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We examine the initiation of 10 coronal jet eruptions in quiet regions on thecentral disk, thereby avoiding near-limb spicule-forest obscuration of theslow-rise onset of the minifilament eruption. From the SDO/AIA 171A12-second-cadence movie of each eruption, we (1) find and compare the starttimes of the minifilament's slow rise, the jet-base bright point, the jet-baseinterior brightening, and the jet spire, and (2) measure the minifilament'sspeed at the start and end of its slow rise. From (a) these data, (b) priorobservations showing that each eruption was triggered by magnetic fluxcancelation under the minifilament, and (c) the breakout-reconnection currentsheet observed in one eruption, we confirm that quiet-region jet-makingminifilament eruptions are miniature versions of CME-making filament eruptions,and surmise that in most quiet region jets: (1) the eruption starts beforerunaway reconnection starts, (2) runaway reconnection does not start until theslow-rise speed is at least about 1 km/s, and (3) at and before eruption onsetthere is no current sheet of appreciable extent. We therefore expect: (i) manyCME-making filament eruptions are triggered by flux cancelation under thefilament, (ii) emerging bipoles seldom, if ever, directly drive jet productionbecause the emergence is seldom, if ever, fast enough, and (iii) at aseparatrix or quasi-separatrix in any astrophysical setting of magnetic fieldin low-beta plasma, a current sheet of appreciable extent can be built onlydynamically by a magnetohydrodynamic convulsion of the field, not byquasi-static gradual converging of the field.

Onset of Magnetic Explosion in Solar Coronal Jets in Quiet Regions on the Central Disk