Astrophysical and Nuclear Physics Aspects of the r-Process

also follow the freeze-out of reactions with declining temperatures and densities explicitely. We compare the similarities and differences between the two approaches. Special emphasis is given to constraints on nuclear properties far from stability, resulting from a comparison with solar r-process abundances in either approach. In particular the behavior of shell closures is examined. In addition, investigations are presented to test whether some features can also provide clear constraints on the permitted astrophysical conditions. We discuss supernova and neutron star merger scenarios with respect to these findings. 1 Introduction The operation of an r-process is characterized by the fact that 10 to 150 neutrons per seed nucleus (in the Fe-peak or somewhat beyond) have to be available to form all heavier r-process nuclei by neutron capture. For a composition of Fe-group nuclei and free neutrons that translates into a neutron excess of j<F26.2