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The origin of r-process elements remains unidentified and still puzzles us.The recent discovery of evidence for the ejection of r-process elements from ashort-duration gamma-ray burst singled out neutron star mergers (NSMs) as theirorigin. In contrast, core-collapse supernovae are ruled out as the main originof heavy r-process elements (A>110) by recent numerical simulations. However,the properties characterizing NSM events - their rarity and high yield ofr-process elements per event - have been claimed to be incompatible with theobserved stellar records on r-process elements in the Galaxy. We add to thispicture with our results, which show that the observed constant [r-process/H]ratio in faint dwarf galaxies and one star unusually rich in r-process in theSculptor galaxy agree well with this rarity of NSM events. Furthermore, wefound that a large scatter in the abundance ratios of r-process elements toiron in the Galactic halo can be reproduced by a scheme that incorporates anassembly of various protogalactic fragments, in each of which r-processelements supplied by NSMs pervade the whole fragment while supernovaedistribute heavy elements only inside the regions swept up by the blast waves.Our results demonstrate that NSMs occurring at Galactic rate of 12-23 per Myrare the main site of r-process elements, and we predict the detection ofgravitational waves from NSMs at a high rate with upcoming advanced detectors.

Enrichment history of r-process elements shaped by a merger of neutron star pairs