Equation of state and neutrino transfer in supernovae and neutron stars
arXiv:2112.11159 · doi:10.1140/epja/s10050-021-00644-z
Abstract
We overview the progress of the tables of the equation of state for astrophysical simulations and the numerical methods of neutrino transfer. Hot and dense matter play essential roles in core-collapse supernovae and neutron stars. Equation of state determines the structure of compact objects and their dynamics through its behavior of thermodynamic quantities. In addition, neutrinos are trapped in supernova cores and neutron star mergers and frequently interact with matter to crucially affect dynamics in determining the explosion mechanism and the final form of compact objects. Therefore, it is essential to implement detailed processes of nuclear and neutrino physics in numerical simulations by having reliable data set of the equation of state and reaction rates. We show examples of developments of the equation of state and the neutrino transfer and discuss research directions toward understanding the explosive phenomena by the first principle calculation.
13 pages, 4 figures; contribution to the EPJ A topical issue "CompOSE: a repository for Neutron Star Equations of State and Transport Properties"
References in corpus (34)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Multi-messenger Observations of a Binary Neutron Star Merger
- PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
- Neutron-Rich Nuclei in Heaven and Earth
- Implications of PREX-II on the equation of state of neutron-rich matter
- Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
- Relativistic effective interaction for nuclei, giant resonances, and neutron stars
- Signals of the QCD phase transition in core-collapse supernovae
- Neutron Stars and the Nuclear Equation of State
- New Hyperon Equations of State for Supernovae and Neutron Stars in Density-dependent Hadron Field Theory
- Neutrino-driven supernova of a low-mass iron-core progenitor boosted by three-dimensional turbulent convection
- Towards Understanding Astrophysical Effects of Nuclear Symmetry Energy
- Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces
- Tables of Hyperonic Matter Equation of State for Core-Collapse Supernovae
- A New Open-Source Nuclear Equation of State Framework based on the Liquid-Drop Model with Skyrme Interaction
- Astrophysical Implications of Equation of State for Hadron-Quark Mixed Phase: Compact Stars and Stellar Collapses
- Neutrino signals from the formation of black hole: a probe of equation of state of dense matter
- Three-dimensional Boltzmann-Hydro code for core-collapse in massive stars I. special relativistic treatments
- Appearance of Light Clusters in Post-bounce Evolution of Core-Collapse Supernovae
- Effects of symmetry energy on equation of state for simulations of core-collapse supernovae and neutron-star mergers
- A new equation of state for core-collapse supernovae based on realistic nuclear forces and including a full nuclear ensemble
- A Detailed Comparison of Multi-Dimensional Boltzmann Neutrino Transport Methods in Core-Collapse Supernovae
- Effects of the symmetry energy on properties of neutron star crusts near the neutron drip density
- Comparing treatments of weak reactions with nuclei in simulations of core-collapse supernovae
- Microscopic equation of state of hot nuclear matter for numerical relativity simulations
- Implications of PREX-2 on the electric dipole polarizability of neutron rich nuclei
- Influence of the symmetry energy on nuclear pasta in neutron star crusts
- Cooling timescale for protoneutron stars and properties of nuclear matter: Effective mass and symmetry energy at high densities
- Dependence of weak interaction rates on the nuclear composition during stellar core collapse
- Medium modifications for light and heavy nuclear clusters in simulations of core collapse supernovae -- Impact on equation of state and weak interactions
- Application of the nuclear equation of state obtained by the variational method to core-collapse supernovae
- Properties of neutrino transfer in a deformed remnant of neutron star merger
- Numerical Study of Stellar Core Collapse and Neutrino Emission Using the Nuclear Equation of State Obtained by the Variational Method
- Impact of neutrino pair-production rates in Core-Collapse Supernovae
Cited by in corpus (3)
- Dense Nuclear Matter Equation of State from Heavy-Ion Collisions
- Effects of nuclear matter and composition in core-collapse supernovae and long-term proto-neutron star cooling
- Self-consistent single-nucleon potential at positive energy produced by semi-realistic interaction and its examination via nucleon-nucleus elastic scattering