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A long-standing scientific puzzle has been to explain the origin of theheaviest elements in the Universe and, more particularly, the production of theelements heavier than iron up to uranium. The rapid neutron capture process (orr-process) is known to synthesize about 50\% of these heavy elements and thelong-lived actinides observed in our solar system and so-called metal-poorr-process-enhanced stars. This thesis aims to study the r-processnucleosynthesis and some of the uncertainties that still govern ourpredictions, namely, nuclear yields and heating rates. Our focus will be on ther-process in neutron star (NS) mergers, which is in the spotlight after recent``multi-messenger'' observations, including the combined detection ofgravitational waves from a NS-NS merger event and its subsequentelectromagnetic counterpart. In this work, we base our nucleosynthesiscalculations on hydrodynamical simulations of NS merger systems, which estimatethe amount of ejected mass and its properties during ejection. Through ourr-process calculations, we estimate the composition of this gravitationallyunbound material, which can contribute to the r-process enrichment of theGalaxy. This work is divided into two studies, each addressing a remaining openquestion regarding the r-process nucleosynthesis. First, a coherent study ofthe impact of neutrino interactions on the r-process element nucleosynthesisand the heating rate produced by the radioactive decay of nuclei synthesized inthe dynamical ejecta of NS-NS mergers is presented. We have studied thematerial ejected from four NS-NS merger systems based on hydrodynamicalsimulations...

The study of r-process nucleosynthesis in binary neutron star mergers: Nucleonic weak interactions and nuclear uncertainties