Large-Scale Magnetic Field Fragmentation in Flux-Tubes Near the Base of the Solar Convection Zone

TL;DR

This paper investigates how magnetic quenching of turbulent thermal diffusivity causes large-scale magnetic field fragmentation near the solar convection zone base, potentially explaining the formation of solar active regions.

Contribution

It introduces a linear stability analysis considering magnetic field-dependent thermal diffusivity, revealing a rapid instability leading to magnetic inhomogeneities.

Findings

Instability has a short growth time compared to solar cycle.

Fragmented magnetic regions are tens of mega-meters in scale.

Magnetic energy of concentrations matches active region energies.

Abstract

Magnetic quenching of turbulent thermal diffusivity leads to instability of the large-scale field with the production of spatially isolated regions of enhanced field. This conclusion follows from a linear stability analysis in the framework of mean-field magnetohydrodynamics that allows for thermal diffusivity dependence on the magnetic field. The characteristic growth time of the instability is short compared to the 11-year period of solar activity. The characteristic scale of the increased field regions measures in tens of mega-meters. The instability can produce magnetic inhomogeneities whose buoyant rise to the solar surface forms the solar active regions. The magnetic energy of the field concentrations coincides in order of magnitude with the energy of the active regions.