The origin of heavy elements: a nuclear physics and astrophysics challenge
Prof. Dr. Almudena Arcones (TU Darmstadt)

Where in the universe are heavy elements synthesized? How are these elements produced? These are two exciting and interdisciplinary questions in nuclear astrophysics today. The favored candidates are core-collapse supernovae and neutron star mergers where extreme conditions enable the rapid neutron capture process (r-process). Recent advances in hydrodynamic simulations with improved microphysics can be combined with observations of the oldest stars to bring new insights about the astrophysical sites where heavy elements are produced. In nuclear physics, a new era for extreme neutron-rich isotopes will start with new facilities like FAIR. In this talk, we will discuss new results on nucleosynthesis in core-collapse supernovae and neutrino-driven winds that produce elements up to silver. Because the synthesis of these elements occurs closer to stability, in the near future, the nuclear physics uncertainties will be reduced by experiments. This will uniquely allow us to combine observations and nucleosynthesis calculations to constrain the astrophysical conditions in neutrino-driven winds and thus gain new insights about core-collapse supernovae. In addition, we will discuss the production of all r-process elements (from the first to the third peak) in neutron star mergers. The radioactive decay of neutron-rich nuclei triggers a electromagnetic signal in mergers known as kilonova. This was potentially observed in 2013 after a short gamma ray burst, associated with a neutron star merger. Nucleosynthesis in mergers takes place far away from stability and our sensitivity studies show the importance of, in particular, nuclear masses and fission properties. Combining nuclear physics experiment and theory, with long-time simulations of neutron star mergers, we will be in a great position to understand the origin of heavy elements.