The Nuclear Level Density and the Determination of Thermonuclear Rates for Astrophysics

Details The Nuclear Level Density and the Determination of Thermonuclear Rates for Astrophysics The Nuclear Level Density and the Determination of Thermonuclear Rates for Astrophysics

1996-02-17

arxiv.org/abs/astro-ph/9602087v1

Mem.Soc.Ast.It. 67 (1996) 851

Astronomy and Astrophysics

Astrophysics

12 pages, 4 Postcript figures, uses memsait.sty; preprint also available at http://quasar.physik.unibas.ch/ . to appear in Mem

Scientific paper

The prediction of cross sections for nuclei far off stability is crucial in the field of nuclear astrophysics. In recent calculations the nuclear level density -- as an important ingredient to the statistical model (Hauser-Feshbach) -- has shown the highest uncertainties. We present a global parametrization of nuclear level densities based on the back-shifted Fermi-Gas formalism. Employment of an energy-dependent level density parameter $a$ and microscopic corrections from a recent FRDM mass formula by M\"oller et al.\ leads to a highly improved fit of level densities at the neutron-separation energy in the mass range $20\le A \le 245$. The importance of using proper microscopic corrections from mass formulae is emphasized. The resulting level description is well suited for astrophysical applications. The level density can also provide clues to the applicability of the statistical model which is only correct for a high density of excited states. Using the above description one can derive a ``map'' for the applicability of the model for reactions of stable and unstable nuclei with neutral and charged particles.

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