  Jets (transient/collimated plasma ejections) occur frequently throughout the
solar corona and contribute mass/energy to the corona and solar wind. By
combining numerical simulations and high-resolution observations, we have made
substantial progress recently on determining the energy buildup and release
processes in these jets. Here we describe a study of 27 equatorial coronal-hole
jets using Solar Dynamics Observatory/AIA and HMI observations on 2013 June
27-28 and 2014 January 8-10. Out of 27 jets, 18 (67%) are associated with
mini-filament ejections; the other 9 (33%) do not show mini-filament eruptions
but do exhibit mini-flare arcades and other eruptive signatures. This indicates
that every jet in our sample involved a filament-channel eruption. From the
complete set of events, 6 jets (22%) are apparently associated with tiny
flux-cancellation events at the polarity inversion line, and 2 jets (7%) are
associated with sympathetic eruptions of filaments from neighboring bright
points. Potential-field extrapolations of the source-region photospheric
magnetic fields reveal that all jets originated in the fan-spine topology of an
embedded bipole associated with an extreme ultraviolet coronal bright point.
Hence, all our jets are in agreement with the breakout model of solar
eruptions. We present selected examples and discuss the implications for the
jet energy build-up and initiation mechanisms.
