nuclear statistical equilibrium codes from cococubed

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Nuclear Statistical Equilibrium

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The public_nse.f program given below illustrates how to put any reaction network into its NSE state. If your going to get serious about NSE calculations, then you'll want to modify the public code to use more accurate nuclear data (e.g., ground state spins and temperature dependent partition functions), add more physics (coulomb corrections), and increase the number of isotopes. Still, the two figures below suggest the public code gives reasonable results for the assumptions made.

Most abundant isotopes
as a function of temperature

Most abundant isotopes
as a function of Y_e

Tests the NSE solver: public_nse.f
To reproduce the classic Clifford & Taylor plot
on the left use fig1_nse.f

You'll also need these include files:
implno.dek
const.dek
network.dek

The movies below accompany the "Proton-Rich Nuclear Statistical Equilibrium" paper published in the Astrophysical Journal and released on astro-ph. My co-authors on this project are Ivo Seitenzahl A. Marin-Lafleche, Ed Brown Georgios Magkotsios, and Jim Truran. Each movie shows the NSE isotope abundance on the vertical axis and either the temperature or electron fraction Y_e on the horizontal axis. Limits for the vertical axis are either 1e-2 or 1e-4, which show less and more isotopes respectively. We cover the density range from 1e3 to 1e9 g/cc.

Density = 1.0e3 g/cc Density = 1.0e4 g/cc