culinary_services
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culinary_services [2014/06/06 14:35] long |
culinary_services [2014/06/06 15:52] long |
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| + | ==========Culinary Services========== | ||
| + | |||
| We are Culinary Services. \\ | We are Culinary Services. \\ | ||
| - | \\ | ||
| - | Who ordered the extra side of <sup>44</sup>Ti? | ||
| - | |||
| **GROUP MEMBERS**\\ | **GROUP MEMBERS**\\ | ||
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| ==== TOPIC ==== | ==== TOPIC ==== | ||
| - | Sensitivity studied of <sup>44</sup>Ti production in in core-collapse supernova environments. | + | Sensitivity studiy of <sup>44</sup>Ti and <sup>56</sup>Ni production in in core-collapse supernova environments. |
| ===Scientific Background=== | ===Scientific Background=== | ||
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| There are many uncertainties in our understanding of core-collapse supernovae, including the explosion mechanism and nucleosynthesis. One way to gain insight into these phenomena is to study the nucleosynthesis of radioactive isotopes in the shock-heated material. These isotopes, such as <sup>44</sup>Ti and <sup>56</sup>Ni, determine the features of the supernova light curve. Observations of supernova remnants can be used to put bounds on the production of these isotopes. | There are many uncertainties in our understanding of core-collapse supernovae, including the explosion mechanism and nucleosynthesis. One way to gain insight into these phenomena is to study the nucleosynthesis of radioactive isotopes in the shock-heated material. These isotopes, such as <sup>44</sup>Ti and <sup>56</sup>Ni, determine the features of the supernova light curve. Observations of supernova remnants can be used to put bounds on the production of these isotopes. | ||
| - | {{ ::cassa.png?nolink&200 |Observation of Cassiopeia A. Green shows 44Ti distribution, blue is 28Si, and the red shows the Fe distribution. (From Grefenstette et al 2014)}} | + | {{ ::cassa.png?nolink&600 |Observation of Cassiopeia A. Green shows 44Ti distribution, blue is 28Si, and the red shows the Fe distribution. (From Grefenstette et al 2014)}} |
| Figure: Observation of Cassiopeia A. Green shows <sup>44</sup>Ti distribution, blue is <sup>28</sup>Si, and the red shows the Fe distribution. (From Grefenstette et al 2014) | Figure: Observation of Cassiopeia A. Green shows <sup>44</sup>Ti distribution, blue is <sup>28</sup>Si, and the red shows the Fe distribution. (From Grefenstette et al 2014) | ||
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| ==Reaction Network == | ==Reaction Network == | ||
| We used the [[https://wikihost.nscl.msu.edu/talent/lib/exe/fetch.php?media=xnet_public.zip|XNet]] reaction network code. Our code included 447 isotopes ranging from hydrogen through germanium. We took the reaction rates from the [[https://groups.nscl.msu.edu/jina/reaclib/db/library.php?action=viewsnapshots|JINA Reaclib database]]. We set the threshold temperature for NSE to be 5 GK. | We used the [[https://wikihost.nscl.msu.edu/talent/lib/exe/fetch.php?media=xnet_public.zip|XNet]] reaction network code. Our code included 447 isotopes ranging from hydrogen through germanium. We took the reaction rates from the [[https://groups.nscl.msu.edu/jina/reaclib/db/library.php?action=viewsnapshots|JINA Reaclib database]]. We set the threshold temperature for NSE to be 5 GK. | ||
| + | |||
| + | ==Initial Abundances and Y$_{e}$== | ||
| + | For any given peak temperature and density, our initial composition was pure $^{28}$Si (therefore Y$_{e}$ = .5) In order to change the initial Y$_{e}$, we just added protons or neutrons to the initial composition according to the following equations: | ||
| + | |||
| + | \begin{equation} | ||
| + | X(^{28}Si) = 1 - \left | 2Y_{e} - 1 \right | \\ | ||
| + | X(p) = \left | 2Y_{e} - 1 \right | \hspace{1cm} X(n) = \left | 2Y_{e} - 1 \right | \\ | ||
| + | proton-rich \hspace{1cm} neutron-rich | ||
| + | \end{equation} | ||
| Finally we looked at the mass fraction of several isotopes. In particular, $^{4}$He, $^{28}$Si, $^{44}$Ti, and $^{56}$Ni. We then compare our results to that of Magkotsios //et al// with in our parameter space. | Finally we looked at the mass fraction of several isotopes. In particular, $^{4}$He, $^{28}$Si, $^{44}$Ti, and $^{56}$Ni. We then compare our results to that of Magkotsios //et al// with in our parameter space. | ||
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| ==$^{44}$Ti Production== | ==$^{44}$Ti Production== | ||
| - | {{ :44ti.png?nolink&900 }} | + | {{ :44ti.png?nolink&900| 44Ti production for a given peak temperature and peak density.}} |
| + | $\hspace{2cm}$ $^{44}$Ti production for a given peak temperature and peak density for three different Y$_{e}$'s | ||
| ==$^{56}$Ni Production== | ==$^{56}$Ni Production== | ||
| - | {{:56ni.png?nolink&900|}} | + | {{:56ni.png?nolink&900| 56Ni production for a given peak temperature and peak density}} |
| + | $\hspace{2cm}$ $^{56}$Ni production for a given peak temperature and peak density for three different Y$_{e}$'s | ||
| **REFERENCES** \\ | **REFERENCES** \\ | ||
culinary_services.txt · Last modified: 2014/06/06 15:52 by long
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