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 …

Laboratory experiments sensitive to the equation of state of neutron rich matter in the vicinity
of nuclear saturation density provide the first rung in a “density ladder” that connects …

Many neutron star properties, such as the proton fraction, reflect the symmetry energy
contributions to the equation of state that dominate when neutron and proton densities differ …

Constraints set on key parameters of the nuclear matter equation of state (EoS) by the
values of the tidal deformability, inferred from GW170817, are examined by using a diverse …

Metamodeling for the nucleonic equation of state (EOS), inspired from a Taylor expansion
around the saturation density of symmetric nuclear matter, is proposed and parameterized in …

We propose the existence of a lower bound on the energy of pure neutron matter (PNM) on
the basis of unitary-gas considerations. We discuss its justification from experimental studies …

Background: The microscopic composition and properties of infinite hadronic matter at a
wide range of densities and temperatures have been subjects of intense investigation for …

One of the major uncertainties in the dense matter equation of state has been the nuclear
symmetry energy. The density dependence of the symmetry energy is important in nuclear …

The speed of sound of the matter within neutron stars may contain nonsmooth structure
related to first-or higher-order phase transitions. Here we investigate what are the …