Perturbation Theory of Nuclear Matter with a Microscopic Effective Interaction

Abstract

An updated and improved version of the effective interaction based on the Argonne\textendash Urbana nuclear Hamiltonian\textemdash derived using the formalism of Correlated Basis Functions (CBF) and the cluster expansion technique\textemdash is employed to obtain a number of properties of cold nuclear matter at arbitrary neutron excess within the formalism of many-body perturbation theory. The numerical results\textemdash including the ground-state energy per nucleon, the symmetry energy, the pressure, the compressibility, and the single-particle spectrum\textemdash are discussed in the context of the available empirical information, obtained from measured nuclear properties and heavy-ion collisions.

References in corpus (32)

• An accurate nucleon-nucleon potential with charge-independence breaking
• The equation of state for nucleon matter and neutron star structure
• Determination of the Equation of State of Dense Matter
• Quantum Monte Carlo methods for nuclear physics
• Quantum Monte Carlo Calculations of $A\le 6$ Nuclei
• Constraints on the density dependence of the symmetry energy
• Chiral three-nucleon forces and neutron matter
• Constraining the neutron-proton effective mass splitting using empirical constraints on the density dependence of nuclear symmetry energy around normal density
• Evolution of Nuclear Spectra with Nuclear Forces
• Quantum Monte Carlo Calculations with Chiral Effective Field Theory Interactions
• Chiral Three-Nucleon Interactions in Light Nuclei, Neutron-$\alpha$ Scattering, and Neutron Matter
• The Nuclear Symmetry Energy
• Results of the ASY-EOS experiment at GSI: The symmetry energy at suprasaturation density
• Local chiral effective field theory interactions and quantum Monte Carlo applications
• Minimally non-local nucleon-nucleon potentials with chiral two-pion exchange including $\Delta$'s
• Constraining the symmetry energy at subsaturation densities using isotope binding energy difference and neutron skin thickness
• Asymmetric nuclear matter based on chiral two- and three-nucleon interactions
• Quantum Monte Carlo calculations of neutron matter with chiral three-body forces
• Local chiral potentials and the structure of light nuclei
• Constraints on the Skyrme Equations of State from Properties of Doubly Magic Nuclei
• Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies
• Variational calculation of the ground state of closed-shell nuclei up to $A=40$
• Shear viscosity of neutron matter from realistic nucleon-nucleon interactions
• Nuclear matter properties from local chiral interactions with $\Delta$ isobar intermediate states
• Neutron matter based on consistently evolved chiral three-nucleon interactions
• Microscopic calculations of transport properties of neutron matter
• Weak response of cold symmetric nuclear matter at three-body cluster level
• Quenching of Weak Interactions in Nucleon Matter
• Neutral current interactions of low-energy neutrinos in dense neutron matter
• Revisiting the Hugenholtz-Van Hove theorem in nuclear matter
• Effective interaction approach to the Fermi hard-sphere system
• Transport properties of the Fermi hard-sphere system

Cited by in corpus (11)

• Cooling timescale for protoneutron stars and properties of nuclear matter: Effective mass and symmetry energy at high densities
• Benchmark calculations of infinite neutron matter with realistic two- and three-nucleon potentials
• Tidal Deformation of Neutron Stars from Microscopic Models of Nuclear Dynamics
• The Photon in Dense Nuclear Matter I: Random Phase Approximation
• Scaling within the Spectral Function approach
• Accurate nuclear symmetry energy at finite temperature within a BHF approach
• The nuclear symmetry energy and the neutron skin thickness in nuclei
• Modeling Neutron Star Matter in the Age of Multimessenger Astrophysics
• Evolution of proto-neutron stars to pulsars, magnetars and central compact objects
• Relativistic Corrections to the CBF Effective Nuclear Hamiltonian
• Impact of three-nucleon forces on gravitational wave emission from neutron stars