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 β−–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 ≤k B T≤ 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.
Similar content being viewed by others
Author information
Authors and Affiliations
Additional information
Received: 29 September 1998 / Revised version: 1 July 1999
Rights and permissions
About this article
Cite this article
Reiß, C., Bender, M. & Reinhard, PG. Nuclear shell gaps at finite temperatures . EPJ A 6, 157–165 (1999). https://doi.org/10.1007/s100500050330
Issue Date:
DOI: https://doi.org/10.1007/s100500050330