Grow-up of a Filament Channel by Intermittent Small-scale Magnetic Reconnection
arXiv:2203.09110 · doi:10.1051/0004-6361/202243115
Abstract
Filament channel (FC), a plasma volume where the magnetic field is primarily aligned with the polarity inversion line, is believed to be the pre-eruptive configuration of coronal mass ejections. Nevertheless, evidence for how the FC is formed is still elusive. In this paper, we present a detailed study on the build-up of a FC to understand its formation mechanism. The New Vacuum Solar Telescope of Yunnan Observatories and Optical and Near-Infrared Solar Eruption Tracer of Nanjing University, as well as the AIA and HMI on board Solar Dynamics Observatory are used to study the grow-up process of the FC. Furthermore, we reconstruct the non-linear force-free field (NLFFF) of the active region using the regularized Biot-Savart laws (RBSL) and magnetofrictional method to reveal three-dimension (3D) magnetic field properties of the FC. We find that partial filament materials are quickly transferred to longer magnetic field lines formed by small-scale magnetic reconnection, as evidenced by dot-like Hα/EUV brightenings and subsequent bidirectional outflow jets, as well as untwisting motions. The Hα/EUV bursts appear repeatedly at the same location and are closely associated with flux cancellation, which occurs between two small-scale opposite polarities and is driven by shearing and converging motions. The 3D NLFFF model reveals that the reconnection takes place in a hyperbolic flux tube that is located above the flux cancellation site and below the FC. The FC is gradually built up toward a twisted flux rope via series of small-scale reconnection events that occur intermittently prior to the eruption.
10 pages, 7 figures, 1 table. A&A accepted
References in corpus (20)
- Preprocessing of vector magnetograph data for a non-linear force-free magnetic field reconstruction
- Observation of An Evolving Magnetic Flux Rope Prior To and During A Solar Eruption
- Tracking Vector Magnetograms with the Magnetic Induction Equation
- Emergence of a Helical Flux Rope Under an Active Region Prominence
- Chirality and Magnetic Configurations of Solar Filaments
- On the Relationship Between a Hot-channel-like Solar Magnetic Flux Rope and its embedded Prominence
- Numerical Simulations of Flare-productive Active Regions: delta-sunspots, Sheared Polarity Inversion Lines, Energy Storage, and Predictions
- Regularized Biot-Savart Laws for Modeling Magnetic Flux Ropes
- Triggering mechanism and material transfer of a failed solar filament eruption
- An observationally-constrained model of strong magnetic reconnection in the solar chromosphere. Atmospheric stratification and estimates of heating rates
- Evolution of the Toroidal Flux of CME Flux Ropes during Eruption
- A Prominence Eruption Driven by Flux Feeding from Chromospheric Fibrils
- Recurrent CME-like eruptions in emerging flux regions. I. On the mechanism of eruptions
- Transition from circular-ribbon to parallel-ribbon flares associated with a bifurcated magnetic flux rope
- Measurements of plasma motions in dynamic fibrils
- Material supply and magnetic configuration of an active region filament
- Magnetic Twists of Solar Filaments
- Dynamics evolution of a solar active-region filament from quasi-static state to eruption: rolling motion, untwisting motion, material transfer, and chirality
- Magnetic separatrix as the source region of the plasma supply for an active-region filament
- Formation and Eruption of a Mini-sigmoid Originating in Coronal Hole