The Microscopic Approach to Nuclear Matter and Neutron Star Matter

Abstract

We review a variety of theoretical and experimental investigations aimed at improving our knowledge of the nuclear matter equation of state. Of particular interest are nuclear matter extreme states in terms of density and/or isospin asymmetry. The equation of state of matter with unequal concentrations of protons and neutrons has numerous applications. These include heavy-ion collisions, the physics of rare, short-lived nuclei and, on a dramatically different scale, the physics of neutron stars. The "common denominator" among these (seemingly) very different systems is the symmetry energy, which plays a crucial role in both the formation of the neutron skin in neutron-rich nuclei and the radius of a neutron star (a system 18 orders of magnitude larger and 55 orders of magnitude heavier). The details of the density dependence of the symmetry energy are not yet sufficiently constrained. Throughout this article, our emphasis will be on the importance of adopting a microscopic approach to the many-body problem, which we believe to be the one with true predictive power.

56 pages, review article to appear in the International Journal of Modern Physics E

References in corpus (13)

• Neutron Star Observations: Prognosis for Equation of State Constraints
• A Radio Pulsar Spinning at 716 Hz
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Nuclear multifragmentation and phase transition for hot nuclei
• Relativistic model for nuclear matter and atomic nuclei with momentum-dependent self-energies
• The physics of dense hadronic matter and compact stars
• The High-Density Symmetry Energy and Direct Urca
• Thermal effects on nuclear symmetry energy with a momentum-dependent effective interaction
• The neutron skin of ${}^{208}$Pb and the density dependence of the symmetry energy
• Effects of $\Lambda$ hyperons on the nuclear equation of state in a Dirac-Brueckner-Hartree-Fock model
• Temperature and momentum dependence of single-particle properties in hot asymmetric nuclear matter
• Nuclear symmetry energy effects on neutron stars properties
• The mean free path of protons and neutrons in isospin-asymmetric nuclear matter

Cited by in corpus (40)

• Equations of state for supernovae and compact stars
• Constraints on the symmetry energy and neutron skins from experiments and theory
• Coupled-cluster computations of atomic nuclei
• Accurate nuclear radii and binding energies from a chiral interaction
• Coupled-cluster calculations of nucleonic matter
• Towards an ab initio covariant density functional for nuclear structure
• Extracting Nuclear Symmetry Energies at High Densities from Observations of Neutron Stars and Gravitational Waves
• GW190814's secondary component with mass $(2.50-2.67)$ M${}_{\odot }$ as a super-fast pulsar
• On the Maximum Mass of Neutron Stars
• Dirac-Brueckner-Hartree-Fock versus chiral effective field theory
• The Nuclear Matter Symmetry Energy at $0.03\le \rho /{\rho }_0\le 0.2$
• Probing isospin- and momentum-dependent nuclear effective interactions in neutron-rich matter
• Constraining the nuclear symmetry energy and properties of neutron star from GW170817 by Bayesian analysis
• Ruling out the supersoft high-density symmetry energy from the discovery of PSR J0740+6620 with mass $2.14_{-0.09}^{+0.10}{M}_{\odot }$
• Lorentz covariant nucleon self-energy decomposition of the nuclear symmetry energy
• Correlations between charge radii differences of mirror nuclei and stellar observables
• Exact versus Taylor-expanded energy density in the study of the neutron star crust-core transition
• Deformation properties with a finite range simple effective interaction
• Contribution of isovector mesons to the symmetry energy in a microscopic model
• Study of spin polarized nuclear matter and finite nuclei with finite range simple effective interaction
• Properties of neutron star described by a relativistic $abinitio$ model
• Nonparametric model for the equations of state of neutron star from deep neural network
• Microscopic in-medium nucleon-nucleon cross sections with improved Pauli blocking effects
• Microscopic approach to the nucleon-nucleon effective interaction and nucleon-nucleon scattering in symmetric and isospin-asymmetric nuclear matter
• Properties of nuclear matter in relativistic Brueckner-Hartree-Fock model with high-precision charge-dependent potentials
• Reconstructed primary fragments and symmetry energy, temperature and density of the fragmenting source in ${}^{64}$Zn + ${}^{112}$Sn at 40 MeV/nucleon
• Spin- and isospin-polarized states of nuclear matter in the Dirac-Brueckner-Hartree-Fock model
• Hot and dense matter beyond relativistic mean field theory
• Low-momentum interactions with Brown-Rho-Ericson scalings and the density dependence of the nuclear symmetry energy
• Dense matter equation of state and phase transitions from a Generalized Skyrme model
• Solution of the Bethe-Goldstone Equation without Partial Wave Decomposition
• Influence of the nuclear matter equation of state on the r-mode instability using the finite-range simple effective interaction
• The finite range simple effective interaction including tensor terms
• In-medium nucleon-nucleon cross-sections with non-spherical Pauli blocking
• The splitting of the one-body potential in spin-polarized isospin-symmetric nuclear matter
• Equation of State of Hot Neutron Star Matter using Finite Range Simple Effective Interaction
• Probing the sensitivity of the total nucleus-nucleus reaction cross section at intermediate energies to medium effects and isospin asymmetries
• An effective Nuclear Model: from Nuclear Matter to Finite Nuclei
• The impact of charge symmetry and charge independence breaking on the properties of neutrons and protons in isospin-asymmetric nuclear matter
• Neutron stars within relativistic central variational method