On the magnetic field required for driving the observed angular-velocity variations in the solar convection zone

TL;DR

This paper investigates the magnetic field strength needed to explain observed changes in the Sun's rotation rate within its convection zone, using helioseismic data and magnetic stress modeling.

Contribution

It proposes a magnetic field configuration consistent with helioseismic angular velocity variations and photospheric measurements, linking magnetic stress to solar rotation changes.

Findings

Magnetic field configuration can account for observed angular velocity variations.

Surface magnetic measurements support the inferred magnetic field strength.

Magnetic stress is a key driver of angular acceleration in the solar convection zone.

Abstract

A putative temporally varying circulation-free magnetic-field configuration is inferred in an equatorial segment of the solar convection zone from the helioseismologically inferred angular-velocity variation, assuming that the predominant dynamics is angular acceleration produced by the azimuthal Maxwell stress exerted by a field whose surface values are consistent with photospheric line-of-sight measurements.