On the Impact of Neutron Star Binaries Natal-Kick Distribution on the Galactic r-process Enrichment

We study the impact of the neutron star binaries’ (NSBs) natal kick distribution on the Galactic r-process enrichment. We model the growth of a Milky Way type halo based on N-body simulation results and its star formation history based on multi epoch abundance matching techniques. We consider the NSBs that merge well beyond the galaxy’s effective radius ($>2\times R_$\mathrm{e}\mathrm{f}\mathrm{f}$$) do not contribute to Galactic r-process enrichment. Assuming a power-law delay-time distribution (DTD) function ($\propto t^{-1}$) with $t_{\mathrm{m}\mathrm{i}\mathrm{n}}=30$ Myr for binaries’ coalescence timescales, and an exponential profile for their natal kick distribution with an average value of 180 km s${}^{-1}$, we show that up to $\sim$ 40% of all formed NSBs do not contribute to r-process enrichment by $z=0$, either because they merge far from the galaxy at a given redshift (up to $\sim$ 25%) or have not yet merged by today ($\sim$15%). Our result is largely insensitive to the details of the DTD function. Assuming a constant coalescence timescale of 100 Myr well approximates the adopted DTD with 30% of the NSBs not contributing to r-process enrichment. Our results, although rather dependent on the adopted natal kick distribution, represent a first step towards estimating the impact of natal kicks and DTD functions on r-process enrichment of galaxies that would need to be incorporated in the hydrodynamical simulations.