Details

Autor(en) / Beteiligte

• Panesar, Navdeep K.
• Sterling, Alphonse C.
• Moore, Ronald L.
• Winebarger, Amy R.
• Tiwari, Sanjiv K.
• Savage, Sabrina L.
• Golub, Leon E.
• Rachmeler, Laurel A.
• Kobayashi, Ken
• Brooks, David H.
• Cirtain, Jonathan W.
• Pontieu, Bart De
• McKenzie, David E.
• Morton, Richard J.
• Peter, Hardi
• Testa, Paola
• Walsh, Robert W.
• Warren, Harry P.

Titel

Hi-C 2.1 Observations of Jetlet-like Events at Edges of Solar Magnetic Network Lanes

Ist Teil von

• Astrophysical journal. Letters, 2019-12, Vol.887 (1), p.L8

Ort / Verlag

Austin: The American Astronomical Society

Erscheinungsjahr

2019

Link zum Volltext

Quelle

Free E-Journal (出版社公開部分のみ）

Beschreibungen/Notizen

• We present high-resolution, high-cadence observations of six, fine-scale, on-disk jet-like events observed by the High-resolution Coronal Imager 2.1 (Hi-C 2.1) during its sounding-rocket flight. We combine the Hi-C 2.1 images with images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and the Interface Region Imaging Spectrograph (IRIS), and investigate each event's magnetic setting with co-aligned line-of-sight magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). We find that (i) all six events are jetlet-like (having apparent properties of jetlets), (ii) all six are rooted at edges of magnetic network lanes, (iii) four of the jetlet-like events stem from sites of flux cancelation between majority-polarity network flux and merging minority-polarity flux, and (iv) four of the jetlet-like events show brightenings at their bases reminiscent of the base brightenings in coronal jets. The average spire length of the six jetlet-like events (9000 3000 km) is three times shorter than that for IRIS jetlets (27,000 8000 km). While not ruling out other generation mechanisms, the observations suggest that at least four of these events may be miniature versions of both larger-scale coronal jets that are driven by minifilament eruptions and still-larger-scale solar eruptions that are driven by filament eruptions. Therefore, we propose that our Hi-C events are driven by the eruption of a tiny sheared-field flux rope, and that the flux rope field is built and triggered to erupt by flux cancelation.