Astrophysical reaction rates in an average direct capture model.

All elements heavier than iron like gold, silver, lead or uranium have been synthesised through neutron capture in red giants (final stage of stars) or in supernovae (star explosions). In the present research project some of these nuclear reactions have been investigated exemplary. Furthermore, the corresponding reaction rates have been calculated. These reaction rates are the input parameters for computerised star evolution simulations, in which abundances for the production of all elements heavier than iron in Red Giants are calculated. In the present research project the dependence of the reaction rates for neutron capture on different nuclear structure models have been investigated. It could be shown that the reaction rates for the nuclear structure model being used in this project are larger than the previously used models. This should also have consequences for future network calculations for the creation of elements in red giants or supernovae.