nu_rnet
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nu_rnet [2014/06/05 15:44] schutrumpg |
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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. | It is possible that electron fraction Ye will affect the neutron density resulting in the abundance pattern of the r-process. | ||
| - | {{:core-collapse_figure.png?500|}} | + | {{:core-collapse_figure.png?650|}} |
| Fig. Schematic representation of the evolutionary stages from stellar core collapse. (Ref. H.Th. Janka, arXiv:astro-ph/0612072) | Fig. Schematic representation of the evolutionary stages from stellar core collapse. (Ref. H.Th. Janka, arXiv:astro-ph/0612072) | ||
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| Last but not least we need a reaction library. This was taken from the JINA Reaclib database. For the r-process only nucleides have to be considered which are stable or even more neutron rich. The proton rich nucleides can be neglected. In the chart of nuclei the considered rates look like this: | Last but not least we need a reaction library. This was taken from the JINA Reaclib database. For the r-process only nucleides have to be considered which are stable or even more neutron rich. The proton rich nucleides can be neglected. In the chart of nuclei the considered rates look like this: | ||
| - | {{ :nuclide_chart.jpg?700 |}} | + | {{ :nuclide_chart.jpg?650 |}} |
| + | The black squares mark the stable isotopes. | ||
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| + | This network includes 4510 species and 53763 reaction rates. This setup requires a very fast matrix solver. | ||
nu_rnet.txt · Last modified: 2014/06/06 09:18 by schutrumpg
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