  The highly r-process enhanced (r-II) metal-poor halo stars we observe today
could play a key role in understanding early ultra-faint dwarf galaxies, the
smallest building blocks of the Milky Way. If a significant fraction of
metal-poor r-II halo stars originated in the ultra-faint dwarf galaxies that
merged to help form the Milky Way, observations of r-II stars could help us
study these now-destroyed systems and probe the formation history of our
Galaxy. To conduct our initial investigation into this possible connection, we
use high-resolution cosmological simulations of Milky-Way-mass galaxies from
the Caterpillar suite in combination with a simple, empirically motivated
treatment of r-process enrichment. We determine the fraction of metal-poor halo
stars that could have formed from highly r-process enhanced gas in
now-destroyed low-mass ultra-faint dwarf galaxies, the simulated r-II fraction,
and compare it to the "as observed" r-II fraction. We find that the simulated
fraction, f_{r-II,sim} ~ 1-2%, can account for around half of the "as observed"
fraction, f_{r-II,obs} ~ 2-4%. The "as observed" fraction likely overrepresents
the fraction of r-II stars due to incomplete sampling, though, meaning
f_{r-II,sim} likely accounts for more than half of the true f_{r-II,obs}.
Further considering some parameter variations and scatter between individual
simulations, the simulated fraction can account for around 20-80% of the "as
observed" fraction.
