Change ratios of magnetic helicity and magnetic free energy during major solar flares

TL;DR

This study analyzes the change ratios of magnetic helicity and free energy during 47 solar flares, revealing distinct differences between confined and eruptive flares, supporting theories of magnetic helicity conservation and removal during CMEs.

Contribution

It provides observational evidence of differing magnetic helicity and energy change ratios in confined versus eruptive flares, enhancing understanding of magnetic processes in solar eruptions.

Findings

Confined flares show median helicity change of -0.8%.

Eruptive flares show median helicity change of -14.5%.

Magnetic free energy decreases more in eruptive flares.

Abstract

Magnetic helicity is an important concept in solar physics, with a number of theoretical statements pointing out the important role of magnetic helicity in solar flares and coronal mass ejections (CMEs). Here we construct a sample of 47 solar flares, which contains 18 no-CME-associated confined flares and 29 CME-associated eruptive flares. We calculate the change ratios of magnetic helicity and magnetic free energy before and after these 47 flares. Our calculations show that the change ratios of magnetic helicity and magnetic free energy show distinct different distributions in confined flares and eruptive flares. The median value of the change ratios of magnetic helicity in confined flares is $-0.8$%, while this number is $-14.5$% for eruptive flares. For the magnetic free energy, the median value of the change ratios is $-4.3$% for confined flares, whereas this number is $-14.6$% for eruptive flares. This statistical result, using observational data, is well consistent with the theoretical understandings that magnetic helicity is approximately conserved in the magnetic reconnection, as shown by confined flares, and the CMEs take away magnetic helicity from the corona, as shown by eruptive flares.