Abstract
The astrophysical r-process produces about half of the elements heavier than iron in the Universe and all of the transactinides. Recently neutron star mergers have been identified as one site of r-process nucleosynthesis. Simulations of this site and the associated nucleosynthesis requires essential nuclear input, ranging from the Equation of State (EoS) of nuclear matter at extreme densities and temperatures to the properties of very neutron-rich nuclei. Many of these quantities have to be modeled, however, constrained by a steadily increasing amount of experimental data. This manuscript summarizes the knowledge of nuclear input required for r-process studies in neutron star mergers.
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