Coulomb dissociation reactions on Mo isotopes for astrophysical applications

Photo-dissociation reactions are important for explaining abundances of the nuclei produced via the so-called p-process, which takes place in Type II supernova explosions. Theoretical calculations of the isotopic p-nuclei abundances require a huge reaction network linking thousands of isotopes, where most of the reaction rates have to be derived from theory. However, it's important that as many rates as possible are measured experimentally to provide pivot points for the calculations. In all present models, a significant underproduction of Mo and Ru p-nuclides is observed. At the same time, 92Mo has one of the highest cosmic abundances of all p-nuclei. At the SIS/FRS/LAND facility at GSI (γ,n) reactions on the stable 92,94,100Mo and the unstable 93Mo isotopes were studied. The experiment was performed in inverse kinematics using the Coulomb dissociation method. The setup provides a possibility to identify the outgoing nucleus with respect to A and Z. Together with a neutron hit in the LAND detector, it allows to tag the proper reaction channel. Gamma-rays emitted by the de-exciting nucleus were measured with the 2π CsI gamma spectrometer. Current status of the analysis, with a focus on the gamma detection, is presented.