Hannover 2013 – scientific programme

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A: Fachverband Atomphysik

A 44: 100 Years of Mass Spectrometry 1

A 44.3: Invited Talk

Friday, March 22, 2013, 12:00–12:30, E 415

High-accuracy mass measurements for nuclear astrophysics — •Susanne Kreim — CERN, Genf, Schweiz — Max-Planck- Institut für Kernphysik, Heidelberg, Deutschland

The mass of a nucleus delivers the binding energy giving insight into structural effects throughout the nuclear chart from the lightest to the heaviest element. Precision measurements of masses far away from the valley of stability are also important to understand nuclear stability. Both notions are crucial for a correct description of astrophysical processes.

The so-called rapid neutron-capture process (r-process) of stellar nucleosynthesis is held responsible for the production of the heavy elements. However, the astrophysical site for a successful r-process has not been identified yet. A possible theory, alternative to the supernova-induced r-process, is the decompression of neutron-star matter by its merger with another neutron star. In the neutron-star crust, exotic rare isotopes become so-called equilibrium nuclei and can contribute to the elemental abundance. Another mechanism of stellar nucleosynthesis is the rp-process, rapid proton-capture process, which takes place on the proton-rich side of the valley of stability and originates in x-ray bursts.

Precise mass values are input parameters that constrain the models for the stellar creation of elements. Whenever masses are not (yet) available, one has to rely on mass models for the nuclei participating in astrophysical processes. New masses offer the required test bench for the predictive power of models. In this contribution, recently performed mass measurements as well as still desired ones will be discussed.