GRADUATE NUCLEAR ASTROPHYSICS CLASS: SPRING 2009

NUCLEAR ASTROPHYSICS RESOURCES
  • National Nuclear Data Center (NNDC)
  • Joint Institute for Nuclear Astrophysics (JINA)
  • Frank Timmes website here
  • A machine readable version of the solar system abundances (K. Lodders, 2003, ApJ, 591, 1220) may be found here. The next to last column is nucleon fraction while the last is the mass fraction (see Arnett, 1996, Ch. 2 for more detail).

    • DRAFT SYLLABUS for revised ASTR 535 and 587 is here

    Burnf: gzipped tarfile of stand-alone reaction network code is here

    Problem set 1 is here

    Problem set 2 is here

    Problem set 3 is here and file nuc.in.24b is here

    SOLAR MODEL AND SOLAR NEUTRINOS

    The input.f file has one single modification: the factor xlfak = 1.0 --> 0.6 to get the correct solar luminosity by scaling the average opacity (see Ch. 6 in Supernovae and Nucleosynthesis). The nuc.in file has been modified to approximate a consistent stellar evolutionary sequence for the Sun. A complete trimmed tarfile for the burn package is here. After this tarfile is unpacked, do the following:

  • cd burnpkg1/src
  • make Burnf
  • cd ..
  • Burnf
    • to get a test sequence *.sol1 for validation. Compare this to the correct sequence *.sol0 in the local directory. There should be no significant differences (except roundoff).

    This has been checked directly (4-2-09) on a macbook (Intel Core 2 Duo, OS X 10.5.6), and a Steward linux box (chandra.as.arizona.edu, Centos), as downloaded from this webpage. Uses the gfortran compiler.

    Burnf for s-process here This is similar to the previous version, but does s-process nucleosynthesis. A new parameter, dndt, which specifies the rate of addition of neutrons (per second per mole), is set in the nuc.in file.

    Final problem set:

    (1) Try the new Burnf for values up to 5.0e-14, and look at the change in abundance of nuclei. The sequence label is "spea" for my results. Change this to "speb" in the file nuc.in before you run your version. The new network has been extended only up to A=111, but shows the correct s-process behavior up to this value for the source rate. Characterize the behavior as a funtion of dndt.

    (2) Compare the neutron densities to those discussed in Lattanzio and Lugaro (2005).

    (3) Comment on any odd-even effect you see.

    (4) Identify any effects of the limited network.

    (5) Search the literature for the "weak s-process", and summarize what it is.

    Good luck!

    Last modified 4-2-09