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We use cosmological, magnetohydrodynamical simulations of Milky Way-massgalaxies from the Auriga project to study their enrichment with rapid neutroncapture (r-process) elements. We implement a variety of enrichment models fromboth binary neutron star mergers and rare core-collapse supernovae. We focus onthe abundances of (extremely) metal-poor stars, most of which were formedduring the first ~Gyr of the Universe in external galaxies and later accretedonto the main galaxy. We find that the majority of metal-poor stars arer-process enriched in all our enrichment models. Neutron star merger modelsresult in a median r-process abundance ratio which increases with metallicity,whereas the median trend in rare core-collapse supernova models isapproximately flat. The scatter in r-process abundance increases for modelswith longer delay times or lower rates of r-process producing events. Ourresults are nearly perfectly converged, in part due to the mixing of gasbetween mesh cells in the simulations. Additionally, different Milky Way-massgalaxies show only small variation in their respective r-process abundanceratios. Current (sparse and potentially biased) observations of metal-poorstars in the Milky Way seem to prefer rare core-collapse supernovae overneutron star mergers as the dominant source of r-process elements at lowmetallicity, but we discuss possible caveats to our models. Dwarf galaxieswhich experience a single r-process event early in their history show highlyenhanced r-process abundances at low metallicity, which is seen both inobservations and in our simulations. We also find that the elements produced ina single event are mixed with ~10^8 Msun of gas relatively quickly,distributing the r-process elements over a large region.

Neutron star mergers and rare core-collapse supernovae as sources of r-process enrichment in simulated galaxies