A review is given of various theoretical approaches for the equation of state (EoS) of dense
matter, relevant for the description of core-collapse supernovae, compact stars, and compact …

Supernova theory, numerical and analytic, has made remarkable progress in the past
decade. This progress was made possible by more sophisticated simulation tools, especially …

A statistical model for the equation of state and the composition of supernova matter is
presented. It consists of an ensemble of nuclei and interacting nucleons in nuclear statistical …

An 8.8 M⊙ electron-capture supernova was simulated in spherical symmetry consistently
from collapse through explosion to essentially complete deleptonization of the forming …

Massive stars end their lives in explosions with kinetic energies on the order of 10 51 erg.
Immediately after the explosion has been launched, a region of low density and high entropy …

The symmetry energy describes how the energy of nuclear matter rises as one goes away
from equal numbers of neutrons and protons. This is very important to describe neutron rich …

We discuss three new equations of state (EOS) in core-collapse supernova simulations. The
new EOS are based on the nuclear statistical equilibrium model of Hempel and Schaffner …

Neutrinos are known to play important roles in many astrophysical scenarios from the early
period of the big bang to current stellar evolution being a unique messenger of the fusion …

We perform state-of-the-art large-scale shell-model calculations of the structure factors for
elastic spin-dependent WIMP scattering off Xe 129, 131, I 127, Ge 73, F 19, Na 23, Al 27 …

Neutrino-driven winds, which follow core-collapse supernova explosions, present a
fascinating nuclear-astrophysics problem that requires an understanding of advanced …