Simulation of the s-process under AGB conditions in a nuclear reaction network
Julia Bliss - Analysis
Jianping Lai - Parameters
Kevin Siegl - Code
Determine theoretical astrophysical conditions for AGB stars during the s-process.
Create reaction network for both 56Fe and solar abundance seeds.
Create toolkit to read binary file into format appropriate for abundance graphing.
Modify xnet code to allow the definition of a time-dependent neutron flux.
We found a set of astrophysical conditions for the s-process in AGB stars, a temperature of 0.28GK and baryon density of 2.6e+3 g/cm^3.
We incorporated those conditions into xnet reaction network with an initial abundance of 4He and 13C in order to produce neutrons and a 1% abundance of 56Fe.
We also developed a python script to extract the abundances at a time step from the xnet binary files.
We then generated final abundances for iron concentrations of .1%, 1%, and 10%.
final abundance format : Z[first column], A[second column], Y[third column]