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group10 [2014/05/30 16:38] siegl created |
group10 [2014/06/12 13:22] (current) siegl |
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**Topic** | **Topic** | ||
- | The effect of initial conditions and reactions on abundances from the s-process in AGB stars. | ||
+ | Simulation of the s-process under AGB conditions in a nuclear reaction network | ||
+ | |||
+ | **Members** | ||
+ | |||
+ | Julia Bliss - Analysis | ||
+ | |||
+ | Jianping Lai - Parameters | ||
+ | |||
+ | Kevin Siegl - Code | ||
+ | |||
+ | ====Log==== | ||
+ | |||
+ | **Initial Goals:** | ||
+ | |||
+ | Determine theoretical astrophysical conditions for AGB stars during the s-process. | ||
+ | |||
+ | Create reaction network for both <sup>56</sup>Fe 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. | ||
+ | |||
+ | **Accomplishments:** | ||
+ | |||
+ | 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 <sup>4</sup>He and <sup>13</sup>C in order to produce neutrons and a 1% abundance of <sup>56</sup>Fe. | ||
+ | |||
+ | 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|}} | ||