Mathieu Samyn

A Hartree-Fock-Bogoliubov mass formula

In order to have more reliable predictions of nuclear masses at the neutron drip line, we here go beyond the recent mass formula HFBCS-1 and present a new mass formula, HFB-1, based on the Hartree-Fock-Bogoliubov method. As with the HFBCS-1 mass formula, we use a 10-parameter Skyrme force along with a 4-parameter δ-function pairing force and a 2-parameter phenomenological Wigner term. However, with the original HFBCS-1 Skyrme force (MSk7), the rms error becomes unacceptably large and a new force fit is required. With the isoscalar and isovector effective masses constrained to be equal, the remaining 15 degrees of freedom are fitted to the masses of all the 1754 measured nuclei with A ≥ 16, N - Z > 2 given in the 1995 Audi-Wapstra compilation. The rms error with respect to the masses of all the 1888 measured nuclei with Z, N ≥ 8 is 0.764 MeV. A complete mass table, HFB-1 (available on the Web), has been constructed, giving all nuclei lying between the two drip lines over the range Z, N ≥ 8 and Z ≤ 120. A comparison between HFB-1 and HFBCS-1 mass tables shows that the HFBCS model is a very good approximation of the HFB theory, in particular for masses, the extrapolated masses never differing by more than 2 MeV below Z ≤ 110. We also find that the behaviour of shell gaps far away from the region of beta stability does not depend on whether the HFBCS or HFB methods are used, in particular, no quenching of astrophysical interest arises from replacing the BCS method by the Bogoliubov method.

Microscopic HFB+QRPA predictions of dipole strength for astrophysics applications

Abstract Large-scale QRPA calculations of the E1-strength are performed on top of HFB calculations in order to derive the radiative neutron capture cross sections for the whole nuclear chart. The HFB + QRPA predictions based on various Skyrme forces with different pairing prescriptions and parameterizations are confronted with experimental photoabsorption data for spherical nuclei. Within the approximations of the present model, the effective nucleon–nucleon interaction is probed with the GDR data. The dipole strengths obtained with the present HFB + QRPA model is finally used to estimate the radiative neutron capture cross section for all nuclei of relevance in astrophysics applications. The resulting rates are shown to be close to the one predicted with the previously determined HFBCS + QRPA model, but for neutron-rich nuclei to differ significantly from the ones obtained with the empirical Lorentzian-like formula.

Further explorations of Skyrme-Hartree-Fock-Bogoliubov mass formulas: II. Role of the effective mass

We have constructed four new complete mass tables, referred to as (Hartree-Fock-Bogoliubov) HFB-4 to HFB-7, each one including all the 9200 nuclei lying between the two drip lines over the range of

Further explorations of Skyrme-Hartree-Fock-Bogoliubov mass formulas. III: Role of particle-number projection

Z

The r-process nucleosynthesis: a continued challenge for nuclear physics and astrophysics

and

The r-process in supernovae: impact of new microscopic mass formulas

N\ensuremath{\geqslant}8

Hartree‐Fock‐Bogoliubov Fission Barriers with Skyrme Forces Adjusted on Masses

and

Calculations of Fission Properties Using Microscopic Models for Astrophysics Applications

Z\ensuremath{\leqslant}120

Nuclear mass predictions within the skyrme HFB theory

. HFB-4 and HFB-5 have the isoscalar effective mass

Hartree-Fock-Bogoliubov Mass Models and the Equation of State of Neutron-Star Crusts

{M}_{s}^{*}