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Magnetic reconnection between a solar filament and nearby coronal loops View all abstracts by submitter

Leping Li   Submitted: 2016-05-12 08:55

Magnetic reconnection between a solar filament and nearby coronal loops | Magnetic reconnection, the rearrangement of magnetic field topology, is a fundamental physical process in magnetized plasma systems all over the universe. Its process is difficult to be directly observed. Coronal structures, such as coronal loops and filament spines, often sketch the magnetic field geometry and its changes in the solar corona. Here we show a highly suggestive observation of magnetic reconnection between an erupting solar filament and its nearby coronal loops, resulting in changes in connection of the filament. X-type structures form when the erupting filament encounters the loops. The filament becomes straight, and bright current sheets form at the interfaces with the loops. Many plasmoids appear in these current sheets and propagate bi-directionally. The filament disconnects from the current sheets, which gradually disperse and disappear, reconnects to the loops, and becomes redirected to the loop footpoints. This evolution of the filament and the loops suggests successive magnetic reconnection predicted by theories but rarely detected with such clarity in observations. Our results on the formation, evolution, and disappearance of current sheets, confirm three-dimensional magnetic reconnection theory and have implications for the evolution of dissipation regions and the release of magnetic energy for reconnection in many magnetized plasma systems.

Authors: Leping Li, Jun Zhang, Hardi Peter, Eric Priest, Huadong Chen, Lijia Guo, Feng Chen, Duncan Mackay
Projects: SDO-AIA,SDO-HMI,STEREO

Publication Status: Nature Physics, 2016, DOI:10.1038/NPHYS3768
Last Modified: 2016-05-13 06:55
Go to main E-Print page  Nonlinear oscillations of coalescing magnetic flux ropes  Energetic characterisation and statistics of solar coronal brightenings  Edit Entry  Download Preprint  Delete Entry 

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