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 …

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 …

Pulsar glitches are rapid spin-up events that occur in the rotation of neutron stars, providing
a valuable probe into the physics of the interiors of these objects. Long-term monitoring of a …

This review focuses on applications of the ideas of superfluidity and superconductivity in
neutron stars in a broader context, ranging from the microphysics of pairing in nucleonic …

As mature neutron stars are cold (on the relevant temperature scale), one has to carefully
consider the state of matter in their interior. The outer kilometre or so is expected to freeze to …

Background: An accurate determination of the core-crust transition is necessary in the
modeling of neutron stars for astrophysical purposes. The transition is intimately related to …

The D1 family of parametrizations of the Gogny interaction commonly suffers from a rather
soft neutron matter equation of state that leads to maximal masses of neutron stars well …

Braking index measurements offer the opportunity to explore the processes affecting the
long-term spin evolution of pulsars and possible evolutionary connections between the …

The crust of a neutron star is thought to be comprised of a lattice of nuclei immersed in a sea
of free electrons and neutrons. As the neutrons are superfluid, their angular momentum is …

Neutron stars are unique cosmic laboratories in which fundamental physics can be probed
in extreme conditions not accessible to terrestrial experiments. In particular, the precise …