Dynamics of the solar tachocline II: the stratified case

TL;DR

This paper provides a comprehensive numerical analysis of the Gough & McIntyre model for the solar tachocline, demonstrating how a primordial magnetic field confined by convection zone flows can explain observed solar rotation and flow patterns.

Contribution

It presents the first fully nonlinear, self-consistent numerical solution of the model that aligns with key solar observational constraints.

Findings

Successful confinement of the magnetic field below the tachocline.

Reproduction of the observed uniform rotation profile.

Confinement of meridional flows to the upper radiative zone.

Abstract

We present a detailed numerical study of the Gough & McIntyre model for the solar tachocline. This model explains the uniformity of the rotation profile observed in the bulk of the radiative zone by the presence of a large-scale primordial magnetic field confined below the tachocline by flows originating from within the convection zone. We attribute the failure of previous numerical attempts at reproducing even qualitatively Gough & McIntyre's idea to the use of boundary conditions which inappropriately model the radiative--convective interface. We emphasize the key role of flows downwelling from the convection zone in confining the assumed internal field. We carefully select the range of parameters used in the simulations to guarantee a faithful representation of the hierarchy of expected lengthscales. We then present, for the first time, a fully nonlinear and self-consistent numerical solution of the Gough & McIntyre model which qualitatively satisfies the following set of observational constraints: (i) the quenching of the large-scale differential rotation below the tachocline - including in the polar regions - as seen by helioseismology (ii) the confinement of the large-scale meridional flows to the uppermost layers of the radiative zone as required by observed light element abundances and suggested by helioseismic sound-speed data.