  During the last several decades, there have been a number of advances in
understanding the rapid neutron-capture process (i.e., the r-process). These
advances include large quantities of high-resolution spectroscopic abundance
data of neutron-capture elements, improved astrophysical models, and
increasingly more precise nuclear and atomic physics data. The elemental
abundances of the heavy neutron-capture elements, from Ba through the third
r-process peak, in low-metallicity ([Fe/H] <~ -2.5) Galactic halo stars are
consistent with the scaled (i.e., relative) solar system r-process abundance
distribution. These abundance comparisons suggest that for elements with Z >=
56 the r-process is robust--appearing to operate in a relatively consistent
manner over the history of the Galaxy--and place stringent constraints on
r-process models. While not yet identified, neutron-rich ejecta outside of the
core in a collapsing (Type II, Ib) supernova continues to be a promising site
for the r-process. Neutron star binary mergers might also be a possible
alternative site. Abundance comparisons of lighter n-capture elements in halo
stars show variations with the scaled solar r-process curve and might suggest
either multiple r-process sites, or, at least, different synthesis conditions
in the same astrophysical site. Constraints on r-process models and clues to
the progenitors of the halo stars--the earliest generations of Galactic
stars--are also provided by the star-to-star abundance scatter of [Eu/Fe] at
low metallicities in the early Galaxy. Finally, abundance observations of
long-lived radioactive elements (such as Th and U) produced in the r-process
can be used to determine the chronometric ages of the oldest stars, placing
constraints on the lower limit age estimates of the Galaxy and the Universe.
