  It is well known that stars move away from their birth location over time via
radial migration. This dynamical process makes computing the correct chemical
evolution, e.g., metallicity gradients, of galaxies very difficult. This
dynamical process makes inferring the chemical evolution of observed galaxies
from their measured abundance gradients very difficult. One way to account for
radial migration is to infer stellar birth radii for individual stars. Many
attempts to do so have been performed over the last years, but are limited to
the Milky Way as computing the birth position of stars requires precise
measurements of stellar metallicity and age for individual stars that cover
large Galactic radii. Fortunately, recent and future surveys will provide
numerous opportunities for inferring birth radii for external galaxies such as
the Large Magellanic Cloud (LMC). In this paper, we investigate the possibility
of doing so using the NIHAO cosmological zoom-in simulations. We find that it
is theoretically possible to infer birth radii with a ~ 25% median uncertainty
for individual stars in galaxies with i) orderliness of the orbits, $\langle
v_\phi \rangle/\sigma_{v} >$ 2, ii) a dark matter halo mass greater or equal to
approximately the LMC mass (~ 2 x 10$^{11} M_\odot$), and iii) after the
average azimuthal velocity of the stellar disk reaches ~70% of its maximum.
From our analysis, we conclude that it is possible and useful to infer birth
radii for the LMC and other external galaxies that satisfy the above criteria.
