  Small, impulsive jets commonly occur throughout the solar corona, but are
especially visible in coronal holes. Evidence is mounting that jets are part of
a continuum of eruptions that extends to much larger coronal mass ejections and
eruptive flares. Because coronal-hole jets originate in relatively simple
magnetic structures, they offer an ideal testbed for theories of energy buildup
and release in the full range of solar eruptions. We analyzed an equatorial
coronal-hole jet observed by SDO/AIA on 09 January 2014, in which the
magnetic-field structure was consistent with the embedded-bipole topology that
we identified and modeled previously as an origin of coronal jets. In addition,
this event contained a mini-filament, which led to important insights into the
energy storage and release mechanisms. SDO/HMI magnetograms revealed footpoint
motions in the primary minority-polarity region at the eruption site, but show
negligible flux emergence or cancellation for at least 16 hours before the
eruption. Therefore, the free energy powering this jet probably came from
magnetic shear concentrated at the polarity inversion line within the embedded
bipole. We find that the observed activity sequence and its interpretation
closely match the predictions of the breakout jet model, strongly supporting
the hypothesis that the breakout model can explain solar eruptions on a wide
range of scales.
