2D dynamics of the radiative core of low mass stars

TL;DR

This paper models the 2D internal dynamics of low mass stars' radiative cores under different boundary rotation conditions, revealing shear-induced rotation patterns and discussing implications for seismic observations.

Contribution

It introduces a 2D hydrodynamical model of stellar radiative cores with imposed differential rotation, exploring shear effects on internal rotation profiles.

Findings

Shear induces cylindrical differential rotation patterns.

A single meridional circulation cell forms per hemisphere.

Results inform interpretations of seismic internal rotation measurements.

Abstract

Understanding the internal rotation of low mass stars all along their evolution is of primary interest when studying their rotational dynamics, internal mixing and magnetic field generation. In this context, helio- and asteroseismology probe angular velocity gradients deep within solar type stars at different evolutionary stages. Still the rotation close to the center of such stars on the main sequence is hardly detectable and the dynamical interaction of the radiative core with the surface convective envelope is not well understood. For instance, the influence of the differential rotation profile sustained by convection and applied as a boundary condition to the radiation zone is very important in the formation of tachoclines. In this work, we study a 2D hydrodynamical model of a radiative core when an imposed, solar or anti-solar, differential rotation is applied at the upper boundary. This model uses the Boussinesq approximation and we find that the shear induces a cylindrical differential rotation associated with a unique cell of meridional circulation in each hemisphere (counterclockwise when the shear is solar-like and clockwise when it is anti-solar). The results are discussed in the framework of seismic observables (internal rotation rate, core-to-surface rotation ratio) while perspectives to improve our modeling by including magnetic field or transport by internal gravity waves will be discussed.