  We report observations of homologous coronal jets and their coronal mass
ejections (CMEs) observed by instruments onboard the Solar Dynamics Observatory
(SDO) and Solar and Heliospheric Observatory (SOHO) spacecraft. The homologous
jets originated from a location with emerging and canceling magnetic field at
the southeast edge of the giant active region (AR) of 2014 October, NOAA 12192.
This AR produced in its interior many non-jet major flare eruptions (X and M
class) that made no CME. During 20-27 October, in contrast to the major-flare
eruptions in the interior, six of the homologous jets from the edge resulted in
CMEs. Each jet-driven CME( ~200-300 kms) was slower-moving than most CMEs; had
angular width (20-50 degree) comparable to that of the base of a coronal
streamer straddling the AR; and was of the `streamer-puff' variety, whereby the
preexisting streamer was transiently inflated but not destroyed by the passage
of the CME. Much of the transition-region-temperature plasma in the
CME-producing jets escaped from the Sun, whereas relatively more of the
transition-region plasma in non-CME-producing jets fell back to the solar
surface. Also, the CME-producing jets tended to be faster and longer-lasting
than the non-CME-producing jets. Our observations imply: each jet and CME
resulted from reconnection opening of twisted field that erupted from the jet
base; and the erupting field did not become a plasmoid as previously envisioned
for streamer-puff CMEs, but instead the jet-guiding streamer-base loop was
blown out by the loop's twist from the reconnection.
