Abstract
The p nucleus 92 Mo is believed to be mainly produced through photodisintegration reactions in type II supernovae. However, this production scenario cannot solely account for the observed solar relative isotopic abundance of 92 Mo. Additional production scenarios have been suggested to explain this discrepancy. One of these scenarios could be the production of 92 Mo in type Ia supernovae via a chain of proton-capture reactions. To verify this scenario, an accurate knowledge of the involved reaction rates is important. We measured the cross section of 90 Zr(p, γ ) reaction using an enriched 90 Zr target by means of in-beam γ -ray spectroscopy in the energy range between 3.6MeV and 5.1MeV. Since the reactions 90 Zr(p, γ ) and 91 Zr(p,n) produce the same nucleus, the contributions of both reactions have to be disentangled. This procedure is explained in this contribution in detail.
Highlights
The elements heavier than iron are mainly produced by neutron-capture reactions within the s and r processes [1, 2]
Even so there are about 35 isotopes, called the p nuclei, that are shielded from the s and r processes by stable or long lived isotopes which have to be produced by other processes [3]
While the relative abundances of most p nuclei can be explained by the γ process, it cannot explain the high isotopic abundance of I% = 14.84% of the p nucleus 92Mo [5]
Summary
The elements heavier than iron are mainly produced by neutron-capture reactions within the s and r processes [1, 2]. The in-beam γ-ray spectroscopy technique was used to measure the corresponding cross section. The radiative proton-capture cross section of 90Zr was measured using high-resolution in-beam γ-ray spectroscopy.
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