On the dynamical interaction between overshooting convection and an underlying dipole magnetic field -- I. The non-dynamo regime

TL;DR

This study investigates how overshooting convection interacts with large-scale dipole magnetic fields in stellar radiative zones, revealing turbulent processes that can confine magnetic fields and impact stellar magnetic dynamics.

Contribution

The paper demonstrates through 3D simulations that turbulent convection can both diffuse and confine dipole magnetic fields in stellar radiative zones, aligning with mean-field models.

Findings

Turbulent diffusion removes magnetic fields faster than molecular diffusion in less turbulent regimes.

Turbulent pumping can partially counteract diffusion, leading to magnetic field confinement.

Simulations support the idea that turbulent convection can confine large-scale magnetic fields in stellar interiors.

Abstract

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 zones. We have run a suite of 3D Boussinesq numerical calculations in a spherical shell that consists of a convection zone with an underlying stable region that initially compactly contains a dipole field. By varying the strength of the convective driving, we find that, in the less turbulent regime, convection acts as turbulent diffusion that removes the field faster than solely molecular diffusion would do. However, in the more turbulent regime, turbulent pumping becomes more efficient and partially counteracts turbulent diffusion, leading to a local accumulation of the field below the overshoot region. These simulations suggest that dipole fields might be confined in underlying stable regions by highly turbulent convective motions at stellar parameters. The confinement is of large-scale field in an average sense and we show that it is reasonably modeled by mean-field ideas. Our findings are particularly interesting for certain models of the Sun, which require a large-scale, poloidal magnetic field to be confined in the solar radiative zone in order to explain simultaneously the uniform rotation of the latter and the thinness of the solar tachocline.