IRIS and SDO Observations of Solar Jetlets Resulting from Network-Edge Flux Cancelation. (arXiv:1811.04314v1 [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:+Tiwari_S/0/1/0/all/0/1">Sanjiv K. Tiwari</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:+Norton_A/0/1/0/all/0/1">Aimee A. Norton</a>
Recent observations show that the buildup and triggering of minifilament
eruptions that drive coronal jets result from magnetic flux cancelation at the
neutral line between merging majority- and minority-polarity magnetic flux
patches. We investigate the magnetic setting of ten on-disk small-scale UV/EUV
jets (jetlets), smaller than coronal X-ray jets but larger than chromospheric
spicules) in a coronal hole by using IRIS UV images and SDOAIA EUV images and
line-of-sight magnetograms from SDO/HMI. We observe recurring jetlets at the
edges of magnetic network flux lanes in the coronal hole. From magnetograms
co-aligned with the IRIS and AIA images, we find, clearly visible in nine
cases, that the jetlets stem from sites of flux cancelation proceeding at an
average rate of 1.5 X 10^18 Mx hr^{-1}, and show brightenings at their bases
reminiscent of the base brightenings in larger-scale coronal jets. We find that
jetlets happen at many locations along the edges of network lanes (not limited
to the base of plumes) with average lifetimes of 3 min and speeds of 70 kms.
The average jetlet-base width (4000 km) is three to four times smaller than for
coronal jets (18,000 km). Based on these observations of ten obvious jetlets,
and our previous observations of larger-scale coronal jets in quiet regions and
coronal holes, we infer that flux cancelation is an essential process in the
buildup and triggering of jetlets. Our observations suggest that network jetlet
eruptions might be small-scale analogs of both larger-scale coronal jets and
the still-larger-scale eruptions producing CMEs.
Recent observations show that the buildup and triggering of minifilament
eruptions that drive coronal jets result from magnetic flux cancelation at the
neutral line between merging majority- and minority-polarity magnetic flux
patches. We investigate the magnetic setting of ten on-disk small-scale UV/EUV
jets (jetlets), smaller than coronal X-ray jets but larger than chromospheric
spicules) in a coronal hole by using IRIS UV images and SDOAIA EUV images and
line-of-sight magnetograms from SDO/HMI. We observe recurring jetlets at the
edges of magnetic network flux lanes in the coronal hole. From magnetograms
co-aligned with the IRIS and AIA images, we find, clearly visible in nine
cases, that the jetlets stem from sites of flux cancelation proceeding at an
average rate of 1.5 X 10^18 Mx hr^{-1}, and show brightenings at their bases
reminiscent of the base brightenings in larger-scale coronal jets. We find that
jetlets happen at many locations along the edges of network lanes (not limited
to the base of plumes) with average lifetimes of 3 min and speeds of 70 kms.
The average jetlet-base width (4000 km) is three to four times smaller than for
coronal jets (18,000 km). Based on these observations of ten obvious jetlets,
and our previous observations of larger-scale coronal jets in quiet regions and
coronal holes, we infer that flux cancelation is an essential process in the
buildup and triggering of jetlets. Our observations suggest that network jetlet
eruptions might be small-scale analogs of both larger-scale coronal jets and
the still-larger-scale eruptions producing CMEs.
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