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.
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