Production of Intermediate Mass Elements in the High-Entropy Supernova Bubble

Details Production of Intermediate Mass Elements in the High-Entropy Supernova Bubble Production of Intermediate Mass Elements in the High-Entropy Supernova Bubble

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993metic..28q.365h&link_type=abstract

Meteoritics, vol. 28, no. 3, volume 28, page 365

Astronomy and Astrophysics

Astrophysics

Nucleosynthesis, Supernova

Scientific paper

Recently much interest has been generated by the study of the neutron-rich alpha-rich freeze out that is expected to occur in the neutrino-energized wind that emerges from the nascent neutron star in a Type II supernova [4]. Such a wind is expected to have high entropy and relatively low electron-to-baryon ratio, Y(sub)e, due to the interaction of the electron neutrinos and anti-neutrinos with the protons and neutron escaping in the wind. It was recognized by [4] that such conditions provide an attractive site for the astrophysical r-process, as well as contributing to the Galactic production of some intermediate mass elements that are usually ascribed to the astrophysical s- and p- processes. Meyer et al. [3] and [1] demonstrated that a solar-system distribution of r-process nuclei might be produced for an interesting range of entropy and Y(sub)e. In this paper we study the production of intermediate mass elements in this high-entropy wind and discuss the implications for isotopic anomalies found in meteorites. The calculations are performed with the help of a single reaction network that is able to describe the establishment of nuclear statistical equilibrium, the charged-particle reaction freeze-out, and the subsequent neutron captures and Beta-decays that produce the r-nuclides. We find that for an entropy per baryon (in units of kappa) of less than s = 200, an r-process does not occur. However, there may be a significant production of intermediate mass elements (especially near the neutron closed shell N = 50). In particular, for entropies near s = 100, there is signficant production of the nuclides ^90Zr, ^89Y, ^88Sr, ^87Rb, ^86Kr, ^82Kr, ^72Ge, and ^70Ge. For entropies near s = 20, the neutron-rich isotopes ^70Zn, ^64Ni, ^60Fe, ^54Cr, and ^50Ti are produced. Of course, these results depend on the Y(sub)e of the emerging wind. We investigate the production of these nuclides within the context of [2] supernova model and discuss the implications of this type of nucleosynthesis for some of the isotopic anomalies found in meteorites. This work was performed under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48. References: [1] Howard W. M. et al. (1993) Ap. J., in press. [2] Mayle R. W. and Wilson J. R. (1993) in preparation. [3] Meyer B. S. et al. (1992) Ap. J., 399, 656. [4] Woosley S. E. and Hoffman R. D. (1992) Ap. J., 395, 202.

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