| Issue |
A&A
Volume 673, May 2023
Solar Orbiter First Results (Nominal Mission Phase)
|
|
|---|---|---|
| Article Number | A83 | |
| Number of page(s) | 8 | |
| Section | The Sun and the Heliosphere | |
| DOI | https://doi.org/10.1051/0004-6361/202245814 | |
| Published online | 10 May 2023 | |
Evidence of external reconnection between an erupting mini-filament and ambient loops observed by Solar Orbiter/EUI⋆
1
School of Astronomy and Space Science, Nanjing University, Nanjing 210046, PR China
e-mail: xincheng@nju.edu.cn
2
Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, PR China
3
Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
4
Solar-Terrestrial Centre of Excellence – SIDC, Royal Observatory of Belgium, Ringlaan 3 Av. Circulaire, 1180 Brussels, Belgium
5
UCL-Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
6
Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale, 91405 Orsay, France
7
Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, 7260 Davos Dorf, Switzerland
8
ETH-Zürich, Wolfgang-Pauli-Str. 27, 8093 Zürich, Switzerland
9
Skobeltsyn Institute of Nuclear Physics, Moscow State University, 119992 Moscow, Russia
Received:
29
December
2022
Accepted:
21
March
2023
Mini-filament eruptions are one of the most common small-scale transients in the solar atmosphere. However, their eruption mechanisms are still not understood thoroughly. Here, with a combination of 174 Å images of high spatio-temporal resolution taken by the Extreme Ultraviolet Imager on board Solar Orbiter and images of the Atmospheric Imaging Assembly on board Solar Dynamics Observatory, we investigate in detail an erupting mini-filament over a weak magnetic field region on 2022 March 4. Two bright ribbons clearly appeared underneath the erupting mini-filament as it quickly ascended, and subsequently, some dark materials blew out when the erupting mini-filament interacted with the outer ambient loops, thus forming a blowout jet characterized by a widening spire. At the same time, multiple small bright blobs of 1−2 Mm appeared at the interaction region and propagated along the post-eruption loops toward the footpoints of the erupting fluxes at a speed of ∼100 km s−1. They also caused a semi-circular brightening structure. Based on these features, we suggest that the mini-filament eruption first experiences internal and then external reconnection, the latter of which mainly transfers mass and magnetic flux of the erupting mini-filament to the ambient corona.
Key words: Sun: flares / Sun: magnetic fields / Sun: corona
Movie (Fig. 1) is available at https://www.aanda.org
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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