1. Ivo Rolf Seitenzahl Graduate Student in Physics Advisor: Jim Truran

2. Nuclear Statistical Equilibrium (NSE) for type 1a supernova simulations

3. Road map NSE equations Plots, plots and more plots (results) Applications to type 1a supernovae

4. Equilibrium equations

5. 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.

7. Derived quantities

8. Basic Picture

11. Effects of excited states and coulomb interaction

17. Effect of neutronization

24. Supernova connection

26. 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

30. 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