Magnetic Field Re-configuration Associated With a Slow Rise Eruptive X1.2 Flare in NOAA Active Region 11944

Vasyl Yurchyshyn, Xu Yang, Gelu Nita, Gregory Fleishman, Valentina Abramenko, Satoshi Inoue, Eun Kyung Lim, Wenda Cao

Research output: Contribution to journalArticlepeer-review

2 Scopus citations

Abstract

Using multi-wavelength observations, we analysed magnetic field variations associated with a gradual X1.2 flare that erupted on January 7, 2014 in active region (AR) NOAA 11944 located near the disk center. A fast coronal mass ejection (CME) was observed following the flare, which was noticeably deflected in the south-west direction. A chromospheric filament was observed at the eruption site prior to and after the flare. We used SDO/HMI data to perform non-linear force-free field extrapolation of coronal magnetic fields above the AR and to study the evolution of AR magnetic fields prior to the eruption. The extrapolated data allowed us to detect signatures of several magnetic flux ropes present at the eruption site several hours before the event. The eruption site was located under slanted sunspot fields with a varying decay index of 1.0-1.5. That might have caused the erupting fields to slide along this slanted magnetic boundary rather than vertically erupt, thus explaining the slow rise of the flare as well as the observed direction of the resulting CME. We employed sign-singularity tools to quantify the evolutionary changes in the model twist and observed current helicity data, and found rapid and coordinated variations of current systems in both data sets prior to the event as well as their rapid exhaustion after the event onset.

Original languageEnglish (US)
Article number816523
JournalFrontiers in Astronomy and Space Sciences
Volume9
DOIs
StatePublished - Apr 14 2022

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics

Keywords

  • Corona -sun
  • activity
  • flares -sun
  • magnetic fields -sun
  • sun
  • sun—active regions

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