Nucleosynthesis in Early Neutrino Driven Winds

AIP Conference Proceedings 02/2008; 1005(1). DOI: 10.1063/1.2920736
Source: arXiv


Nucleosynthesis in early neutrino winds is investigated. Presented is a brief overview of two recent problems of supernova nucleosynthesis. In the first part we investigate the effect of nuclear parameters on the synthesis of Mo92 and Mo94. Based on recent experimental results, we find that the proton rich winds of the model investigated here can not be the source of solar Mo92 and Mo94. In the second part we investigate the nucleosynthesis from neutron rich bubbles and show that they do not contribute to the overall nucleosynthesis.

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Available from: Robert Buras-Schnell, Jun 02, 2014
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    ABSTRACT: 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 ≤ Y e ≤ 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 Y e–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.
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    ABSTRACT: The effects of ion screening in stellar core collapses are investigated based on a new progenitor star model. Simulation results show that ion screening slightly affects the leptons and decreases explosion energy, which is a negative factor for energy transfer supernova explosions. We also investigate the effect on type II-supernova explosions of neutrino-nucleus elastic scattering based on the new progenitor star model. It is shown that, compared with the previously calculated results, neutrinos-nucleus elastic scattering in stellar core collapses is more severe, leading to an obvious reduction of the neutrino leakage energy loss and an increase of supernova explosion energy.
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    ABSTRACT: Based on the new progenitor stars model, the influence of ion screening is investigated. The simulation results show that ion screening has weak perturbation effects to the leptons in type-II supernova explosion. Ion screening decreases slightly the fraction of leptons and prolongs slightly the shock propagation time. Moreover, simulation results are shown that ion screening increases the total energy loss and reduces the shock energy, eventually decreasing of explosion energy and becomes a negative factor to supernova explosion. In addition, comparison of slight perturbated variation of ion screening to leptons, but simulation results show that ion screening affects obviously explosion energy of type-II supernova, hence, it can also confirm that the variation of leptons is very sensitive to energy in supernova explosion.
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