The nuclear equation of state (EOS) is at the center of numerous theoretical and
experimental efforts in nuclear physics. With advances in microscopic theories for nuclear …

We summarize our current knowledge of neutron-star masses and radii. Recent
instrumentation and computational advances have resulted in a rapid increase in the …

Recent developments in the theory of pure neutron matter and experiments concerning the
symmetry energy of nuclear matter, coupled with recent measurements of high-mass …

The interpretation of pulsar rotational glitches, the sudden increase in spin frequency of
neutron stars, is a half-century-old challenge. The common view is that glitches are driven by …

Neutron stars are valuable laboratories for the study of dense matter. Recent observations
have uncovered both massive and low-mass neutron stars and have also set constraints on …

Radio pulsars are rapidly rotating highly magnetized neutron stars. This comprehensive
book is a unique resource that brings together the key observational techniques …

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 structure of neutron stars is considered from theoretical and observational perspectives.
We demonstrate an important aspect of neutron star structure: the neutron star radius is …

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 …

Neutron stars are some of the densest manifestations of massive objects in the universe.
They are ideal astrophysical laboratories for testing theories of dense matter physics and …