Sequence of cartoons portraying the topology and reconnection of the magnetic field in the standard model for solar coronal jets. Only a few representative field lines (blue or red) are drawn. Left: the field configuration before the burst of reconnection that produces the jet. The dashed oval is the polarity inversion line around the positive flux of the emerging magnetic arch. The nearly unstable portion of the current sheet between the emerging closed field and the ambient open field is represented by the curved black line segment. Middle: the growing jet early in the burst of reconnection that occurs in the disrupted current sheet and that is symbolized here by the slanted X. Red field lines are reconnected ones that have reconnection-heated hot plasma on them. Blue field lines either have yet to or will not undergo reconnection. Right: the decaying jet immediately after the burst of reconnection has ended.