Study Of The Correlation Between Solar Magnetic Reconnection Flux With Solar Flare Types And Duration

Solar flares are eruptive or confined electromagnetic radiation associated with a magnetic energy release in the solar atmosphere. To understand the characteristic, the linear correlation coefficient for total magnetic reconnection flux and flare duration versus flare class by flare type were find. The flare duration was derived from Geostationary Operational Environmental Satellites (GOES). The GOES X-ray sensors detect solar flare intensity and classify them as A, B, C, M, or X according to their peak fluxes. A total of 33 flare events of M5 to X5 flare classes within 45° of Sun’s disk center were examined, dated between February 2011 to September 2017. The flare is spotted using the AIA 1600 Å filtergram with a threshold of 1300 count. The magnetic flux was determined via the HMI 6173 Å filtergram. Their data are accessible through the Joint Science Operations Center (JSOC). Both images were co-registered and superimposed to identify the newly brightened pixels (AIA) then calculated the underlying magnetic field (HMI). The linear correlation between flare class against duration by Full Width Half Maximum (FWHM) is weak (0.19) before the segregation by flare types. However, the further breakdown shows confined flares have a higher linear correlations coefficient (0.58) than eruptive (0.08) no correlation

Characterising Solar Magnetic Reconnection in Confined and Eruptive Flares

Magnetic reconnection is a fundamental mechanism through which energy stored in magnetic fields is released explosively on a massive scale, they could be presented as eruptive or confined flares, depending on their association with coronal mass ejections (CMEs). Several previous works have concluded that there is no correlation between flare duration and flare class, however, their sample sizes are skewed towards B and C classes; they hardly represent the higher classes. Therefore, we studied a sample without extreme events in order to determine the correlation between flare duration and flare type (confined and eruptive). We examined $33$ flares with classes between M5 to X5 within $45^{\circ}$ of the disk centres, using data from the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI). We find that the linear correlation between flare class against flare duration by full width half maximum (FWHM) in general is weak ($r=0.19$); however, confined flares have a significant correlation ($r=0.58$) compared to eruptive types ($r=0.08$). Also, the confined M class flares' average duration is less than half of the eruptive flares. Similarly, confined flares have a higher correlation ($r=0.89$) than eruptive flares ($r=0.60$) between flare classes against magnetic reconnection flux. In this work, a balanced sample size between flare types is an important strategy for obtaining a reliable quantitative comparison.Comment: 26 pages, 11 figure