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 …

Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared
goal of both nuclear physics and astrophysics. Except possible phase transitions, the density …

The surface of neutron-rich heavy nuclei, with a neutron skin created by excess neutrons,
provides an important terrestrial model system to study dilute neutron-rich matter. By using …

We develop a kinetic approach to the production of light nuclei up to mass number A⩽ 4 in
intermediate-energy heavy-ion collisions by including them as dynamic degrees of freedom …

The Equation of State (EOS) of uniform neutron-rich nucleonic matter of isospin asymmetry
δ=(ρ n—ρ p)/ρ and density ρ can be expressed in terms of the energy per nucleon E (ρ, δ) …

Within the framework of an extended quantum molecular dynamics model, we simulated Ca
40+ O 16 collisions at beam energies ranging from 60 to 150 MeV/nucleon for O 16 with …

A nucleus is a quantum many body system made of strongly interacting Fermions, protons
and neutrons (nucleons). This produces a rich Nuclear Equation of State whose knowledge …

We compare three different statistical models for the equation of state (EOS) of stellar matter
at subnuclear densities and temperatures (0.5–10 MeV) expected to occur during the …

The issue of cluster production in heavy-ion collisions is addressed in a new manner, by
implementing cluster correlation into the quantum molecular dynamics (QMD) transport …

The modification of the ground state properties of light atomic nuclei in the nuclear and
stellar medium is addressed, using chemical equilibrium constants evaluated from a new …