  Binary neutron star mergers (BNSMs) is currently the most promising source of
\textsl{r}-process thanks to the detection of GW170817. The estimated occurring
frequency and the amount of mass ejected per merger indicate that BNSMs by
itself 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 flat
trend expected from BNSMs with a standard delay time distribution (DTD)
$\propto t^{-1}$. This has led to the suggestion that either additional sources
or modification to the DTD of BNSMs is required to match the observations. We
investigate the effects of natal kicks received during the birth of neutron
star binaries on the chemical evolution of \textsl{r}-process element Eu in the
Milky 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-out
disk evolution are combined with natal kicks, BNSMs can naturally reproduce the
observed decreasing trend of [Eu/Fe] with [Fe/H] in the solar neighborhood
without the need for modification to the DTD or additional \textsl{r}-process
sources.
