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

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 …

Heavy atomic nuclei have an excess of neutrons over protons, which leads to the formation
of a neutron skin whose thickness is sensitive to details of the nuclear force. This links …

The symmetry energy and its density dependence are crucial inputs for many nuclear
physics and astrophysics applications, as they determine properties ranging from the …

The recent experimental determination of the parity violating asymmetry A PV in Ca 48 and
Pb 208 at Jefferson Lab is important for our understanding on how neutrons and protons …

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 …

Despite their long history and astrophysical importance, some of the key properties of
neutron stars are still uncertain. The extreme conditions encountered in their interiors …

We introduce a new framework for quantifying correlated uncertainties of the infinite-matter
equation of state derived from chiral effective field theory (χ EFT). Bayesian machine …

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

We tabulate the atomic mass excesses and binding energies, ground-state shell-plus-
pairing corrections, ground-state microscopic corrections, and nuclear ground-state …