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A generalized method to calculate the excitation-energy dependent parityratio in the nuclear level density is presented, using the assumption ofPoisson distributed independent quasi particles combined with BCS occupationnumbers. It is found that it is crucial to employ a sufficiently large modelspace to allow excitations both from low-lying shells and to higher shellsbeyond a single major shell. Parity ratios are only found to equilibrate aboveat least 5-10 MeV of excitation energy. Furthermore, an overshooting effectclose to major shells is found where the parity opposite to the ground stateparity may dominate across a range of several MeV before the parity ratiofinally equilibrates. The method is suited for large-scale calculations asneeded, for example, in astrophysical applications. Parity distributions werecomputed for all nuclei from the proton dripline to the neutron dripline andfrom Ne up to Bi. These results were then used to recalculate astrophysicalreaction rates in a Hauser-Feshbach statistical model. Although certaintransitions can be considerably enhanced or suppressed, the impact onastrophysically relevant reactions remains limited, mainly due to the thermalpopulation of target states in stellar reaction rates.

Large-scale prediction of the parity distribution in the nuclear level density and application to astrophysical reaction rates