Speaker
Mr
Felix Sainsbury-Martinez
(University of Exeter)
Description
Low-Mass stars are typically fully convective, and as such their dynamics may differ significantly from sun-like stars. Here we present a series of 3D anelastic simulations of fully convective stars, designed to investigate how the meridional circulation, the differential rotation, and entropy are affected by varying stellar parameters, such as the luminosity or the rotation rate. We also investigate, more specifically, a theoretical model in which isorotation contours and residual entropy ($S' = S - S_{r}$) are intrinsically linked via the thermal wind equation (as proposed in the Solar context by Balbus 2009). We have selected our simulation parameters in such as way as to span the transition between Solar-like differential rotation (fast equator + slow poles) and "anti-Solar" differential rotation (slow equator + fast poles), as characterised by the convective Rossby number and $\Delta\Omega$. We illustrate the transition from single-celled to multi-celled MC profiles, and from positive to negative latitudinal entropy gradients. We find generally poor correlation between the residual entropy profile and the isorotation contours, suggesting that the link between these quantities is not as strong as suggested by some previous models.
Author
Mr
Felix Sainsbury-Martinez
(University of Exeter)
Co-author
Dr
Matthew Browning
(University of Exeter)
