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Co-Production of Light p-, s- and r-Process Isotopes in the High-Entropy Wind of Type II Supernovae

Published online by Cambridge University Press:  05 March 2013

K. Farouqi ,
K.-L. Kratz  and
B. Pfeiffer
K. Farouqi
Affiliation:
Department of Astrophysics and Astronomy, University of Chicago, Chicago, IL 60637, USA
K.-L. Kratz*
Affiliation:
Max-Planck-Institut für Chemie, Otto-Hahn-Institut, D-55128 Mainz, Germany
B. Pfeiffer
Affiliation:
Max-Planck-Institut für Chemie, Otto-Hahn-Institut, D-55128 Mainz, Germany
*
CCorresponding author. Email: k-l.kratz@mpic.de
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Abstract

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We have performed large-scale nucleosynthesis calculations within the high-entropy-wind (HEW) scenario of Type II supernovae. The primary aim was to constrain the conditions for the production of the classical ‘p-only’ isotopes of the light trans-Fe elements. We find, however, that for electron fractions in the range 0.458 ≤ Ye ≤ 0.478, sizeable abundances of p-, s- and r-process nuclei between 64Zn and 98Ru are coproduced in the HEW at low entropies (S ≤ 100) by a primary charged-particle process after an α-rich freezeout. With the above Ye–S correlation, most of the predicted isotopic abundance ratios within a given element, e.g. 64Zn(p)/70Zn(r) or 92Mo(p)/94Mo(p), as well as of neighboring elements, e.g. 70Ge(s + p)/74Se(p) or 74Se(p)/78Kr(p) agree with the observed Solar-System ratios. Taking the Mo isotopic chain as a particularly challenging example, we show that our HEW model can account for the production of all 7 stable isotopes, from ‘p-only’ 92Mo, via ‘s-only’ 96Mo up to ‘r-only’ 100Mo. Furthermore, our model is able to reproduce the isotopic composition of Mo in presolar SiC X-grains.

Keywords

nuclear reactions, nucleosynthesis, abundancesstars: winds, outflowssupernovae: general
Type
Theory, Evolution and Models
Information
Publications of the Astronomical Society of Australia , Volume 26 , Issue 3 , 2009 , pp. 194 - 202
Copyright
Copyright © Astronomical Society of Australia 2009

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