The hypothesis is explored that the extinct radioactivities found in primitive solar system material were all primarily injected into the system by a triggering supernova shock wave that initiated the formation of the system. Some of the radioactivities are made by the r-process, and much of the discussion will center on problems of understanding the apparently dual nature of this process. The theory developed to explain jets and outflows from accretion disks is applied to the supernova core collapse process, and it is argued that the neutrino-driven neutron wind is loaded onto the twisting magnetic lines of force emerging from the neutron star remnant and forms the body of the jet material ejected from the supernova remnant neutron star. The ejection velocity can be expected to vary over the cross section of the jet, leading to variations in the neutron/seed ratio; a high ratio leads to fission recycling in the r-process and the high-A portion of the r-process abundance curve, but a low ratio forms the low-A portion of the curve. This r-process jet, when colliding with the outgoing supernova envelope, may produce significant amounts of deuterium in the galaxy, together with the Li, Be, and B isotopes hitherto attributed to cosmic ray spallation in the galaxy, and the Be 10 extinct radioactivity in the early solar system.