Coronal jets are transient narrow features in the solar corona that originate from all regions of the solar disk : active regions , quiet sun , and coronal holes .
Recent studies indicate that at least some coronal jets in quiet regions and coronal holes are driven by the eruption of a minifilament \citep Sterling2015 following flux cancellation at a magnetic neutral line \citep Panesar2016 .
We have tested the veracity of that view by examining 60 random jets in quiet regions and coronal holes using multithermal ( 304 Å , 171 Å , 193 Å , and 211 Å ) extreme ultraviolet ( EUV ) images from the Solar Dynamics Observatory ( SDO ) /Atmospheric Imaging Assembly ( AIA ) and line-of-sight magnetograms from the SDO/Helioseismic and Magnetic Imager ( HMI ) .
By examining the structure and changes in the magnetic field before , during , and after jet onset , we found that 85 % of these jets resulted from a minifilament eruption triggered by flux cancellation at the neutral line .
The 60 jets have a mean base diameter of 8800 \pm 3100 km and a mean duration of 9 \pm 3.6 minutes .
These observations confirm that minifilament eruption is the driver and magnetic flux cancellation is the primary trigger mechanism for most coronal hole and quiet region coronal jets .