Dense nuclear matter equation of state from heavy-ion collisions
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 …
experimental efforts in nuclear physics. With advances in microscopic theories for nuclear …
Nuclear effective field theory: status and perspectives
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 …
theories (EFTs) connected to the standard model through symmetries and lattice simulations …
From hadrons to quarks in neutron stars: a review
In recent years our understanding of neutron stars has advanced remarkably, thanks to
research converging from many directions. The importance of understanding neutron star …
research converging from many directions. The importance of understanding neutron star …
Nuclear physics multimessenger astrophysics constraints on the neutron star equation of state: adding NICER's PSR J0740+ 6620 measurement
In the past few years, new observations of neutron stars (NSs) and NS mergers have
provided a wealth of data that allow one to constrain the equation of state (EOS) of nuclear …
provided a wealth of data that allow one to constrain the equation of state (EOS) of nuclear …
Constraining the speed of sound inside neutron stars with chiral effective field theory interactions and observations
The dense matter equation of state (EOS) determines neutron star (NS) structure but can be
calculated reliably only up to one to two times the nuclear saturation density, using accurate …
calculated reliably only up to one to two times the nuclear saturation density, using accurate …
Constraining neutron-star matter with microscopic and macroscopic collisions
Interpreting high-energy, astrophysical phenomena, such as supernova explosions or
neutron-star collisions, requires a robust understanding of matter at supranuclear densities …
neutron-star collisions, requires a robust understanding of matter at supranuclear densities …
High-quality two-nucleon potentials up to fifth order of the chiral expansion
We present NN potentials through five orders of chiral effective field theory ranging from
leading order (LO) to next-to-next-to-next-to-next-to-leading order (N 4 LO). The construction …
leading order (LO) to next-to-next-to-next-to-next-to-leading order (N 4 LO). The construction …
Symmetry parameter constraints from a lower bound on neutron-matter energy
We propose the existence of a lower bound on the energy of pure neutron matter (PNM) on
the basis of unitary-gas considerations. We discuss its justification from experimental studies …
the basis of unitary-gas considerations. We discuss its justification from experimental studies …
Unified equations of state for cold non-accreting neutron stars with Brussels–Montreal functionals–I. Role of symmetry energy
JM Pearson, N Chamel, AY Potekhin… - Monthly Notices of …, 2018 - academic.oup.com
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 …
thermodynamically consistent treatment of all regions of cold non-accreting neutron stars. In …
Combining electromagnetic and gravitational-wave constraints on neutron-star masses and radii
We perform a joint Bayesian inference of neutron-star mass and radius constraints based on
GW170817, observations of quiescent low-mass x-ray binaries (QLMXBs), photospheric …
GW170817, observations of quiescent low-mass x-ray binaries (QLMXBs), photospheric …