Stellar weak interaction rates for intermediate-mass nuclei. IV - Interpolation procedures for rapidly varying lepton capture rates using effective log (ft)-values

@article{Fuller1985StellarWI,
  title={Stellar weak interaction rates for intermediate-mass nuclei. IV - Interpolation procedures for rapidly varying lepton capture rates using effective log (ft)-values},
  author={George M. Fuller and William A. Fowler and M. J. Newman},
  journal={The Astrophysical Journal},
  year={1985},
  volume={293},
  pages={1-16}
}
Simple expressions for continuum electron and positron capture phase space factors and the associated neutrino energy loss integrals are presented in terms of standard Fermi integrals. Continuous approximations to the relevant Fermi integrals and their first derivatives are made. These allow the computation of effective log (ft)--values, at each temperature and density point, for the continuum lepton capture rates considered in the earlier papers in this series. Since the effective log (ft… 

Tables from this paper

Estimates of stellar weak interaction rates for nuclei in the mass range A=65-80
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 grid appropriate for
Expanded calculation of weak-interaction-mediated neutrino cooling rates due to 56 Ni in stellar matter
An accurate estimate of the neutrino cooling rates is required in order to study the various stages of stellar evolution of massive stars. Neutrino losses from proto-neutron stars play a crucial role
Stellar electron capture rates on neutron-rich nuclei and their impact on stellar core collapse
During the late stages of gravitational core-collapse of massive stars, extreme isospin asymmetries are reached within the core. Due to the lack of microscopic calculations of electron capture (EC)
Energy rates due to weak decay rates of vanadium isotopes in stellar environment
The neutrino cooling and gamma heating rates are considered as an important input needed to study the final phases of the evolution of high-mass stars. The weak-interaction mediated processes, namely
Impact of electron capture rates for nuclei far from stability on core-collapse supernovae
The impact of electron-capture (EC) cross sections on neutron-rich nuclei on the dynamics of core-collapse during infall and early post-bounce is studied performing spherically symmetric simulations
Electron capture in stars
TLDR
To derive reliable capture rates for core-collapse supernovae, a dedicated strategy has been developed based on a hierarchy of nuclear models specifically adapted to the abundant nuclei and astrophysical conditions present under various collapse conditions.
Description of weak-interaction rates within the relativistic energy density functional theory
A new theoretical framework has been established and applied in the calculation of electron capture (EC) and β-decay rates in stellar environment, characterized by high density and temperature. For
...
...

References

SHOWING 1-3 OF 3 REFERENCES
M. 1984, Nucl. Phys., submitted
  • Proc. Internat. Conf. on Spin Excitations in Nuclei
  • 1979
Atomic Data Nucl
    Atomic Data Nucl. Data Tobles
    • 1978