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We have used the galaxy modeling algorithm \texttt{GravPot16}, to explore themore probable orbital elements of a sample of 64 selected N-rich stars acrossthe Milky Way. Using the newly measured proper motions from \texttt{Gaia} DR2with existing line-of-sight velocities from APOGEE-2 survey andspectrophotometric distance estimations from the \texttt{StarHorse}. We adopteda set of high-resolution particle simulations evolved in the same steady-stateGalactic potential model with a bar, in order to identify the groups of N-richstars that have a high probability of belonging to the bulge/bar, disk, andstellar halo component. We find that the vast majority of the N-rich stars showtypically maximum height from the Galactic plane below 3 kpc, and developrather eccentric orbits (\textit{e}$>$0.5), which means these stars appear tohave bulge/bar-like and/or halo-like orbits. We also show that $\sim66$\% ofthe selected N-rich stars currently lives in the inner Galaxy inside thecorotation radius (C.R.), whilst $\sim14$\% of the N-rich star resides inhalo-like orbits. Among the N-rich in the inner Galaxy, $\sim27\%$ of themshare orbital properties in the boundary between bulge/bar and disk, dependingon the bar pattern speeds. Our dynamical analysis also indicates that some ofthe N-rich are likely halo interlopers and therefore suggest that halocontamination is not insignificant within the bulge area.

Dynamical Orbital classification of selected N-rich stars with \textit{Gaia} DR2 astrometry