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Merging neutron star binaries are prime candidate sources for heavy r-processnucleosynthesis. The amount of heavy r-process material is consistent with themass ejection and rates of mergers, and abundances of relic radioactivematerials suggest that heavy r-process material is produced in rare events.Observations of possible macronovae provide further support for this model.Still, some concerns remain. One is the observation of heavy r-process elementsin Ultra Faint Dwarf (UFD) galaxies. The escape velocities from UFDs are sosmall that the natal kicks, taking place at neutron stars birth, might ejectsuch binaries from UFDs. Furthermore the old stellar populations of UFDsrequires that r-process nucleosynthesis must have taken place very early on,while it may take several Gyr for compact binaries to merge. This last problemarises also within the Milky Way where heavy r-process materials has beenobserved in some low metallicity stars. We show here that since a significantfraction of neutron star binaries form with a very small proper motion thosewon't be ejected even from a UFD. Furthermore, a significant fraction of thesebinaries merge within a few hundred Myr and in some cases the merger time iseven shorter than a hundred Myr. This population of "rapid mergers" explainsthe appearance of heavy r-process material in both UFDs and in the Milky Way.

Natal Kicks and Time Delays in Merging Neutron Star Binaries - Implications for r-process nucleosynthesis in Ultra Faint Dwarfs and in the Milky Way