Equation of state and neutrino transfer in supernovae and neutron stars

TL;DR

This paper reviews recent advancements in the equation of state data and neutrino transfer methods crucial for simulating supernovae and neutron stars, emphasizing their roles in astrophysical dynamics.

Contribution

It provides an overview of the latest developments in equation of state tables and neutrino transfer techniques, highlighting their importance in astrophysical simulations.

Findings

Development of comprehensive equation of state tables for dense matter

Improved numerical methods for neutrino transfer in simulations

Insights into supernova explosion mechanisms and neutron star formation

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.