nu_rnet
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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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| It came out that at high Temperatures around 10 GK mainly free neutrons and free protons exist. The other abundances were found to be very low. Thus, for our final calculations we did not use the nse, but changed the proton fraction directly by varying the proton to neutron rate in the initial abundances and neglecting the all other abundances. | It came out that at high Temperatures around 10 GK mainly free neutrons and free protons exist. The other abundances were found to be very low. Thus, for our final calculations we did not use the nse, but changed the proton fraction directly by varying the proton to neutron rate in the initial abundances and neglecting the all other abundances. | ||
| + | ===Reaction Network=== | ||
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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: | ||
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| + | {{ :nuclide_chart.jpg?700 |}} | ||
| + | The black squares mark the stable isotopes. | ||
nu_rnet.txt ยท Last modified: 2014/06/06 09:18 by schutrumpg
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