culinary_services
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culinary_services [2014/06/05 15:14] warren |
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 studied 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 <sup>44</sup>Ti distribution, blue is <sup>28</sup>Si, 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) | ||
| Using simulations, we can use these observations to gain insight into the supernova environment. By matching observed abundances, we can gain insight into the environment in which this nucleosynthesis must have taken place and in turn, the details of the explosion mechanism. However, most core-collapse supernova simulations do not include sufficiently large reaction networks to simulate this nucleosynthesis. | Using simulations, we can use these observations to gain insight into the supernova environment. By matching observed abundances, we can gain insight into the environment in which this nucleosynthesis must have taken place and in turn, the details of the explosion mechanism. However, most core-collapse supernova simulations do not include sufficiently large reaction networks to simulate this nucleosynthesis. | ||
| Line 24: | Line 24: | ||
| ===Simulations=== | ===Simulations=== | ||
| + | ==Parameter Space== | ||
| We have chosen to do a parameter space study in peak temperature, density, and electron fraction, tarting with a set parameter space of peak temperatures [T<sub>9</sub> = 4 - 7] and densities [$\rho$ = 10<sup>5</sup> - 10<sup>7</sup> g/cm<sup>3</sup>] for three values of the electron fraction [Y<sub>e</sub> = 0.45, 0.50, 0.55]. This parameter space roughly corresponds with the shock heated region in simulations of Cassiopeia A-like supernovae (Young & Fryer 2007). | We have chosen to do a parameter space study in peak temperature, density, and electron fraction, tarting with a set parameter space of peak temperatures [T<sub>9</sub> = 4 - 7] and densities [$\rho$ = 10<sup>5</sup> - 10<sup>7</sup> g/cm<sup>3</sup>] for three values of the electron fraction [Y<sub>e</sub> = 0.45, 0.50, 0.55]. This parameter space roughly corresponds with the shock heated region in simulations of Cassiopeia A-like supernovae (Young & Fryer 2007). | ||
| + | ==Thermodynamic Trajectories== | ||
| We use analytic adiabatic freeze-out trajectories (Hoyle et al. 1964; Fowler & Hoyle 1964) which satisfy the differential equations: | We use analytic adiabatic freeze-out trajectories (Hoyle et al. 1964; Fowler & Hoyle 1964) which satisfy the differential equations: | ||
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| \end{equation} | \end{equation} | ||
| - | Where $\tau$ is the free-fall timescale. | + | where $\tau$ is the hydrodynamic timescale. |
| This leads to temperature and density trajectories: | This leads to temperature and density trajectories: | ||
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| where $T_0$ and $\rho_0$ are the peak temperature and density in the supernova. | where $T_0$ and $\rho_0$ are the peak temperature and density in the supernova. | ||
| + | ==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. | ||
| ===Results=== | ===Results=== | ||
| + | |||
| + | ==$^{44}$Ti Production== | ||
| + | {{ :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== | ||
| + | {{: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** \\ | ||
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| [[http://adsabs.harvard.edu/abs/2004NewAR..48...61V|X-ray and gamma-ray studies of Cas A (Vink 2004)]]\\ | [[http://adsabs.harvard.edu/abs/2004NewAR..48...61V|X-ray and gamma-ray studies of Cas A (Vink 2004)]]\\ | ||
| [[http://adsabs.harvard.edu/abs/2007ApJ...664.1033Y|Uncertainties in Supernova Yields I One-dimensional Explosions (Young & Fryer 2007)]]\\ | [[http://adsabs.harvard.edu/abs/2007ApJ...664.1033Y|Uncertainties in Supernova Yields I One-dimensional Explosions (Young & Fryer 2007)]]\\ | ||
| - | [[http://adsabs.harvard.edu/abs/2014Natur.506..339G|Asymmetries in core-collapse supernovae from maps of radioactive <sup>44</sup>Ti in Cassiopeia A (Grefenstette et al 2014)]] | + | [[http://adsabs.harvard.edu/abs/2014Natur.506..339G|Asymmetries in core-collapse supernovae from maps of radioactive 44Ti in Cassiopeia A (Grefenstette et al 2014)]] |
culinary_services.txt · Last modified: 2014/06/06 15:52 by long
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