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Abstract
Magnetic reconnection is a key mechanism involved in solar eruptions and is also a prime possibility to heat the low corona to millions of degrees. Here, we present ultra-high-resolution extreme ultraviolet observations of persistent null-point reconnection in the corona at a scale of about 390 km over one hour observations of the Extreme-Ultraviolet Imager on board Solar Orbiter spacecraft. The observations show formation of a null-point configuration above a minor positive polarity embedded within a region of dominant negative polarity near a sunspot. The gentle phase of the persistent null-point reconnection is evidenced by sustained point-like high-temperature plasma (about 10 MK) near the null-point and constant outflow blobs not only along the outer spine but also along the fan surface. The blobs appear at a higher frequency than previously observed with an average velocity of about 80 km s−1 and life-times of about 40 s. The null-point reconnection also occurs explosively but only for 4 minutes, its coupling with a mini-filament eruption generates a spiral jet. These results suggest that magnetic reconnection, at previously unresolved scales, proceeds continually in a gentle and/or explosive way to persistently transfer mass and energy to the overlying corona.
Magnetic reconnection is a fundamental energy release mechanism in space and laboratory plasmas. Here, the authors show persistent magnetic null-point reconnection in the solar corona at a scale of about 390 km.
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1 Nanjing University, School of Astronomy and Space Science, Nanjing, China (GRID:grid.41156.37) (ISNI:0000 0001 2314 964X); Max Planck Institute for Solar System Research, Göttingen, Germany (GRID:grid.435826.e) (ISNI:0000 0001 2284 9011); Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, China (GRID:grid.419897.a) (ISNI:0000 0004 0369 313X)
2 University of St. Andrews, School of Mathematics and Statistics, Fife, UK (GRID:grid.11914.3c) (ISNI:0000 0001 0721 1626)
3 Nanjing University, School of Astronomy and Space Science, Nanjing, China (GRID:grid.41156.37) (ISNI:0000 0001 2314 964X); Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, China (GRID:grid.419897.a) (ISNI:0000 0004 0369 313X)
4 Sorbonne Université, Observatoire de Paris - PSL, École Polytechnique, IP Paris, CNRS, Laboratory for Plasma Physics (LPP), Paris, France (GRID:grid.419897.a); Rosseland Centre for Solar Physics, Institute for Theoretical Astrophysics, Universitetet i Oslo, Oslo, Norway (GRID:grid.5510.1) (ISNI:0000 0004 1936 8921)
5 Max Planck Institute for Solar System Research, Göttingen, Germany (GRID:grid.435826.e) (ISNI:0000 0001 2284 9011)
6 Chinese Academy of Sciences, State Key Laboratory of Space Weather, National Space Science Center, Beijing, China (GRID:grid.9227.e) (ISNI:0000000119573309)
7 Nanjing University, School of Astronomy and Space Science, Nanjing, China (GRID:grid.41156.37) (ISNI:0000 0001 2314 964X); Sorbonne Université, Observatoire de Paris - PSL, École Polytechnique, IP Paris, CNRS, Laboratory for Plasma Physics (LPP), Paris, France (GRID:grid.41156.37)
8 Solar-Terrestrial Centre of Excellence - SIDC, Royal Observatory of Belgium, Brussels, Belgium (GRID:grid.425636.0) (ISNI:0000 0001 2297 3653)
9 Solar-Terrestrial Centre of Excellence - SIDC, Royal Observatory of Belgium, Brussels, Belgium (GRID:grid.425636.0) (ISNI:0000 0001 2297 3653); Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia (GRID:grid.14476.30) (ISNI:0000 0001 2342 9668)
10 Mullard Space Science Laboratory, University College London, Dorking, UK (GRID:grid.83440.3b) (ISNI:0000000121901201)
11 PMOD/WRC, Davos Dorf, Switzerland (GRID:grid.83440.3b); ETH-Zürich, Zürich, Switzerland (GRID:grid.5801.c) (ISNI:0000 0001 2156 2780)
12 ETH-Zürich, Zürich, Switzerland (GRID:grid.5801.c) (ISNI:0000 0001 2156 2780)
13 Institut d’Astrophysique Spatiale, Université Paris-Saclay, Orsay Cedex, France (GRID:grid.482888.6) (ISNI:0000 0004 0614 9404)