Homologous CME/flares from AR 12371

Nugget
Number:	318
1st Author:	Panditi Vemareddy
2nd Author:	Pascal Demoulin
Published:	19 March 2018
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Introduction

Active regions (ARs) with sigmoidal structure, generally seen in soft X-rays and EUV, are prone to eruptions (coronal mass ejections, CMEs) and associated flares. Some ARs show a rapid succession of CMEs and flares over a timescale of few hours. These can have astonishing similarities in all properties, in which case they are called homologous events. The time intervals can be small compared to the typical timescale for magnetic energy build-up in the existing coronal fields, so the emergence of new magnetic flux has been suggested to be responsible for the phenomenon of repetitive flares and CMEs (Ref[1]). On the other hand, successive CMEs can also occur from ARs in a timescale comparable to energy build-up by footpoint motions in the post-emergence phase. The velocity field derived from tracked magnetograms indicates frequently persistent shear and converging motions of polarity regions about the polarity inversion line. These motions introduce huge amounts of magnetic energy and helicity in the region's magnetic structure, enabling flares and CMEs. While the stored energy configuration is vital, the persistence of sigmoidal structure is the central feature for the successive CME occurrence from a source AR and had been the central subject for eruptive activity.

Active Region NOAA 12371

AR 12371 was in a post-emerged phase, producing successive fast CMEs in the span of its disk transit (18-25 June, 2015). EUV observations at the Sun register the initiation times of four eruptions as June 18/15:05 UT (CME1), 21/00:45 UT (CME2), 22/16:15 UT (CME3), and 25/07:30 UT (CME4), respectively. Subsequently, the disk-integrated GOES X-ray light curve (Figure 1a) shows that the CMEs were associated with long duration M-class flares. The matching EUV double dimming, three-part CME structure, and fast propagation speeds in LASCO FOV (>1000 kms^-1) altogether characterize these CMEs as homologous events.

Figure 1: Magnetic evolution in AR 12371 during its disk transit, (a) disk integrated soft X-ray GOES flux. Vertical lines mark the CME start times, (b) net magnetic flux φ from north and south polarities, (c) coronal twist parameter αav averaged over the AR, (d) helicity flux injection (in blue), and coronal helicity H normalized by (in red), (e) energy flux injection dE/dt (in blue) and its coronal accumulation (in red). The observed decrease in net magnetic flux is due to flux cancellation at the polarity inversion line. Corresponding to the persistent strong shear motions, the H-flux is strong up to June 21 and accordingly ∣αav∣ shows an increasing trend.

References

[1] ["Recurrent flare/CME events from an emerging flux region"