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
into the conservation equations:
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