Dependence of weak interaction rates on the nuclear composition during stellar core collapse

  title={Dependence of weak interaction rates on the nuclear composition during stellar core collapse},
  author={Shun Furusawa and Hiroki Nagakura and Kohsuke Sumiyoshi and Chinami Kato and Shoichi Yamada},
  journal={Physical Review C},
We investigate the influences of the nuclear composition on the weak interaction rates of heavy nuclei during the core collapse of massive stars. The nuclear abundances in nuclear statistical equilibrium (NSE) are calculated by some equation of state (EOS) models including in-medium effects on nuclear masses. We systematically examine the sensitivities of electron capture and neutrino-nucleus scattering on heavy nuclei to the nuclear shell effects and the single-nucleus approximation. We find… 
Comparing Treatments of Weak Reactions with Nuclei in Simulations of Core-collapse Supernovae
We perform an extensive study of the influence of nuclear weak interactions on core-collapse supernovae, paying particular attention to consistency between nuclear abundances in the equation of state
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
Sensitivity of nuclear statistical equilibrium to nuclear uncertainties during stellar core collapse
I have systematically investigated the equations of state (EOSs) in nuclear statistical equilibrium under thermodynamic conditions relevant for core collapse of massive stars by varying the bulk
Equilibrium nuclear ensembles taking into account vaporization of hot nuclei in dense stellar matter
We investigate the high-temperature effect on the nuclear matter that consists of mixture of nucleons and all nuclei in the dense and hot stellar environment. The individual nuclei are described
Nuclear Equation of state for Compact Stars and Supernovae
The equation of state (EoS) of hot and dense matter is a fundamental input to describe static and dynamical properties of neutron stars, core-collapse supernovae and binary compact-star mergers. We
Nuclear Statistical Equilibrium equation of state for core collapse
Nuclei in central engine of core-collapse supernovae
This article summarizes recent works by the author (Furusawa, 2013, Astrophys. J. 772, 95, Nagakura 2017, The Astrophysical Journal Supplement Series 229, 42, Furusawa, 2018, Phys. Rev. C 98, 065802,
A new equation of state for core-collapse supernovae based on realistic nuclear forces and including a full nuclear ensemble
We have constructed a nuclear equation of state (EOS) that includes a full nuclear ensemble for use in core-collapse supernova simulations. It is based on the EOS for uniform nuclear matter that two


Annual Review Of Nuclear And Particle Science
The contents of this review reflect some of the shifts of emphasis that are occurring among the fields of astrophysics, nuclear physics, and elementary particle physics. Particle physics has made
Nuclear Structure
IN a recent note in NATURE,1 Bartlett has shown that the nuclei of the light elements may be represented by a model built up of appropriate numbers of neutrons and protons arranged in independent
Atomic Data and Nuclear Data Tables
a b s t r a c t The ab initio quasirelativistic Hartree–Fock method developed specifically for the calculation of spectral parameters of heavy atoms and highly charged ions is used to derive
For a small driven system coupled strongly to a heat bath, internal energy and exchanged heat are identified such that they obey the usual additive form of the first law. By identifying this exchanged
and a at
The xishacorene natural products are structurally unique apolar diterpenoids that feature a bicyclo[3.3.1] framework. These secondary metabolites likely arise from the well-studied, structurally
  • J. Suppl. 58, 771
  • 1985
Nuclear Physics A 957
  • 188
  • 2017
  • Phys. A 957, 188
  • 2017
  • J. 252, 715
  • 1982