The solar tachocline is an internal region of the Sun possessing strong radial and latitudinal
shears straddling the base of the convective envelope. Based on helioseismic inversions …

A major outstanding problem in solar physics is the confinement of the solar tachocline, the
thin shear layer that separates nearly solid-body rotation in the radiative interior from strong …

With an emphasis on numerical modelling, Physics of the Sun: A First Course presents a
quantitative examination of the physical structure of the Sun and the conditions of its …

Context. The internal rotation of the Sun constitutes a fundamental constraint when
modelling angular momentum transport in stellar interiors. In addition to the more external …

We recently presented the first 3D numerical simulation of the solar interior for which
tachocline confinement was achieved by a dynamo-generated magnetic field. In this follow …

We present MAESTROeX, a massively parallel solver for low Mach number astrophysical
flows. The underlying low Mach number equation set allows for efficient, long-time …

Rossby and Magnetic Prandtl Number Scaling of Stellar Dynamos - IOPscience This site uses
cookies. By continuing to use this site you agree to our use of cookies. To find out more, see …

Context. Some contracting or expanding stars are thought to host a large-scale magnetic
field in their radiative interior. By interacting with the contraction-induced flows, such fields …

The propagation of meridional circulation below the base of the convection zone (CZ) of low-
mass stars may play a crucial role in the transport of angular momentum and also …

Motivated by the dynamics in the deep interiors of many stars, we study the interaction
between overshooting convection and the large-scale poloidal fields residing in radiative …