2018 Impact factor 2.481
Hadrons and Nuclei
Eur. Phys. J. A 6, 157-165

Nuclear shell gaps at finite temperatures

C. Reiß1 - M. Bender2,3 - P.-G. Reinhard1,4

1 Institut für Theoretische Physik II, Universität Erlangen-Nürnberg, Staudtstrasse 7, 91058 Erlangen, Germany
2 Department of Physics and Astronomy, The University of North Carolina, Chapel Hill, NC 27516-3255, USA
3 Department of Physics and Astronomy, The University of Tennessee, Knoxville, TN 37996, USA
4 Joint Institute for Heavy-Ion Research, Oak Ridge National Laboratory, P. O. Box 2008, Oak Ridge, TN 37831, USA

Received: 29 September 1998 / Revised version: 1 July 1999 Communicated by F. Lenz

Abstract
Neutron-rich nuclei with a closed neutron shell represent chains of waiting-point nuclei in the astrophysical r-process. Details of their nuclear structure like separation energies, shell structure and $\beta^-$-decay half-lives have a dramatic influence on element abundances calculated from r-process simulations. Actual supernova scenarios take place at finite temperature. To investigate the influence of finite temperature on binding energies and shell gaps, i.e. the second derivative of the binding energy, we calculate the shell gaps in the range of interest and slightly beyond, i.e. $0 \leq k_{\rm B}T \leq 0.8$ MeV. Basis of the description is the self-consistent Skyrme-Hartree-Fock model and an extension of BCS pairing to finite temperature using a natural orbital representation.

PACS
21.60.Jz Hartree-Fock and random-phase approximations - 21.60.-n Nuclear-structure models and methods


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