Recommended quantities

Cross sections
  1. (n,g) (n,p), (n,a),
  2. (p,g) (p,n), (p,a),
  3. (a,g) (a,n), (a,p),

Reaction rates
  1. (n,g) (n,p), (n,a),
  2. (p,g) (p,n), (p,a),
  3. (a,g) (a,n), (a,p),

Normalized partition function G(T)

30 keV Laboratory Maxwellian Averaged (n,g) Cross Sections MACS


Description of TALYS models

Below are various links to 8892 isotopes for astrophysics applications (cross sections, reaction rates and MACS) based on TALYS calculations (version 1.96).

Different reaction "model sets" were used: "a model set" represents a combination of 9 TALYS models:

  1. Gamma strength function (values 8 or 9): either Gogny D1M HFB+QRPA, or SMLO
  2. Level density (values 1, 2 or 5): Constant temperature + Fermi gas model, or Back-shifted Fermi gas model, or Microscopic level densities (Skyrme force) from Hilaire's combinatorial tables
  3. JLM microscopic optical model potential or KD optical model (values y or n)
  4. Gamma strength function for M1 (values 3 or 8): Hartree-Fock BCS tables or Gogny D1M HFB+QRPA
  5. Collective enhancement (values y or n): yes or no
  6. Width fluctuation (values 0, 1 or 2): Moldauer model, or Hofmann-Richert-Tepel-Weidenmueller model
  7. Mass model (values 0, 1, 2 or 3): Duflo-Zuker formula, Moeller table, Goriely HFB-Skyrme table, or HFB-Gogny D1M table (except for known masses, where the experimental value is used)
  8. Alpha optical model (values 5 or 6): Demetriou/Goriely, or Avrigeanu
  9. Fission model (values 1 or 5): "experimental" fission barriers, or WKB approximation for fission path model.

Each of the set models is named with 9 values, such as "91n3n1261" (default TALYS model), or 85n8n1261. These values correspond to the ones in the TALYS manual.

Examples of input/output files


Cross sections from 0.01 eV to 20 MeV; Typical examples:

  1. (n,g), (n,p), (n,a) -- input, energy grid, output xs000000.tot, xs010000.tot and xs000001.tot.
  2. (p,g), (p,n), (p,a) -- input, energy grid, output xs000000.tot, xs100000.tot and xs000001.tot.
  3. (a,g), (a,n), (a,p) -- input, energy grid, output xs000000.tot, xs100000.tot and xs010000.tot.

Reaction rates for all temperatures taking into account the thermal population of the target; Typical examples:

  1. (n,g), (n,p), (n,a) -- input, energy grid, output astrorate.g, astrorate.p and astrorate.a.
  2. (p,g), (p,n), (p,a) -- input, energy grid, output astrorate.tot.
  3. (a,g), (a,n), (a,p) -- input, energy grid, output astrorate.tot.

Normalized partition function G(T); Typical examples:

  1. neutrons -- input, energy grid, output astrorate.tot.

30 keV MACS Laboratory (not stellar) Maxwellian Averaged (n,g) Cross Sections; Typical examples:

  1. neutrons -- input, output macs.g.



Quantities with uncertainties
    10 models 480 models 960 models
    (A< 210) (A≥210)
  1. cross sections:
  2. (n,g) (n,p) (n,a) (n,g) (n,p) (n,a) (n,g) (n,p) (n,a)
  3. cross sections:
  4. (p,g) (p,n) (p,a) (p,g) (p,n) (p,a) (p,g) (p,n) (p,a)
  5. cross sections:
  6. (a,g) (a,n) (a,p) (a,g) (a,n) (a,p) (a,g) (a,n) (a,p)
  7. reaction rates:
  8. (n,g) (n,p) (n,a) (n,g) (n,p) (n,a) (n,g) (n,p) (n,a)
  9. reaction rates:
  10. (p,g) (p,n) (p,a) (p,g) (p,n) (p,a) (p,g) (p,n) (p,a)
  11. reaction rates:
  12. (a,g) (a,n) (a,p) (a,g) (a,n) (a,p) (a,g) (a,n) (a,p)
  13. Normalization function:
  14. G(T) G(T) G(T)
  15. Maxwellian Averaged (n,g) :
  16. MACS MACS MACS