We review the current status and recent progress of microscopic many-body approaches
and phenomenological models, which are employed to construct the equation of state of …

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 …

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 …

The theory of the nuclear energy-density functional is used to provide a unified and
thermodynamically consistent treatment of all regions of cold non-accreting neutron stars. In …

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 …

We put constraints on the secondary component of GW190814 by analyzing the
observational data of the event. The relativistic mean-field models are used to calculate the …

If a phase transition is allowed to take place in the core of a compact star, a new stable
branch of equilibrium configurations can appear, providing solutions with the same mass as …

Among the various oscillation modes of neutron stars, f-and g-modes are the most likely to
be ultimately observed in binary neutron star mergers due to their relatively large coupling …

Neutron stars serve as excellent next-generation thermal detectors of dark matter, heated by
the scattering and annihilation of dark matter accelerated to relativistic speeds in their deep …