The rprocess in the light of a microscopic model for nuclear masses
Abstract
The influence of nuclear mass models on the rabundance distribution is investigated in the framework of the canonical rprocess model. Among the nuclear properties of interest for the rprocess, nuclear masses clearly have the most decisive influence. They not only determine the position of the neutron drip line, the value of the neutron separation energies and the betadecay Qvalues (and consequently affect the neutron capture cross sections and the betadecay rates), but also indirectly modify the rates of fission and betadelayed processes. All rprocess calculations have so far made use of droplettype mass formulas only, the reliability of which remains very uncertain along the rprocess path (i.e., far off the experimentally known region). A new mass table based on the microscopic Extended ThomasFermi plus Strutinsky Integral method is now available and has been used to calculate the production of rnuclei within the waiting point approximation. The rabundance distribution obtained with microscopic masses shows significant differences from the one derived with a droplet mass formula. These differences are analyzed in detail.
 Publication:

Astronomy and Astrophysics
 Pub Date:
 August 1992
 Bibcode:
 1992A&A...262...73G
 Keywords:

 Astronomical Models;
 Neutron Cross Sections;
 Nuclear Fusion;
 Particle Mass;
 Supernovae;
 Abundance;
 Canonical Forms;
 Neutron Decay;
 Astrophysics