Hi-C 2.1 Observations of Jetlet-like Events at Edges of Solar Magnetic Network Lane. (arXiv:1911.02331v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Panesar_N/0/1/0/all/0/1">Navdeep K. Panesar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sterling_A/0/1/0/all/0/1">Alphonse C. Sterling</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moore_R/0/1/0/all/0/1">Ronald L. Moore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winebarger_A/0/1/0/all/0/1">Amy R. Winebarger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tiwari_S/0/1/0/all/0/1">Sanjiv K. Tiwari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Savage_S/0/1/0/all/0/1">Sabrina L. Savage</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golub_L/0/1/0/all/0/1">Leon Golub</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rachmeler_L/0/1/0/all/0/1">Laurel A. Rachmeler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_K/0/1/0/all/0/1">Ken Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">David H. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cirtain_J/0/1/0/all/0/1">Jonathan W. Cirtain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pontieu_B/0/1/0/all/0/1">Bart De Pontieu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McKenzie_D/0/1/0/all/0/1">David E. McKenzie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morton_R/0/1/0/all/0/1">Richard J. Morton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peter_H/0/1/0/all/0/1">Hardi Peter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Testa_P/0/1/0/all/0/1">Paola Testa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walsh_R/0/1/0/all/0/1">Robert W. Walsh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Warren_H/0/1/0/all/0/1">Harry P. Warren</a>
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 SDO/AIA, and IRIS, and investigate each event’s magnetic
setting with co-aligned line-of-sight magnetograms from SDO/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 (9,000$pm$3000km) is three times shorter than that for IRIS
jetlets (27,000$pm$8000km). While not ruling out other generation mechanisms,
the observations suggest that at least four of these events may be miniature
versions of both larger-scale coronal jets that are driven by minifilament
eruptions and still-larger-scale solar eruptions that are driven by filament
eruptions. Therefore, we propose that our Hi-C events are driven by the
eruption of a tiny sheared-field flux rope, and that the flux-rope field is
built and triggered to erupt by flux cancelation.
We present high-resolution, high-cadence observations of six, fine-scale,
on-disk jet-like events observed by the High-resolution Coronal Imager 2.1
(Hi-C 2.1) during its sounding-rocket flight. We combine the Hi-C 2.1 images
with images from SDO/AIA, and IRIS, and investigate each event’s magnetic
setting with co-aligned line-of-sight magnetograms from SDO/HMI. We find that:
(i) all six events are jetlet-like (having apparent properties of jetlets),
(ii) all six are rooted at edges of magnetic network lanes, (iii) four of the
jetlet-like events stem from sites of flux cancelation between
majority-polarity network flux and merging minority-polarity flux, and (iv)
four of the jetlet-like events show brightenings at their bases reminiscent of
the base brightenings in coronal jets. The average spire length of the six
jetlet-like events (9,000$pm$3000km) is three times shorter than that for IRIS
jetlets (27,000$pm$8000km). 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.
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