This paper reviews the remarkable developments in numerical geodynamo simulations over
the last few years. Simulations with Ekman numbers as low as E= 10− 8 E= 10− 8 are now …

We present an attempt to reach realistic turbulent regime in direct numerical simulations of
the geodynamo. We rely on a sequence of three convection-driven simulations in a rapidly …

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 …

Precession of planets or moons affects internal liquid layers by driving flows, instabilities and
possibly dynamos. The energy dissipated by these phenomena can influence orbital …

Dynamic modeling of sequences of earthquakes and aseismic slip (SEAS) provides a self‐
consistent, physics‐based framework to connect, interpret, and predict diverse geophysical …

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 …

Precession of planets or moons affects internal liquid layers by driving flows, instabilities and
possibly dynamos. The energy dissipated by these phenomena can influence orbital …

Bottom-heated convection in rotating spherical shells provides a simple analogue for many
astrophysical and geophysical fluid systems. We construct a database of 74 three …

We present a set of numerical simulations that model the convection zones of solar-like
stars. With this suite of numerical experiments, we explore how the nature of the convective …

We explore how thermal Rossby waves propagate within the gravitationally stratified
atmosphere of a low-mass star with an outer convective envelope. Under the conditions of …