A statistical Analysis of Magnetic Field Changes in the Photosphere During Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons

TL;DR

This study uses high-cadence vector magnetograms from the Solar Dynamics Observatory to analyze magnetic field changes during solar flares, revealing their relationship with flare ribbons and suggesting mechanisms like magnetic reconnection and coronal implosion.

Contribution

It provides the first detailed analysis linking the duration of magnetic field changes to flare duration and their association with flare ribbon properties.

Findings

Largest magnetic changes occur near the polarity inversion line.

Field changes are more related to ribbon properties than active region size.

Duration of field changes correlates with flare duration, averaging 29% of the GOES flare.

Abstract

We analyze high-cadence vector magnetograms (135~s) and flare-ribbon observations of 37 flares from the Solar Dynamics Observatory to understand the spatial and temporal properties of changes in the photospheric vector magnetic field and their relationship to footpoints of reconnected fields. Confirming previous studies, we find that the largest permanent changes in the horizontal field component lie near the polarity inversion line, whereas changes in the vertical field are less pronounced and are distributed throughout the active region. We find that pixels swept up by ribbons do not always exhibit permanent changes in the field. However, when they do, ribbon emission typically occurs several minutes before the start of field changes. The changes in the properties of the field show no relation to the size of active regions, but are strongly related to the flare-ribbon properties such as ribbon magnetic flux and ribbon area. For the first time, we find that the duration of permanent changes in the field is strongly coupled with the duration of the flare, lasting on average 29\% of the duration of the GOES flare. Our results suggest that changes in photospheric magnetic fields are caused by a combination of two scenarios: contraction of flare loops driven by magnetic reconnection and coronal implosion.