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Ivo Rolf Seitenzahl Graduate Student in Physics Advisor: Jim Truran. N uclear S tatistical E quilibrium (NSE) for type 1a supernova simulations. Road map. NSE equations Plots, plots and more plots (results) Applications to type 1a supernovae. Equilibrium equations. Method of solving.

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Ivo Rolf Seitenzahl

Graduate Student in Physics

Advisor: Jim Truran


N uclear s tatistical e quilibrium nse for type 1a supernova simulations
Nuclear Statistical Equilibrium (NSE)for type 1a supernova simulations


Road map
Road map

  • NSE equations

  • Plots, plots and more plots (results)

  • Applications to type 1a supernovae



Method of solving
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.







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


Conclusions
Conclusions large portion of the early explosion (allows us to treat ashes as NSE)

  • 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


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