Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
arXiv:2211.06060 · doi:10.3847/1538-4357/aca08c
Abstract
We investigate the formation and eruption of hot channels associated with the M6.5 class flare (SOL2015-06-22T18:23) occurring in NOAA AR 12371 on 2015 June 22. Two flare precursors are observed before the flare main phase. Observations in 94 Å and 131 Å by SDO/AIA have revealed the early morphology of the first hot channel as a group of hot loops, which is termed as seed hot channel. A few seed hot channels are formed above the polarity inversion line (PIL) and the formation is associated with footpoint brightenings' parallel motion along the PIL, which proceeds into the early stage of the flare main phase. During this process, seed hot channels build up and rise slowly, being accelerated at the peak of the second precursor. They merge in the process of acceleration forming a larger hot channel, which then forms an "inverted γ" shape kinking structure. Before the flare peak, the second kinking hot channel with negative crossing appears near the first kinking hot channel that has erupted. The eruption of these two hot channels produce two peaks on the main flare's GOES light curve. The footpoint brightenings' propagation along the PIL indicate that the first kinking hot channel may be formed due to zipper reconnection. The occurrence of merging between seed hot channels observed by AIA is supported by the extrapolated nonlinear force-free field models. The observed writhing motion of the first kinking hot channel may be driven by the Lorentz force.
References in corpus (20)
- Torus instability
- Ideal kink instability of a magnetic loop equilibrium
- Optimization code with weighting function for the reconstruction of coronal magnetic fields
- Observation of An Evolving Magnetic Flux Rope Prior To and During A Solar Eruption
- Photospheric flux cancellation and associated flux rope formation and eruption
- A fundamental mechanism of solar eruption initiation
- Sigmoid-to-Flux-Rope Transition Leading to A Loop-Like Coronal Mass Ejection
- Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections
- Flux Rope Formation Preceding Coronal Mass Ejection Onset
- High-resolution observations of flare precursors in the low solar atmosphere
- Initiation and Early Kinematic Evolution of Solar Eruptions
- Magnetic Flux Ropes in the Solar Corona: Structure and Evolution toward Eruption
- Flux-Rope Twist in Eruptive Flares and CMEs: due to Zipper and Main-Phase Reconnection
- Double arc instability in the solar corona
- On the Brightening Propagation of Post-Flare Loops Observed by TRACE
- Witnessing a Large-scale Slipping Magnetic Reconnection along a Dimming Channel during a Solar Flare
- Testing non-linear force-free coronal magnetic field extrapolations with the Titov-Demoulin equilibrium
- HXR emission from an activated flux rope and subsequent evolution of an eruptive long duration solar flare
- The Evolution of Writhe in Kink-Unstable Flux Ropes and Erupting Filaments
- The Rotation of Magnetic Flux Rope Formed during Solar Eruption