This is an old revision of the document!
[Group 7]
* Group name: $\nu$Rnet
* Members:
Tony Ahn: Analysis person
Tsung-han Yeh: Parameter person
Bastian Schuetrumpf: Code person
* Motivation
It is possible that electron fraction Ye will affect the neutron density resulting in the abundance pattern of the r-process.
Fig. Schematic representation of the evolutionary stages from stellar core collapse. (Ref. H.Th. Janka, arXiv:astro-ph/0612072)
* Method:
- To simulate r-process using x-net
- To change Ye considering effects of the neutrino driven wind
- 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:
To set the initial electron fraction $Y_e$ which is equivalent to the proto fraction due to charge neutrality, we ran the nse version of the xnet code. Therefore the lines in the code tagged by !NSE have to be uncommented and the lines tagged by !NOTNSE have to be commented. This can be done quickly with the following commands in Unix:
sed -e 's/^\!\(.*\!NSE\)/ \1/' conditions.f90 >conditions.f90- sed -e 's/^\!\(.*\!NSE\)/ \1/' net_mpi.f90 >net_mpi.f90- sed -e 's/^\!\(.*\!NSE\)/ \1/' net.f90 >net.f90- sed -e 's/^\!\(.*\!NSE\)/ \1/' data_distribute_mpi.f90 >data_distribute_mpi.f90- mv conditions.f90- conditions.f90 mv net_mpi.f90- net_mpi.f90 mv net.f90- net.f90 mv data_distribute_mpi.f90- data_distribute_mpi.f90 sed -e 's/^\!\(.*\!NOTNSE\)/!\1/' net.f90 >net.f90- mv net.f90- net.f90
Additionally the line
NSE_OBJ = nse.o
has to be uncommented.