Ivo Rolf Seitenzahl Graduate Student in Physics Advisor: Jim Truran.
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Transcript of Ivo Rolf Seitenzahl Graduate Student in Physics Advisor: Jim Truran.
![Page 1: Ivo Rolf Seitenzahl Graduate Student in Physics Advisor: Jim Truran.](https://reader036.fdocuments.us/reader036/viewer/2022062519/5697bf931a28abf838c8f584/html5/thumbnails/1.jpg)
•Ivo Rolf Seitenzahl
•Graduate Student in Physics
•Advisor: Jim Truran
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Nuclear Statistical Equilibrium (NSE)
for type
1a supernova si
mulations
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Road map
•NSE equations
•Plots, plots and more plots (results)
•Applications to type 1a supernovae
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Equilibrium equations
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Method of solving
Substitute
into the conservation equations:
1)
2)
Solve with Newton-Raphson method numerically for the chemical potentials of neutrons and protons. Substitute
back to get NSE massfractions of the nuclei as a function of temperature, density and electron fraction.
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Derived quantities
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Basic Picture
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Effects of excited states and coulomb
interaction
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Effect of neutronization
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Supernova connection
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• Timescale to reach NSE is less than dynamic timescale for a large portion of the early explosion (allows us to treat ashes as NSE)
• Heat capacity of the ion gas depends on , which in NSE is a function of
• Weak interactions are energy sink
• Light curve sensitive to amount of produced, which depends in NSE sensitively on
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Conclusions
•Exited states and Coulomb corrections to ideal gas must be included to compute massfractions
•Inclusion of weak interactions probably important for type 1 a supernova dynamics
•Include neutronization rates and energy loss in simulations at the ASCI Flash Center in Chicago