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Multimessenger observations of the neutron star merger event GW170817 havere-energized the debate over the astrophysical origins of the most massiveelements via the r-process nucleosynthesis. A key aspect of such studies iscomparing astronomical observations to theoretical nucleosynthesis yields in ameaningful way. To perform realistic nucleosynthesis calculations,understanding the uncertainty in microphysics details such as nuclear reactionrates is as essential as understanding uncertainties in modeling theastrophysical environment. We present an investigation of neutron capture ratecalculations' uncertainty away from stability using the Hauser-Feshbach model.We provide a quantitative measure of the calculations' dependability when weextrapolate models of statistical properties to nuclei in an r-process network.We select several level density and gamma-ray strength models appropriate forneutron-capture and use them to calculate the reaction rate for each nucleus inthe network. We observe how statistical properties affect the theoreticalreaction rates. The rates are then sampled with the Monte Carlo technique andused in network calculations to map the range of possible r-process abundances.The results show that neutron capture rates can vary by a couple of orders ofmagnitude between calculations. Phenomenological models provide smootherresults than semi-microscopic. They cannot, however, reproduce nuclearstructure changes such as shell closures. While semi-microscopic models predictnuclear structure effects away from stability, it is not clear that theseresults are quantitatively accurate. The effect of the uncertainty on r-processyields is large enough to impede comparisons between observation andcalculations. Progress in developing better microscopic models of gammastrengths and level densities is urgently needed to improve the fidelity ofr-process models.

Propagation of Hauser-Feshbach uncertainty estimates to r-process  nucleosynthesis: Benchmark of statistical property models for neutron rich  nuclei far from stability