Despite their long history and astrophysical importance, some of the key properties of
neutron stars are still uncertain. The extreme conditions encountered in their interiors …

In this article, I introduce ideas and techniques to extract information about the equation of
state of matter at very high densities from gravitational waves emitted before, during and …

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 …

The symmetry energy contribution to the nuclear equation of state impacts various
phenomena in nuclear astrophysics, nuclear structure, and nuclear reactions. Its …

This paper presents a detailed assessment of the ability of the 240 Skyrme interaction
parameter sets in the literature to satisfy a series of criteria derived from macroscopic …

The nuclear symmetry energy characterizes the variation of the binding energy as the
neutron to proton ratio of a nuclear system is varied. This is one of the most important …

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 …