We present a practical solution to the ''sign problem''in the auxiliary field Monte Carlo
approach to the nuclear shell model. The method is based on extrapolation from a …

Nuclear weak interaction rates for fp-and fpg-shell nuclei in stellar matter and the associated
energy losses are calculated using a modified form of proton–neutron quasiparticle random …

We estimate lepton capture and emission rates, as well as neutrino energy loss rates, for
nuclei in the mass range A= 65–80. These rates are calculated on a temperature/density …

Measurements of the (n, p) reaction cross section on Ni 6 0, 6 2, 6 4 have been made at 198
MeV for θ lab= 0–20 in 4 steps. Multipole analyses have been performed on the resulting …

We have calculated the Gamow-Teller strength distributions for the ground states and first
excited states in 55Co and 56Ni. These calculations have been performed by shell model …

Recently (Brown\& Bethe 1994) it was suggested that most stars with main sequence mass
in the range of about $18-30 M_ {\odot} $ explode, returning matter to the Galaxy, and then …

We calculate supernova electron capture and β-decay rates for various pf-shell nuclei using
large-scale shell-model techniques. We show that the centroid of the Gamow-Teller strength …

The thermonuclear explosion of massive white dwarfs is believed to explain at least a
fraction of Type Ia supernovae (SNIa). After thermal runaway, electron captures on the ashes …

Using the theory of relativity in superstrong magnetic fields (SMFs) and a nuclear shell
model, we carry out an estimation of electron capture (EC) rates on iron-group nuclei in …

At densities between 108 and 1010 g/cm3 electron capture in a presupernova collapse is
believed to mainly occur on odd-odd nuclei. We have derived the rates for six of the most …