Comparison of statistical treatments for the equation of state for core-collapse supernovae

Abstract

Neutrinos emitted during the collapse, bounce and subsequent explosion provide information about supernova dynamics. The neutrino spectra are determined by weak interactions with nuclei and nucleons in the inner regions of the star, and thus the neutrino spectra are determined by the composition of matter. The composition of stellar matter at temperature ranging from $T=1-3$ MeV and densities ranging from $10^{-5}$ to 0.1 times the saturation density is explored. We examine the single-nucleus approximation commonly used in describing dense matter in supernova simulations and show that, while the approximation is accurate for predicting the energy and pressure at most densities, it fails to predict the composition accurately. We find that as the temperature and density increase, the single nucleus approximation systematically overpredicts the mass number of nuclei that are actually present and underestimates the contribution from lighter nuclei which are present in significant amounts.

12 pages, 11 figures

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Cited by in corpus (25)

• Equations of state for supernovae and compact stars
• New Equations of State in Simulations of Core-Collapse Supernovae
• The Overarching Framework of Core-Collapse Supernova Explosions as Revealed by 3D Fornax Simulations
• Symmetry energy impact in simulations of core-collapse supernovae
• A New Open-Source Nuclear Equation of State Framework based on the Liquid-Drop Model with Skyrme Interaction
• Statistical approach for supernova matter
• Statistical description of complex nuclear phases in supernovae and proto-neutron stars
• Deep Crustal Heating in a Multicomponent Accreted Neutron Star Crust
• A comparative study of statistical models for nuclear equation of state of stellar matter
• Towards an Understanding of the Resolution Dependence of Core-Collapse Supernova Simulations
• Comparing treatments of weak reactions with nuclei in simulations of core-collapse supernovae
• The equation of state and composition of hot, dense matter in core-collapse supernovae
• Clusterized nuclear matter in the (proto-)neutron star crust and the symmetry energy
• Hot and Dense Homogeneous Nucleonic Matter Constrained by Observations, Experiment, and Theory
• Composition of nuclear matter with light clusters and Bose-Einstein condensation of $\alpha$ particles
• Ensemble in-equivalence in supernova matter within a simple model
• Hot and Dense Matter Equation of State Probability Distributions for Astrophysical Simulations
• Light clusters in dilute heavy-baryon admixed nuclear matter
• The proto-neutron star inner crust in a multi-component plasma approach
• Sensitivity of nuclear statistical equilibrium to nuclear uncertainties during stellar core collapse
• Fragments' internal and kinetic temperatures in the framework of a Nuclear Statistical Multifragmentation Model
• Light clusters in the liquid proto-neutron star inner crust
• Phase diagram of neutron-rich nuclear matter and its impact on astrophysics
• Some aspects of the phase diagram of nuclear matter relevant to compact stars
• Isobar correlations bearing information on the properties of hot disassembling nuclear sources