This shows you the differences between two versions of the page.
Both sides previous revision Previous revision Next revision | Previous revision | ||
group10 [2014/06/03 17:54] bliss |
group10 [2014/06/12 13:22] (current) siegl |
||
---|---|---|---|
Line 25: | Line 25: | ||
Modify xnet code to allow the definition of a time-dependent neutron flux. | Modify xnet code to allow the definition of a time-dependent neutron flux. | ||
- | **References** | + | **Accomplishments:** |
- | **s-process abundances in the solar system** | + | 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. |
- | remark: | + | We incorporated those conditions into xnet reaction network with an initial abundance of <sup>4</sup>He and <sup>13</sup>C in order to produce neutrons and a 1% abundance of <sup>56</sup>Fe. |
- | Z[first column], A[second column], Y[third column] | + | |
+ | 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%. | ||
+ | |||
+ | **References** | ||
+ | |||
+ | {{:sprocesskaeppler.pdf|}} | ||
+ | |||
+ | {{:sprocesslugaro.pdf|}} | ||
+ | |||
+ | final abundance format : | ||
+ | Z[first column], A[second column], Y[third column] | ||
+ | Presentation: | ||
+ | {{::today.odp|}} | ||