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 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 …

Neutron-star cores contain matter at the highest densities in our Universe. This highly
compressed matter may undergo a phase transition where nuclear matter melts into …

In recent years our understanding of the dense matter equation of state (EOS) of neutron
stars has significantly improved by analyzing multimessenger data from radio/X-ray pulsars …

Observations of neutron-star mergers with distinct messengers, including gravitational
waves and electromagnetic signals, can be used to study the behavior of matter denser than …

The nuclear-physics landscape has been redesigned as a sequence of effective field
theories (EFTs) connected to the standard model through symmetries and lattice simulations …

The properties of neutron stars are determined by the nature of the matter that they contain.
These properties can be constrained by measurements of the star's size. We obtain stringent …

Observations of neutron stars, whether in binaries or in isolation, provide information about
the internal structure of the most extreme material objects in the Universe. In this work, we …

We use gravitational-wave observations of the binary neutron star merger GW170817 to
explore the tidal deformabilities and radii of neutron stars. We perform a Bayesian parameter …

Over the last decade, new developments in Similarity Renormalization Group techniques
and nuclear many-body methods have dramatically increased the capabilities of ab initio …