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Ivo Rolf Seitenzahl Graduate Student in Physics Advisor: Jim Truran

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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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Presentation Transcript
slide1
Ivo Rolf Seitenzahl

Graduate Student in Physics

Advisor: Jim Truran

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.

slide26
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
  • 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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