  We study the formation of coronal jets through numerical simulation of the
emergence of a twisted magnetic flux rope into a pre-existing open magnetic
field. Reconnection inside the emerging flux rope in addition to that between
the emerging and pre-existing fields give rise to the violent eruption studied.
The simulated event closely resembles the coronal jets ubiquitously observed by
Hinode/XRT and demonstrates that heated plasma is driven into the extended
atmosphere above. Thermal conduction implemented in the model allows us to
qualitatively compare simulated and observed emission from such events. We find
that untwisting field lines after the reconnection drive spinning outflows of
plasma in the jet column. The Poynting flux in the simulated jet is dominated
by the untwisting motions of the magnetic fields loaded with high-density
plasma. The simulated jet is comprised of spires of untwisting field that are
loaded with a mixture of cold and hot plasma and exhibit rotational motion of
order 20 km/s and match contemporary observations.
