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We investigate the origin in the early Solar System of the short-livedradionuclide 244Pu (with a half life of 80 Myr) produced by the rapid (r)neutron-capture process. We consider two large sets of r-processnucleosynthesis models and analyse if the origin of 244Pu in the ESS isconsistent with that of the other r and slow (s) neutron-capture processradioactive nuclei. Uncertainties on the r-process models come from both thenuclear physics input and the astrophysical site. The former strongly affectsthe ratios of isotopes of close mass (129I/127I, 244Pu/238U, and 247Pu/235U).The 129I/247Cm ratio, instead, which involves isotopes of a very differentmass, is much more variable than those listed above and is more affected by thephysics of the astrophysical site. We consider possible scenarios for theevolution of the abundances of these radioactive nuclei in the galacticinterstellar medium and verify under which scenarios and conditions solutionscan be found for the origin of 244Pu that are consistent with the origin of theother isotopes. Solutions are generally found for all the possible differentregimes controlled by the interval ($\delta$) between additions from the sourceto the parcel of interstellar medium gas that ended up in the Solar System,relative to decay timescales. If r-process ejecta in interstellar medium aremixed within a relatively small area (leading to a long $\delta$), we derivethat the last event that explains the 129I and 247Cm abundances in the earlySolar System can also account for the abundance of 244Pu. Due to its longerhalf life, however, 244Pu may have originated from a few events instead of oneonly. If r-process ejecta in interstellar medium are mixed within a relativelylarge area (leading to a short $\delta$), we derive that the time elapsed fromthe formation of the molecular cloud to the formation of the Sun was 9-16 Myr.

Origin of Plutonium-244 in the Early Solar System