Bereiche | Tage | Auswahl | Suche | Aktualisierungen | Downloads | Hilfe

A: Fachverband Atomphysik

A 31: Fathoming Stellar Evolution with Laboratory Precision SYSE (with MS, Q, MO, EP)

A 31.1: Hauptvortrag

Mittwoch, 19. März 2014, 14:00–14:30, Audimax

Addressing open questions of stellar evolution with laboratory experiments — •Almudena Arcones — Technische Universität Darmstadt, Institut für Kernphysik, Germany — GSI Helmholtzzentrum für Schwerionenforschung GmbH, Germany

After several hydrostatic burning stages, massive stars end their life as core-collapse supernova explosions. These high-energy events enrich the interstellar medium with elements formed during the stellar life, produce new heavy elements, and are the birthplace of neutron stars. An exciting stage in the life of neutron stars is the merger with another neutron star or a black hole. Both, core-collapse supernovae and neutron star mergers are sources of heavy elements in the universe. Elements from Sr to Ag can be synthesized in neutrino-driven winds after core-collapse supernovae via charged particle reactions through nuclei relatively close to stability. Heavier elements are produced in rare supernovae and neutron star mergers via the rapid neutron capture process (r-process). In this talk, the role of nuclear masses will be presented showing how further experimental information is highly necessary to constrain the nucleosynthesis and the still uncertain theoretical models. In addition, the r-process can be directly observed after a neutron star merger in the form of a light curve (kilonova) triggered by the radioactive decay of neutron-rich nuclei. In order to obtain the maximum information from such events more atomic data are required to calculate the opacities for r-process ejecta. Therefore, precision experiments are critical to understand supernova, neutron star mergers and their implication in the chemical history of the universe.