Formation of a Solar Filament by Magnetic Reconnection and Associated Chromospheric Evaporation and Subsequent Coronal Condensation
arXiv:2110.10951 · doi:10.3847/2041-8213/ac31b6
Abstract
We present the first observation of a solar filament formed by magnetic reconnection and associated chromospheric evaporation and subsequent coronal condensation. Driven by shearing motion during flux emergence, a sequential tether-cutting reconnection processes occurred and resulted in an M1.3 confined flare accompany with the formation of a sigmoid structure. It is found that the flare had a conjugate compact footpoint brightenings, which correspond to the footpoints of the sigmoid. Furthermore, observational evidence of explosive evaporation is well diagnosed at the conjugate footpoint brightenings in the impulsive phase of the flare. After the flare, continuous cool condensations formed at about the middle section of the sigmoid and then moved in opposite directions along the sigmoid, eventually leading to the formation of the filament. These observations suggest that magnetic reconnection not only can form the magnetic field structure of the filament, but also heat their chromospheric footpoints during their formation and drive chromospheric evaporation. As a result, the heated chromospheric plasma may be evaporated into the magnetic field structure of the filament, where the accumulated hot plasma might suffer from thermal instability or thermal non-equilibrium, causing catastrophic cooling and coronal condensation to form the cool dense material of the filament. This observation lends strong support to the evaporative-condensation model and highlights the crucial role of magnetic reconnection in forming both the magnetic field structure and the cool dense material of filaments.
17 pages, 5 figures, accepted for publication in ApJ Letters
References in corpus (21)
- Tracking Vector Magnetograms with the Magnetic Induction Equation
- Emergence of a Helical Flux Rope Under an Active Region Prominence
- Modelling of EIS spectrum drift from instrumental temperatures
- Open questions on prominences from coordinated observations by IRIS, Hinode, SDO/AIA, THEMIS, and the Meudon/MSDP
- Direct Observations of Tether-cutting Reconnection During a Major Solar Event From 2014 February 24 to 25
- Simulations of solar filament fine structures and their counterstreaming flows
- The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He I 10830 A triplet
- Observations of Solar Coronal Rain in Null Point Topologies
- Reconnection-Condensation Model for Solar Prominence Formation
- The Dynamics of Funnel Prominences
- The formation of an inverse S-shaped active-region filament driven by sunspot motion and magnetic reconnection
- Evidence of Explosive Evaporation in a Microflare Observed by Hinode/EIS
- Investigating Energetic X-Shaped Flares on the Outskirts of A Solar Active Region
- The eruption of a small-scale emerging flux rope as the driver of an M-class flare and a coronal mass ejection
- The Origin of Solar Filament Plasma Inferred from in situ Observations of Elemental Abundances
- Recurrent Two-Sided Loop Jets Caused by Magnetic Reconnection between Erupting Minifilaments and Nearby Large Filament
- A unified model of solar prominence formation
- Filament Eruption and Its Reformation Caused by Emerging Magnetic Flux
- Heating at the remote footpoints as a brake on jet flows along loops in the solar atmosphere
- On-disk solar coronal condensations facilitated by magnetic reconnection between open and closed magnetic structures
- How eruptions of a small filament feed materials to a nearby larger-scaled filament