Bayesian refinement of covariant energy density functionals
arXiv:2301.09692 · doi:10.1103/PhysRevC.107.045802
Abstract
The last five years have seen remarkable progress in our quest to determine the equation of state of neutron rich matter. Recent advances across the theoretical, experimental, and observational landscape have been incorporated in a Bayesian framework to refine existing covariant energy density functionals previously calibrated by the properties of finite nuclei. In particular, constraints on the maximum neutron star mass from pulsar timing, on stellar radii from the NICER mission, on tidal deformabilities from the LIGO-Virgo collaboration, and on the dynamics of pure neutron matter as predicted from chiral effective field theories, have resulted in significant refinements to the models, particularly to those predicting a stiff symmetry energy. Still, even after these improvements, we find challenging to reproduce simultaneously the neutron skin thickness of both Pb and Ca recently reported by the PREX/CREX collaboration.
16 pages, 7 Figures, 3 Tables
References in corpus (22)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
- A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
- Neutron Star Observations: Prognosis for Equation of State Constraints
- Nuclear symmetry energy probed by neutron skin thickness of nuclei
- PSR J0952-0607: The Fastest and Heaviest Known Galactic Neutron Star
- Neutron skin of 208Pb, nuclear symmetry energy, and the parity radius experiment
- Neutron matter at next-to-next-to-next-to-leading order in chiral effective field theory
- Sound velocity bound and neutron stars
- Building relativistic mean field models for finite nuclei and neutron stars
- Incompressibility of neutron-rich matter
- Impact of the symmetry energy on the outer crust of non-accreting neutron stars
- A bound on the speed of sound from holography
- The nuclear symmetry energy and stability of matter in neutron star
- Relativistic description of dense matter equation of state and compatibility with neutron star observables: a Bayesian approach
- Impact of the neutron star crust on the tidal polarizability
- Implications of PREX-2 on the electric dipole polarizability of neutron rich nuclei
- Exact versus Taylor-expanded energy density in the study of the neutron star crust-core transition
- Analysis of the neutron matter equation of state and the symmetry energy up to fourth order of chiral effective field theory
- The Equation of State of Neutron-Rich Matter at Fourth Order of Chiral Effective Field Theory and the Radius of a Medium-Mass Neutron Star