nu_rnet
Differences
This shows you the differences between two versions of the page.
| Both sides previous revision Previous revision Next revision | Previous revision | ||
|
nu_rnet [2014/06/05 18:29] schutrumpg |
nu_rnet [2014/06/06 09:18] (current) schutrumpg |
||
|---|---|---|---|
| Line 62: | Line 62: | ||
| ===Matrix Solver=== | ===Matrix Solver=== | ||
| - | The standart matrix solver included in the xnet programm "LAPACK" is too slow to solve a network like this. Faster solutions are sparse matrix solver. Two interfaces are included in xnet: For MA48 and Pardiso. Instructions to include these matrix solvers in the code can be found in the documentation of the code. We experienced problems for both with Linux: Pardiso should be much faster than MA48 needs a full compiled LAPACK library. This is included in the ifort compiler. Finally we succeeded in compiling Pardiso version with ifort. The program can be found here. | + | The standart matrix solver included in the xnet programm "LAPACK" is too slow to solve a network like this. Faster solutions are sparse matrix solver. Two interfaces are included in xnet: For MA48 and Pardiso. Instructions to include these matrix solvers in the code can be found in the documentation of the code. We experienced problems for both with Linux: Pardiso should be much faster than MA48 needs a full compiled LAPACK library. This is included in the ifort compiler. Finally we succeeded in compiling Pardiso version with ifort. The program can be found in the document server. |
| ====Results==== | ====Results==== | ||
| - | ==$Y_e=0.2$== | + | ==$Y_e=0.15$== |
| {{ :ev15.png?400 |}} | {{ :ev15.png?400 |}} | ||
| ==$Y_e=0.25$== | ==$Y_e=0.25$== | ||
| - | {{ :ev250.png?400 |}} | + | {{ :ev25.png?400 |}} |
| ==$Y_e=0.4$== | ==$Y_e=0.4$== | ||
| - | {{ :ev35.png?400 |}} | + | {{ :ev40.png?400 |}} |
| - | The preliminary results show the abundances of selected nuclides. The abundances are representative for the regions of magic neutron numbers | + | The preliminary results show the abundances of selected nuclides. The abundances are representative for the regions of magic neutron numbers 82 and 126. The abundances in these regions should be high. For $Y_e=0.15$ only small abundances for these nuclides are present, because the seed density consisting of almost the same number of protons and neutrons is too small. For $Y_e=0.25$ we see strong abundances of these nuclides, but for higher $Y_e>0.4$ the neutron density is too small. Thus neutron capure is too slow and the heavy elements cannot be built. |
nu_rnet.1402007340.txt.gz ยท Last modified: 2014/06/05 18:29 by schutrumpg
Page Tools
Except where otherwise noted, content on this wiki is licensed under the following license: CC Attribution-Share Alike 4.0 International
