Studies attempting to quantify the sensitivity of the r-process abundances
to nuclear input have to cope with the fact that the theoretical models they
rely on, rarely come with confidence intervals. This problem has been dealt
with by either estimating these intervals and propagating them statistically to
the final abundances using reaction networks within simplified astrophysical
models, or by running more realistic astrophysical simulations using different
nuclear-physics models consistently for all the involved nuclei. Both of these
approaches have their strengths and weaknesses. In this work, we use the
reaction network code SkyNet to run r-process calculations for five
trajectories using 49 different neutron-capture rate models. Our results shed
light on the importance of taking into account shell effects and pairing
correlations in the network calculations.Comment: 11 pages, 7 figure