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Binary neutron star mergers (BNSMs) is currently the most promising source of\textsl{r}-process thanks to the detection of GW170817. The estimated occurringfrequency and the amount of mass ejected per merger indicate that BNSMs byitself can account for all the \textsl{r}-process enrichment in the Galaxy.However, the decreasing trend of [Eu/Fe] vs [Fe/H] of disk stars for[Fe/H]$\gtrsim -1$ in the solar neighborhood is inconsistent with the flattrend expected from BNSMs with a standard delay time distribution (DTD)$\propto t^{-1}$. This has led to the suggestion that either additional sourcesor modification to the DTD of BNSMs is required to match the observations. Weinvestigate the effects of natal kicks received during the birth of neutronstar binaries on the chemical evolution of \textsl{r}-process element Eu in theMilky Way by combining the results from the galactic dynamics code\textsc{galpy} with a one-zone Galactic chemical evolution model\textsc{omega}. We show that when key inputs from simulations of the inside-outdisk evolution are combined with natal kicks, BNSMs can naturally reproduce theobserved decreasing trend of [Eu/Fe] with [Fe/H] in the solar neighborhoodwithout the need for modification to the DTD or additional \textsl{r}-processsources.

Neutron Star Mergers as the Main Source of R-process: Natal Kicks And Inside-Out Evolution to The Rescue