  We study 14 large solar jets observed in polar coronal holes. In EUV movies
from SDO/AIA, each jet appears similar to most X-ray jets and EUV jets that
erupt in coronal holes, but each is exceptional in that it goes higher than
most, so high that it is observed in the outer corona beyond 2.2 RSun in images
from the SOHO/LASCO/C2 coronagraph. From AIA He II 304 {\AA} movies and
LASCO/C2 running-difference images of these high-reaching jets, we find: (1)
the front of the jet transits the corona below 2.2 RSun at a speed typically
several times the sound speed; (2) each jet displays an exceptionally large
amount of spin as it erupts; (3) in the outer corona, most of the jets display
measureable swaying and bending of a few degrees in amplitude; in three jets
the swaying is discernibly oscillatory with a period of order 1 hour. These
characteristics suggest that the driver in these jets is a magnetic-untwisting
wave that is basically a large-amplitude (i.e., non-linear) torsional Alfven
wave that is put into the reconnected open field in the jet by interchange
reconnection as the jet erupts. From the measured spinning and swaying we
estimate that the magnetic-untwisting wave loses most of its energy in the
inner corona below 2.2 RSun. We point out that the torsional waves observed in
Type-II spicules might dissipate in the corona in the same way as the
magnetic-untwisting waves in our big jets and thereby power much of the coronal
heating in coronal holes.
