Neutron stars provide a window into the properties of dense nuclear matter. Several recent
observational and theoretical developments provide powerful constraints on their structure …

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 made of constraints on the nuclear symmetry energy parameters arising from
nuclear binding energy measurements, theoretical chiral effective field predictions of …

We combine the equation of state of dense matter up to twice nuclear saturation density n
sat obtained using chiral effective field theory (χ EFT) and recent observations of neutron …

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 …

The uncertainties in neutron star radii and crust properties due to our limited knowledge of
the equation of state are quantitatively analyzed. We first demonstrate the importance of a …

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 …

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 …

A whole decades research collated, organised and synthesised into one single book!
Following a 60-page review of the seminal treatises of Misner, Thorne, Wheeler and …

An equation of state (EOS) of neutron star matter, describing both the neutron star crust and
the liquid core, is calculated. It is based on the effective nuclear interaction SLy of the …