  Solar coronal jets have been observed in detail since the early 1990s. While
it is clear that these jets are magnetically driven, the details of the driving
process has recently been updated. Previously it was suspected that the jets
were a consequence of magnetic flux emergence interacting with ambient coronal
field. New evidence however indicates that often the direct driver of the jets
is erupting field, often carrying cool material (a "minifilament"), that
undergoes interchange magnetic reconnection with preexisting field ([1]). More
recent work indicates that the trigger for eruption of the minifilament is
frequently cancelation of photospheric magnetic fields at the base of the
minifilament. These erupting minifilaments are analogous to the better-known
larger-scale filament eruptions that produce solar flares and, frequently,
coronal mass ejections (CMEs). A subset of coronal jets drive narrow
"white-light jets," which are very narrow CME-like features, and apparently a
few jets can drive wider, although relatively weak, "streamer-puff" CMEs. Here
we summarize these recent findings.
