This shows you the differences between two versions of the page.
Both sides previous revision Previous revision Next revision | Previous revision Next revision Both sides next revision | ||
nu_rnet [2014/06/02 16:36] ahn |
nu_rnet [2014/06/05 13:54] schutrumpg |
||
---|---|---|---|
Line 1: | Line 1: | ||
- | [Group 7] | + | **[Group 7]** |
- | * Group name: $\nu$Rnet | + | *** Group name:** $\nu$Rnet |
- | * Members: | + | *** Members:** |
Tony Ahn: Analysis person | Tony Ahn: Analysis person | ||
Line 11: | Line 11: | ||
Bastian Schuetrumpf: Code person | Bastian Schuetrumpf: Code person | ||
- | * Motivation | + | *** Motivation** |
- | It is possible that neutrino driven wind will affect the neutron density resulting in the abundance pattern of the r-process. | + | |
- | {{:core-collapse_figure.png?200|}} | + | 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|}} | ||
+ | |||
+ | Fig. Schematic representation of the evolutionary stages from stellar core collapse. (Ref. H.Th. Janka, arXiv:astro-ph/0612072) | ||
+ | |||
+ | *** Method:** | ||
- | * Method: | ||
- To simulate r-process using x-net | - To simulate r-process using x-net | ||
Line 21: | Line 26: | ||
- To find change of the r-process path and change of the abundance pattern | - To find change of the r-process path and change of the abundance pattern | ||
+ | |||
+ | *** Input Parameters:** | ||
+ | |||
+ | 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: | ||
+ | |||
+ | {{ :out.jpg?500 |}} | ||