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Solar twins, i.e., stars that are nearly identical to the Sun, includingtheir metallicities, in the solar vicinity show ages widely distributed from0-10 Gyr. This fact matches the orbital history of solar twins in the newparadigm of galactic dynamics, in which stars radially move on the disk whenthey encounter transient spiral arms. This finding suggests that older twinswere born closer to the Galactic center and traveled a longer distance to reachtheir present location, according to the hypothesis that chemical enrichmentoccurs more quickly and that solar metallicity is attained on a shortertimescale with a decreasing Galactocentric distance (R_GC). We show thatabundance patterns covering a wide range of heavy elements for solar twinssharing similar ages are identical and that their variation among different agegroups can be understood on the basis of the age-R_GC connection within theframework of Galactic chemical evolution. This study identifies the Galacticbulge as the birthplace of the oldest solar twins. Based on this scheme, wefind that the relation between [r-process/Fe] and R_GC for the inner Galacticregion is incompatible with the hypothesis of a sole site for r-processproduction, that is, neutron star mergers, whose delay time distribution couldbe approximated by the power-law form (proportional to t^n). Alternatively,this relation suggests the presence of two distinct sites for r-processproduction: short-lived massive stars, ending with specific core-collapsesupernovae, and neutron star mergers that are heavily inclined to emerge withlonger delay times, as represented by n=0-0.5.

Two Sites of r-Process Production Assessed on the Basis of the Age-tagged Abundances of Solar Twins