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Magnetic fields are at the heart of the observed stellar activity inlate-type stars, and they are presumably generated by a dynamo mechanism at theinterface layer between the radiative and the convective stellar regions. Sincedynamo models are based on the interaction between differential rotation andconvective motions, the introduction of rotation in the ATON 2.3 stellar codeallows for explorations regarding a physically consistent treatment of magneticeffects in stellar structure and evolution, even though there are formidablemathematical and numerical challenges involved. As examples, we presenttheoretical estimates for both the local (tau_c) and global (tau_g) convectiveturnover times for rotating pre-main sequence solar-type stars, based onup-to-date input physics for stellar models. Our theoretical predictions arecompared with the previous ones available in the literature. In addition, weinvestigate the dependence of the convective turnover time on convectionregimes, the presence of rotation and atmospheric treatment. Those estimates,this quantities can be used to calculate the Rossby number, Ro, which isrelated to the magnetic activity strength in dynamo theories and, at least formain-sequence stars, shows an observational correlation with stellar activity.More important, they can also contribute for testing stellar models againstobservations. Our theoretical values of tau_c, tau_g and Ro qualitatively agreewith those published by Kim & Demarque (1996). By increasing the convectionefficiency, tau_g decreases for a given mass. FST models show still lowervalues. The presence of rotation shifts tau_g towards slightly higher valueswhen compared with non-rotating models. The use of non-gray boundary conditionsin the models yields values of tau_g smaller than in the gray approximation.

Theoretical values of convective turnover times and Rossby numbers for solar-like, pre-main sequence stars