Speed of Meridional Flows and Magnetic Flux Transport on the Sun

TL;DR

This study investigates the speed of magnetic flux transport on the Sun's surface using magnetic butterfly diagrams and compares it with helioseismology measurements, revealing differences influenced by local flows and implications for solar dynamo modeling.

Contribution

It provides a novel analysis of magnetic flux transport speeds and highlights the importance of considering longitudinal flow structures in solar dynamo models.

Findings

Magnetic flux transport speeds are generally consistent with helioseismology measurements.

Local circulation flows around active regions significantly affect flux transport.

Helioseismology-derived meridional flow measurements may not directly represent magnetic flux transport.

Abstract

We use the magnetic butterfly diagram to determine the speed of the magnetic flux transport on the solar surface towards the poles. The manifestation of the flux transport is clearly visible as elongated structures extended from the sunspot belt to the polar regions. The slopes of these structures are measured and interpreted as meridional magnetic flux transport speed. Comparison with the time-distance helioseismology measurements of the mean speed of the meridional flows at the depth of 3.5--12 Mm shows a generally good agreement, but the speeds of the flux transport and the meridional flow are significantly different in areas occupied by the magnetic field. The local circulation flows around active regions, especially the strong equatorward flows on the equatorial side of active regions affect the mean velocity profile derived by helioseismology, but do not influence the magnetic flux transport. The results show that the mean longitudinally averaged meridional flow measurements by helioseismology may not be used directly in solar dynamo models for describing the magnetic flux transport, and that it is necessary to take into account the longitudinal structure of these flows.