  Comparisons between the predicted abundances of short-lived r-nuclides
(107Pd, 129I, 182Hf, and 244Pu) in the interstellar medium (ISM) and the
observed abundances in the early solar system (ESS) conclusively showed that
these nuclides cannot simply be derived from galactic chemical evolution (GCE)
if synthesized in a unique stellar environment. It was thus suggested that two
di erent types of stars were responsible for the production of light and heavy
r-nuclides. Here, new constraints on the 244Pu=238U production ratio are used
in an open nonlinear GCE model. It is shown that the two r-process scenario
cannot explain the low abundance of 244Pu in the ESS and that this requires
either than actinides be produced at an additional site (A-events) or more
likely, that 129I and 244Pu be inherited from GCE and 107Pd and 182Hf be
injected in the ESS by the explosion of a nearby supernova.
