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Identification of Pre-flare Processes and Their Possible Role in Driving a Large-scale Flux Rope Eruption with Complex M-class Flare in the Active Region NOAA 12371

Abstract

In this article, we study the origin of precursor flare activity and investigate its role towards triggering the eruption of a flux rope which resulted into a dual-peak M-class flare (SOL2015-06-21T02:36) in the active region NOAA 12371. The flare evolved in two distinct phases with peak flux levels of M2.1 and M2.6 at an interval of \(\approx 54\) min. The active region exhibited striking moving magnetic features (MMFs) along with sunspot rotation. Nonlinear force-free field (NLFFF) modelling of the active region corona reveals a magnetic flux rope along the polarity inversion line in the trailing sunspot group which is observationally manifested by the co-spatial structures of an active region filament and a hot channel identified in the 304 and 94 Å images, respectively, from the Atmospheric Imaging Assembly (AIA). The active region underwent a prolonged phase of flux enhancement followed by a relatively shorter period of flux cancellation prior to the onset of the flare which led to the build up and activation of the flux rope. Extreme ultra-violet (EUV) images reveal localised and structured pre-flare emission, from the region of MMFs, adjacent to the location of the main flare. Our analysis reveals strong, localised regions of photospheric currents of opposite polarities at the precursor location, thereby making the region susceptible to small-scale magnetic reconnection. Precursor reconnection activity from this location most likely induced a slipping reconnection towards the northern leg of the hot channel which led to the destabilisation of the flux rope. The application of magnetic virial theorem suggests that there was an overall growth of magnetic free energy in the active region during the prolonged pre-flare phase which decayed rapidly after the hot channel eruption and its successful transformation into a halo coronal mass ejection (CME).

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Notes

  1. 1.

    See https://www.swpc.noaa.gov/products/solar-region-summary.

  2. 2.

    See https://cdaw.gsfc.nasa.gov/CME_list/index.html.

  3. 3.

    See https://www.swpc.noaa.gov/products/solar-and-geophysical-activity-summary.

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Acknowledgements

The authors would like to thank the SDO and RHESSI teams for their open data policy. SDO is NASA’s mission under the Living With a Star (LWS) program. RHESSI was the sixth mission in the SMall EXplorer (SMEX) program of NASA. The authors are also thankful to Dr. Thomas Wiegelmann for providing the NLFFF code. AP acknowledges partial support of NASA grant 80NSSC17K0016 and NSF award AGS-1650854. We also acknowledge the constructive comments and useful suggestions of the anonymous referee, which improved the presentation and scientific content of the article.

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Mitra, P.K., Joshi, B. & Prasad, A. Identification of Pre-flare Processes and Their Possible Role in Driving a Large-scale Flux Rope Eruption with Complex M-class Flare in the Active Region NOAA 12371. Sol Phys 295, 29 (2020). https://doi.org/10.1007/s11207-020-1596-2

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Keywords

  • Active Regions, Magnetic Fields
  • Flares, Dynamics, Pre-Flare Phenomena, Relation to Magnetic Field
  • Magnetic fields, Models
  • X-Ray Bursts, Association with Flares