Turbulent magnetic helicity fluxes in solar convective zone

TL;DR

This paper derives and analyzes turbulent magnetic helicity fluxes in the solar convective zone, highlighting their role in dynamo saturation and magnetic field generation through a mean-field spectral $ au$ approximation.

Contribution

It introduces a detailed derivation of turbulent magnetic helicity fluxes including non-gradient and gradient parts, considering the effects of stratification and shear in the solar convective zone.

Findings

Turbulent magnetic helicity fluxes include non-gradient and gradient contributions.

Fluxes are driven by kinetic $oldsymbol{ m oldsymbol{ m f ext{ extmu}}}$ effect, shear, and magnetic diffusion.

Dominant fluxes in the solar convective zone are due to the kinetic $oldsymbol{ m ext{ extmu}}$ effect and its derivatives.

Abstract

Combined action of helical motions of plasma (the $\alpha$ effect) and non-uniform (differential) rotation is a key dynamo mechanism of solar and galactic large-scale magnetic fields. Dynamics of magnetic helicity of small-scale fields is a crucial mechanism in a nonlinear dynamo saturation where turbulent magnetic helicity fluxes allow to avoid catastrophic quenching of the $\alpha$ effect. The convective zone of the Sun and solar-like stars as well as galactic discs are the source for production of turbulent magnetic helicity fluxes. In the framework of the mean-field approach and the spectral $\tau$ approximation, we derive turbulent magnetic helicity fluxes using the Coulomb gauge in a density-stratified turbulence. The turbulent magnetic helicity fluxes include non-gradient and gradient contributions. The non-gradient magnetic helicity flux is proportional to a nonlinear effective velocity (which vanishes in the absence of the density stratification) multiplied by small-scale magnetic helicity, while the gradient contributions describe turbulent magnetic diffusion of the small-scale magnetic helicity. In addition, the turbulent magnetic helicity fluxes contain source terms proportional to the kinetic $\alpha$ effect or its gradients, and also contributions caused by the large-scale shear (solar differential rotation). We have demonstrated that the turbulent magnetic helicity fluxes due to the kinetic $\alpha$ effect and its radial derivative in combination with the nonlinear magnetic diffusion of the small-scale magnetic helicity are dominant in the solar convective zone.