This shows you the differences between two versions of the page.
Both sides previous revision Previous revision Next revision | Previous revision Next revision Both sides next revision | ||
culinary_services [2014/06/05 14:59] warren |
culinary_services [2014/06/05 15:16] warren |
||
---|---|---|---|
Line 24: | Line 24: | ||
===Simulations=== | ===Simulations=== | ||
- | 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> = 0.45,0.5,0.55]. 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). |
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: | ||
Line 32: | Line 32: | ||
\end{equation} | \end{equation} | ||
- | Where $\tau$ is some static free-fall timescale. | + | where $\tau$ is the hydrodynamic timescale. |
- | This **obviously** leads to: | + | This leads to temperature and density trajectories: |
\begin{equation} | \begin{equation} | ||
Line 40: | Line 40: | ||
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. | ||
- | Then you run the code, and it doesn't work. (nevermind, it does work.) | + | 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. |
===Results=== | ===Results=== | ||
**REFERENCES** \\ | **REFERENCES** \\ | ||
- | [[http://iopscience.iop.org/0067-0049/191/1/66|Trends in 44Ti and 56Ni from Core-Collapse Supernovae (Magkotsios et al (2010))]]\\ | + | [[http://adsabs.harvard.edu/abs/2010ApJS..191...66M|Trends in 44Ti and 56Ni from Core-Collapse Supernovae (Magkotsios et al 2010)]]\\ |
- | [[http://iopscience.iop.org/0004-637X/504/1/500|Nuclear Reactions Governing the Nucleosynthesis of 44Ti (The et al (1998))]]\\ | + | [[http://adsabs.harvard.edu/abs/1998ApJ...504..500T|Nuclear Reactions Governing the Nucleosynthesis of 44Ti (The et al 1998)]]\\ |
- | [[http://www.sciencedirect.com/science/article/pii/S1387647303002707|X-ray and gamma-ray observations of Cas A]] | + | [[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/2014Natur.506..339G|Asymmetries in core-collapse supernovae from maps of radioactive 44Ti in Cassiopeia A (Grefenstette et al 2014)]] |