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

Abstract

Abstract Solar twins, i.e., stars that are nearly identical to the Sun, including their metallicities, in the solar vicinity show ages widely distributed from 0 to 10 Gyr. This fact matches the orbital history of solar twins in the new paradigm of galactic dynamics, in which stars radially move on the disk when they encounter transient spiral arms. This finding suggests that older twins were born closer to the Galactic center and traveled a longer distance to reach their present location, according to the hypothesis that chemical enrichment occurs more quickly and that solar metallicity is attained on a shorter timescale with a decreasing Galactocentric distance (R GC). We show that abundance patterns covering a wide range of heavy elements for solar twins sharing similar ages are identical and that their variation among different age groups can be understood on the basis of the age–R GC connection within the framework of Galactic chemical evolution. This study identifies the Galactic bulge as the birthplace of the oldest solar twins. Based on this scheme, we find that the relation between [r-process/Fe] and R GC for the inner Galactic region is incompatible with the hypothesis of a sole site for r-process production, that is, neutron star mergers, whose delay time distribution could be approximated by the power-law form (∝ t n ). Alternatively, this relation suggests the presence of two distinct sites for r-process production: short-lived massive stars, ending with specific core-collapse supernovae, and neutron star mergers that are heavily inclined to emerge with longer delay times, as represented by n = 0−0.5.