Nuclear Astrophysics


This is an area for providing nuclear data for astrophysics calculations, such as nucleosynthesis, stellar evolution, the Big Bang, and super-nova dynamics. As a start, we are including conventional astrophysics representations (the astrophysical S-factor and the reaction rate sigma-v-bar versus temperature) for several charged-particle induced reactions from recent LANL evaluations by Gerry Hale and Philip Page, links to recent papers on astrophysical topics from our Group, and links to nuclear masses and other properties for almost 9000 nuclides from Moller and Nix.

This area is a component of our participation in the Astrophysics Task Force under the US Nuclear Reaction Data Network (USNRDN). The USNRDN is a project of DOE/NP. For more information, see the Astrophysics Task Force section on the USNRDN Home Page. Additional nuclear data for astrophysics is available online from LBNL.

NEW for Jan'00! Plots in PDF format for Adobe acroread.


Articles on Nuclear Astrophysics

For some background information on nuclear astrophysics and the effects of nuclear data on some of the most interesting problems of astronomy, see the general article on Nuclear Astrophysics or the advanced article on Helium Burning in Stars from our Schoolbus Tour.

Reaction Q-Values and Thresholds

Computes reaction Q-values and thresholds using experimental and theoretical nuclear masses. ryxm@lanl.gov

Astrophysical Data for Charged-Particle Reactions

These reactions of astrophysical interest were taken from evaluations made with the EDA R-matrix code by Gerry Hale and Philip Page. The plots in this section are available in Postscript, PDF, and GIF formats. The Postscript form is usually preferrable for those with a Postscript viewer, such as ghostview, because it gives both high-quality viewing and printing. The PDF files also have this advantage when used with Adobe acroread. For those without ghostview or acroread, the GIF files can be used for viewing, and the Postscript files can be downloaded for printing.
  • D(d,n)3He
    • Postscript | PDF | GIF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF | GIF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • D(d,p)T
    • Postscript | PDF | GIF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF | GIF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • T(d,n)4He
    • Postscript | PDF | GIF plot of the astrophysical S factor.
    • Table of the astrophysical S factor with error estimates.
    • Postscript | PDF | GIF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • T(t,2n)4He
    • Postscript | PDF | GIF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF | GIF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 3He(d,p)4He
    • Postscript | PDF | GIF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF | GIF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 6Li(p,3He)4He
    • Postscript | PDF | GIF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF | GIF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 6Li(d,a)4He
    • Postscript | PDF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 6Li(d,p)7Li
    • Postscript | PDF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 6Li(d,n)7Be
    • Postscript | PDF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 7Li(p,a)4He
    • Postscript | PDF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 10B(p,a)7Be
    • Postscript | PDF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 11B(p,a)8Be
    • Postscript | PDF | GIF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF | GIF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • 13C(p,g)14N
    • Postscript | PDF plot of the astrophysical S factor.
    • Table of the astrophysical S factor.
    • Postscript | PDF plot of the reaction rate sigma-v-bar versus temperature.
    • Table of the reaction rate sigma-v-bar versus temperature.
  • Postscript | PDF | GIF plot comparing four astrophysical deuteron reactions.
  • Comparisons of Hale results for sigma-v-bar with those of Hoffman and Woosley.
See our Charged Particle Data area for more information on the LANL evaluations.

Interactive Access to Nuclear Properties for Astrophysics

Get masses, deformations, decay Q-values, half-lives, spins, and separation energies for 9000 nuclides here!

The alpha+Carbon Astrophysical Reaction

This is a long version of the paper G. M. Hale, "Extrapolation of alpha+Carbon Reaction Cross Section to Astrophysical Energies," presented at the Fourth International Symposium on Nuclear Astrophysics, "Nuclei in the Cosmos 1996," at the University of Notre Dame, 20-27 June 1996. Postscript file (1.0 MB).

Nuclear Masses for Astrophysical Applications

Astrophysical parameters from the paper ``Nuclear Ground-State Masses and Deformations,'' by P. Möller, J. R. Nix, W. D. Myers, and W. J. Swiatecki, Atomic Data Nucl. Data Tables 59, 185-381 (1995). It consists of a text section, eight black-and-white figures, 12 color figures, and a table of ground-state masses and deformation for 8979 nuclei ranging from oxygen-16 to A=339. Those with access to the decompression program gunzip should select these compressed files. Others should select these normal files. Reference: LA-UR-93-3083.

Other Nuclear Properties for Astrophysical Applications

Properties taken from the preprint ``Nuclear Properties for Astrophysical Applications,'' by P. Möller, J. R. Nix, and K.-L. Kratz, which has been submitted for publication to Atomic Data Nucl. Data Tables. It consists of a text section, 16 color figures, 83 black-and-white figures, and a table of ground-state properties for 8979 nuclei ranging from oxygen-16 to A = 339. The tabulated quantities include the ground-state odd-proton and odd-neutron spins and parities, proton and neutron pairing gaps, binding energy, one- and two-neutron separation energies, quantities related to beta-delayed one- and two-neutron emission probabilities, beta-decay energy release and half-life with respect to Gamow-Teller decay, one- and two-proton separation energies, and alpha-decay energy release and half-life. Those with access to the decompression program gunzip should select these compressed files. For the benefit of those without access to gunzip, we have also provided these normal files. Reference: LA-UR-94-3898.


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Photo credit: Dr. Christoper Burrows, ESA/STScI and NASA, Hubble Space Telescope, 1994. He is not guilty for the color and contrast transformations! ryxm@lanl.gov.

March 2006
ryxm@lanl.gov