Some Limitations of Detailed Balance for Inverse Reaction Calculations in the Astrophysical p Process
- Conference date: 14−19 Oct 1990
- Location: Pacific Grove, California (USA)
p‐Process modeling of some rare but stable proton‐rich nuclei requires knowledge of a variety of neutron, charged particle, and photonuclear reaction rates at temperatures of 2 to 3×109 °K. Detailed balance is usually invoked to obtain the stellar photonuclear rates, in spite of a number of well‐known constraints. In this work we attempt to calculate directly the stellar rates for (γ,n) and (γ,α) reactions on 151Eu. These are compared with stellar rates obtained from detailed balance, using the same input parameters for the stellar (n,γ) and (α,γ) reactions on 150Eu and 147Pm, respectively. The two methods yielded somewhat different results, which will be discussed along with some sensitivity studies.
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