Nuclear Statistical Equilibrium Equation of State for Core Collapse
arXiv:1807.06871 · doi:10.1016/j.nuclphysa.2018.11.003
Abstract
Extensive calculations of properties of supernova matter are presented, using the extended Nuclear Statistical Equilibrium model of PRC92 055803 (2015) based on a statistical distribution of Wigner-Seitz cells modeled using realistic nuclear mass and level density tables, complemented with a non-relativistic Skyrme functional for unbound particles and beyond drip-line nuclei. Both thermodynamic quantities and matter composition are examined as a function of baryonic density, temperature, and proton fraction, within a large domain adapted for applications in supernova simulations. The results are also provided in the form of a table, with grid mesh and format compatible with the CompOSE platform [http://compose.obspm.fr/] for direct use in supernova simulations. Detailed comparisons are also presented with other existing databases, all based on relativistic mean-field functionals, and the differences between the different models are outlined. We show that the strongest impact on the predictions is due to the different hypotheses used to define the cluster functional and its modifications due to the presence of a nuclear medium.
33 pages, 8 figures
References in corpus (14)
- Theory of Core-Collapse Supernovae
- Symmetry Energy I: Semi-Infinite Matter
- A New Open-Source Nuclear Equation of State Framework based on the Liquid-Drop Model with Skyrme Interaction
- The pasta phase within density dependent hadronic models
- A new equation of state for core-collapse supernovae based on realistic nuclear forces and including a full nuclear ensemble
- Statistical description of complex nuclear phases in supernovae and proto-neutron stars
- A comparative study of statistical models for nuclear equation of state of stellar matter
- Supernova equations of state including full nuclear ensemble with in-medium effects
- Light nuclei in supernova envelopes: a quasiparticle gas model
- Dependence of weak interaction rates on the nuclear composition during stellar core collapse
- Light clusters in warm stellar matter: explicit mass shifts and universal cluster-meson couplings
- Stellar electron capture rates on neutron-rich nuclei and their impact on core-collapse
- Pasta phases within the QMC model
- Composition of nuclear matter with light clusters and Bose-Einstein condensation of particles
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- Light Neutral Clusters in Supernova Matter
- New {\em ab initio} constrained extended Skyrme equations of state for simulations of neutron stars, supernovae and binary mergers: I. Subsaturation density domain