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Conference Paper

Coronal jets of all sizes observed at sites of magnetic flux cancelation

Authors

Panesar,  Navdeep
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Sterling,  Alphonse
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Moore,  Ronald
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Tiwari,  Sanjiv
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

Hansteen,  Viggo
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

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Citation

Panesar, N., Sterling, A., Moore, R., Tiwari, S., Hansteen, V. (2023): Coronal jets of all sizes observed at sites of magnetic flux cancelation, XXVIII General Assembly of the International Union of Geodesy and Geophysics (IUGG) (Berlin 2023).
https://doi.org/10.57757/IUGG23-3576


Cite as: https://gfzpublic.gfz-potsdam.de/pubman/item/item_5020497
Abstract
Solar coronal jets of all sizes are magnetically channeled eruptions that occur in all types of solar environments (e.g. active regions, quiet-Sun regions and coronal holes). They are often observed in the solar corona in EUV and coronal X-ray images. Recent studies show that coronal jets are driven by the eruption of small-scale filaments (minifilaments). Once the eruption is underway external and internal reconnection evidently makes the jet spire and the bright emission in the jet base. By examining pre-jet evolutionary changes in line-of-sight SDO/HMI magnetograms while examining concurrent E(UV) images (from SDO/AIA, Solar Orbiter/EUI, and IRIS) of coronal and transition-region emission, we find clear evidence that flux cancelation is the main process that builds pre-jet minifilaments, and is also the main process that triggers the eruptions. In addition to typical coronal jets, we find that small-scale jets (jetlets/network jets) are rooted at the edges of magnetic network lanes, and often come from the sites of flux cancelation. We also compare some of the small-scale observed jets with analogous jets in a Bifrost MHD simulation of a quiet Sun region. Simulations clearly show that jets often come from sites of flux cancelation. From our observations we infer that magnetic reconnection driven flux cancelation is the fundamental process for the buildup and triggering of all sizes of jets.