The Sun and other stars are magnetic: magnetism pervades their interiors and affects their
evolution in a variety of ways. In the Sun, both the fields themselves and their influence on …

The review considers the modelling process for stellar convection rather than specific
astrophysical results. For achieving reasonable depth and length we deal with …

Numerical solutions of partial differential equations enable a broad range of scientific
research. The Dedalus project is a flexible, open-source, parallelized computational …

Both observations and numerical simulations are discordant with predictions of conventional
stellar evolution codes for the latest stages of a massive star's life before core collapse. The …

The observational absence of giant convection cells near the Sun's outer surface is a long-
standing conundrum for solar modelers. We herein propose an explanation. Rotation …

There is considerable interest in hydrodynamic instabilities in dead zones of protoplanetary
disks as a mechanism for driving angular momentum transport and as a source of particle …

The Sun's axisymmetric large-scale flows, differential rotation and meridional circulation, are
thought to be maintained by the influence of rotation on the thermal-convective motions in …

On Differential Rotation and Overshooting in Solar-like Stars - IOPscience This site uses
cookies. By continuing to use this site you agree to our use of cookies. To find out more, see …

The extent of mixed regions around convective zones is one of the biggest uncertainties in
stellar evolution. One-dimensional overshooting descriptions introduce a free parameter (f …

The cores of main sequence intermediate-and high-mass stars are convective. Mixing at the
radiative–convective boundary, waves excited by the convection, and magnetic fields …