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The recent detection of 60Fe in the cosmic rays provides conclusive evidencethat there is a recently synthesized component (few MY) in the GCRs (Binns etal. 2016). In addition, these nuclei must have been synthesized and acceleratedin supernovae near the solar system, probably in the Sco-Cen OB associationsubgroups, which are about 100 pc distant from the Sun. Recent theoretical workon the production of r-process nuclei appears to indicate that it is difficultfor SNe to produce the solar system abundances relative to iron of r-processelements with high atomic number (Z), including the actinides (Th, U, Np, Pu,and Cm). Instead, it is believed by many that the heaviest r-process nuclei, orperhaps even all r-process nuclei, are produced in binary neutron star mergers.Since we now know that there is at least a component of the GCRs that has beenrecently synthesized and accelerated, models of r-process production by SNe andBNSM can be tested by measuring the relative abundances of these ultra-heavyr-process nuclei, and especially the actinides, since they are radioactive andprovide clocks that give the time interval from nucleosynthesis to detection atEarth. Since BNSM are believed to be much less frequent in our galaxy than SNe(roughly 1000 times less frequent, the ratios of the actinides, each with theirown half-life, will enable a clear determination of whether the heaviestr-process nuclei are synthesized in SNe or in BNSM. In addition, the r-processnuclei for the charge range from 34 to 82 can be used to constrain models ofr-process production in BNSM and SNe. Thus, GCRs become a multi-messengercomponent in the study of BNSM and SNe.

Ultra-heavy cosmic-ray science--Are r-process nuclei in the cosmic rays produced in supernovae or binary neutron star mergers?