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A model for the explosive synthesis of p nuclei

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Abstract

A model for the synthesis of p nuclei during a supernova explosion of a 25 M ⊙ star is presented. Its main distinguishing feature is the requirement that the yield of s nuclei after the explosion fully correspond to the observed solar-system abundances. A fully self-consistent system of kinetic equations including (n, γ), (p, γ), (α, γ), (p, n), (α, n), and (α, p) reactions and their reverse reactions was solved for the mass fractions of various nuclei, taking into account the dynamics of the propagation of the supernova shock. The absolute abundances of the p nuclei are calculated, and the role of helium layers in the supernova in the synthesis of r nuclei is analyzed. The calculated abundances of p nuclei are in overall good agreement with observations. This makes it possible to synthesize 113In, 138La, and some other problematic isotopes, although the problem of synthesizing molybdenum and ruthenium remains.

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Authors and Affiliations

  1. Voronezh State University, Voronezh, Russia

    E. M. Babishov & I. V. Kopytin

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  1. E. M. Babishov
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  2. I. V. Kopytin
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Original Russian Text © E.M. Babishov, I.V. Kopytin, 2006, published in Astronomicheskiĭ Zhurnal, 2006, Vol. 83, No. 7, pp. 638–648.

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Babishov, E.M., Kopytin, I.V. A model for the explosive synthesis of p nuclei. Astron. Rep. 50, 569–578 (2006). https://doi.org/10.1134/S1063772906070079

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  • DOI: https://doi.org/10.1134/S1063772906070079

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