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 SDO /AIA 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 \sim 1.5 \times 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 70km s ^ { -1 } .
The average jetlet-base width ( 4000 km ) is three to four times smaller than for coronal jets ( \sim 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 .