convective zone) fails for fully convective stars and there is no agreement on this in the literature.

Our calculations were performed with the ATON stellar evolution code. We concentrated our analysis on fully and partially convective stars motivated by recent observations of slowly rotating fully convective stars, whose X-ray emissions correlate with their Rossby numbers in the same way as in solar-like stars, suggesting that the presence of a tachocline is not required for magnetic field generation. We investigate the behaviour of {tau}_c_ over the stellar radius for stars of different masses and ages.