Laboratory experiments sensitive to the equation of state of neutron rich matter in the vicinity
of nuclear saturation density provide the first rung in a “density ladder” that connects …

Now 50 years since the existence of the neutron star crust was proposed, we review the
current understanding of the nuclear physics of the outer layers of accreting neutron stars …

A general review of the crystalline solutions of the generalized Skyrmemodel and their
application to the study of cold nuclear matter at finite density and the Equation of State …

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 …

In this work, we estimate how much bulk viscosity driven by Urca processes is likely to affect
the gravitational wave signal of a neutron star coalescence. In the late inspiral, we show that …

By numerically inverting the Tolman-Oppenheimer-Volkov (TOV) equation using an explicitly
isospin-dependent parametric Equation of State (EOS) of dense neutron-rich nucleonic …

Young, rapidly spinning magnetars are invoked as central engines behind a diverse set of
transient astrophysical phenomena, including gamma-ray bursts, superluminous …

The neutron skin thickness Δ r np of heavy nuclei is essentially determined by the symmetry
energy density slope L (ρ) at ρ c= 0.11 fm− 3≈ 2/3 ρ 0 (ρ 0 is nuclear saturation density) …

We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear
matter under neutron star merger conditions, in the temperature range 1mEv< T≲ 5 mEv. We …

We review the prospects for detecting quark matter in neutron star cores. We survey the
proposed signatures and emphasize the importance of data from neutron star mergers …