Panesar, Navdeep ; Sterling, Alphonse ; Moore, Ronald ; Tiwari, Sanjiv ; Hansteen, Viggo H. ; Berghmans, David ; Cheung, Mark ; Muller, Daniel ; Auchere, Frederic ; Zhukov, Andrei

Poster presented at 246th Meeting of the American Astronomical Society, Anchorage/Alaska on 2025-06-08

Abstract: We present the magnetic origin of different types of campfires and coronal jets, using line-of-sight magnetograms from the Solar Dynamics Observatory (SDO)/Helioseismic and Magnetic Imager, together with extreme ultraviolet images from the Solar Orbiter/ Extreme Ultraviolet Imager and from the SDO/Atmospheric Imaging Assembly. We find that (i) both campfires and coronal jets reside above neutral lines and they often appear at sites of magnetic flux cancelation between a majority-polarity magnetic flux patch and a merging minority-polarity flux patch, with a flux cancelation rate of ∼1018 Mx hr−1 (ii) The majority of campfire brightenings are preceded by eruption of a cool-plasma structure, analogous to erupting minifilaments that precede coronal jets. Our observations suggest that (a) the presence of magnetic flux ropes may be ubiquitous in the solar atmosphere and not limited to coronal jets and larger-scale eruptions that make CMEs, and (b) magnetic flux cancelation, most likely accompanied with magnetic reconnection in the lower solar atmosphere, is the fundamental process for the formation and triggering of most solar campfires and coronal jets. Finally, we compare fine-scale jets (i.e., campfires and similar jet-like features that are smaller than typical coronal jets) with results found from a Bifrost MHD simulation.

Keyword(s): Solar Orbiter ; EUI ; jets ; campfires
Links: link; link2