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Coronal jets are transient narrow features in the solar corona that originatefrom all regions of the solar disk: active regions, quiet sun, and coronalholes. Recent studies indicate that at least some coronal jets in quiet regionsand coronal holes are driven by the eruption of a minifilament following fluxcancellation at a magnetic neutral line. We have tested the veracity of thatview by examining 60 random jets in quiet regions and coronal holes usingmultithermal (304 A, 171 A, 193 A, and 211 A) extreme ultraviolet (EUV) imagesfrom 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 aminifilament eruption triggered by flux cancellation at the neutral line. The60 jets have a mean base diameter of 8800 +/- 3100 km and a mean duration of 9+/-3.6 minutes. These observations confirm that minifilament eruption is thedriver and magnetic flux cancellation is the primary trigger mechanism for mostcoronal hole and quiet region coronal jets.

Magnetic Flux Cancellation as the Trigger Mechanism of Solar Coronal Jets