# Evolution of the Sun's non-axisymmetric toroidal field

## TL;DR

This study models the Sun's non-axisymmetric azimuthal magnetic flux using a kinematic flux transport model, revealing that non-axisymmetric components are minor and have limited impact on flux emergence locations.

## Contribution

It introduces a new kinematic flux transport model based on the Babcock-Leighton framework to infer subsurface non-axisymmetric magnetic flux from surface observations.

## Key findings

- Non-axisymmetric azimuthal flux constitutes about 3% of total flux.
- Non-axisymmetric structures have limited influence on flux emergence.
- Emergence probability depends on the ratio of active region flux to underlying azimuthal flux.

## Abstract

Aims. We aim to infer the sub-surface distribution of the Sun's non-axisymmetric azimuthal magnetic flux from observable quantities, such as the surface magnetic field and the large scale plasma flows. Methods. We have built a kinematic flux transport model of the solar dynamo based on the Babcock-Leighton framework. We constructed the source term for the poloidal field using SOLIS magnetograms spanning three solar cycles. Based on this source we calculated the azimuthal flux below the surface. The flux transport model has two free parameters which we constrain using sunspot observations from cycle 22. We compared the model results with observations from cycle 23. Results. The structure of the azimuthal field is mainly axisymmetric. The departures from axisymmetry represent, on average, ~3% of the total azimuthal flux. Owing to its relative weakness, the non-axisymmetric structure of the azimuthal field does not have a significant impact on the location in which the emergences appear or on the amount of flux contained in them. We find that the probability of emergence is a function of the ratio between the flux content of an active region and the underlying azimuthal flux.