  Growing interests in the chemical feature of r-process elements among nearby
disk stars represented by the [Eu/Fe] vs. [Fe/H] diagram have sprouted since it
can assess the origin of r-process elements through the comparison with
theoretical models, including a test as to if neutron star mergers can be the
major site of r-process nucleosynthesis. On the other hand, recent studies
reveal that local chemistry is strongly coupled with the dynamics of Galactic
disk, which predicts that stars radially move on the disk where the observed
elemental feature is different at various Galactocentric distances. Here, we
show that radial migration of stars across the Galactic disk plays a crucial
role in shaping the r-process abundance feature in the solar vicinity. In this
proposed scenario, we highlight the importance of migration from the outer disk
where [r-process/Fe] of some old stars is predicted to be enhanced to the level
beyond the expectation from the observed Galactic Fe and Eu radial gradient,
which results in a large span of [r-process/Fe] among nearby disk stars. The
variation in the [r-process/Fe] ratio seen across the Galactic disk as well as
in dwarf galaxies may be an outcome of different stellar initial mass functions
which change the occurrence frequency between supernovae leaving behind neutron
stars and ones ending with black holes. Here we propose that enhancement in
[Eu/Fe] is attributed to the initial mass function lacking high-mass stars such
as > 25 solar masses in the scheme for which neutron star mergers are a major
source of r-process elements.
