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nu_rnet [2014/05/30 17:31] schutrumpg |
nu_rnet [2014/06/05 13:54] schutrumpg |
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- | **Members:** | + | **[Group 7]** |
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+ | *** Group name:** $\nu$Rnet | ||
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+ | *** Members:** | ||
Tony Ahn: Analysis person | Tony Ahn: Analysis person | ||
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Bastian Schuetrumpf: Code person | Bastian Schuetrumpf: Code person | ||
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+ | *** Motivation** | ||
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+ | It is possible that electron fraction Ye will affect the neutron density resulting in the abundance pattern of the r-process. | ||
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+ | {{:core-collapse_figure.png?500|}} | ||
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+ | Fig. Schematic representation of the evolutionary stages from stellar core collapse. (Ref. H.Th. Janka, arXiv:astro-ph/0612072) | ||
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+ | *** Method:** | ||
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+ | - To simulate r-process using x-net | ||
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+ | - To change Ye considering effects of the neutrino driven wind | ||
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+ | - To find change of the r-process path and change of the abundance pattern | ||
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+ | *** Input Parameters:** | ||
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+ | At first we had to set a reasonable temperature and density trajectory for a neutrino driven wind in which the r-process takes place. We take a realistic trajectory from Raphael Hix the temperature and density profile looks like this: | ||
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+ | {{ :out.jpg?200 |}} | ||
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