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Nuclear Statistical Equilibrium

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Contact: F.X.Timmes
my one page vitae,
full vitae,
research statement, and
teaching statement.

The instrument in the bzip2 tarball public_nse.tbz illustrates how to put any reaction network into its NSE state. If you are going to get serious about NSE calculations, then you'll want to modify this 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.


image
Most abundant isotopes
as a function of temperature
image
Most abundant isotopes
as a function of Ye


The movies below accompany "Proton-Rich Nuclear Statistical Equilibrium". Each movie shows the isotope abundance on the vertical axis and either the temperature or electron fraction Ye on the horizontal axis. Limits for the abundance vertical axes are 0.01 (i.e., major abundances only; lower limits of 10-4 are avaliable upon request). The movies cover the temperature range 3 ≤ T9 ≤, density range 103 to 109 g cm-3, and Ye range 0.4 to 0.6.

ρ = 103 g cm-3
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Abundance vs Ye
ρ = 103 g cm-3
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Abundance vs Temp
ρ = 104 g cm-3
*
Abundance vs Ye
ρ = 104 g cm-3
*
Abundance vs Temp
ρ = 105 g cm-3
*
Abundance vs Ye
ρ = 105 g cm-3
*
Abundance vs Temp
ρ = 106 g cm-3
*
Abundance vs Ye
ρ = 106 g cm-3
*
Abundance vs Temp
ρ = 107 g cm-3
*
Abundance vs Ye
ρ = 107 g cm-3
*
Abundance vs Temp
ρ = 108 g cm-3
*
Abundance vs Ye
ρ = 108 g cm-3
*
Abundance vs Temp
ρ = 109 g cm-3
*
Abundance vs Ye
ρ = 109 g cm-3
*
Abundance vs Temp

 



Please cite the relevant references if you publish a piece of work that use these codes, pieces of these codes, or modified versions of them. Offer co-authorship as appropriate.