Ensembles of unified crust and core equations of state in a nuclear-multimessenger astrophysics environment
arXiv:2112.12108 · doi:10.1140/epja/s10050-022-00710-0
Abstract
We present an ensemble of unified neutron star crust and core equations of state, constructed using an extended Skyrme energy density functional through the crust and outer core, and appended by two piecewise polytropes at higher densities. The equations of state are parameterized by the first three coefficients in the density expansion of the symmetry energy and , the moment of inertia of a 1.338 M star and the maximum neutron star mass . We construct an ensemble with uniform priors on all five parameters, and then apply data filters to the ensemble to explore the effect of combining neutron skin data from PREX with astrophysical measurements of radii and tidal deformabilities from NICER and LIGO/VIRGO. Neutron skins are calculated directly using the EDFs. We demonstrate that both the nuclear data and astrophysical data play a role in constraining crust properties such as the mass, thickness and moment of inertia of the crust and the nuclear pasta layers therein, and that astrophysical data better constrains than PREX data.
arXiv comment11 Pages, 3 figures, 1 table; accepted by EPJA
References in corpus (87)
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- GW170817: Measurements of Neutron Star Radii and Equation of State
- 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
- A unified equation of state of dense matter and neutron star structure
- The Equation of State from Observed Masses and Radii of Neutron Stars
- Neutron Star Structure and the Neutron Radius of 208Pb
- Constraints on a phenomenologically parameterized neutron-star equation of state
- Constraining the Maximum Mass of Neutron Stars From Multi-Messenger Observations of GW170817
- Using gravitational-wave observations and quasi-universal relations to constrain the maximum mass of neutron stars
- Constraints on the symmetry energy and neutron skins from experiments and theory
- Evidence for quark-matter cores in massive neutron stars
- Accurate Determination of the Neutron Skin Thickness of Pb through Parity-Violation in Electron Scattering
- Nuclear symmetry energy probed by neutron skin thickness of nuclei
- Measurement of the Neutron Radius of 208Pb Through Parity-Violation in Electron Scattering
- Implications of PREX-II on the equation of state of neutron-rich matter
- I-Love-Q Relations in Neutron Stars and their Applications to Astrophysics, Gravitational Waves and Fundamental Physics
- Complete electric dipole response and the neutron skin in 208Pb
- Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
- I-Love-Q
- Modeling GW170817 based on numerical relativity and its implications
- Neutron skins and neutron stars in the multi-messenger era
- GW170817, General Relativistic Magnetohydrodynamic Simulations, and the Neutron Star Maximum Mass
- Neutron skin of 208Pb, nuclear symmetry energy, and the parity radius experiment
- Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory
- Constraining the speed of sound inside neutron stars with chiral effective field theory interactions and observations
- Constraints on neutron star radii based on chiral effective field theory interactions
- Pulsar Constraints on Neutron Star Structure and Equation of State
- Charge, neutron, and weak size of the atomic nucleus
- Approximate Universal Relations for Neutron Stars and Quark Stars
- Nonparametric constraints on neutron star matter with existing and upcoming gravitational wave and pulsar observations
- Neutron star radii and crusts: uncertainties and unified equations of state
- A NICER view of PSR J0030+0451: Implications for the dense matter equation of state
- A way forward in the study of the symmetry energy: experiment, theory, and observation
- Pulsar glitches: The crust is not enough
- The equation of state for dense nucleonic matter from a metamodeling. I. Foundational aspects
- Resonant Shattering of Neutron Star Crusts
- Constraints on the Symmetry Energy Using the Mass-Radius Relation of Neutron Stars
- Mapping crustal heating with the cooling lightcurves of quasi-persistent transients
- Tidal deformability from GW170817 as a direct probe of the neutron star radius
- Multimessenger Parameter Estimation of GW170817
- Higher-order effects on the incompressibility of isospin asymmetric nuclear matter
- Disordered nuclear pasta, magnetic field decay, and crust cooling in neutron stars
- Crustal Entrainment and Pulsar Glitches
- Spectral Representations of Neutron-Star Equations of State
- Non-parametric inference of the neutron star equation of state from gravitational wave observations
- Nonparametric Inference of Neutron Star Composition, Equation of State, and Maximum Mass with GW170817
- Electric dipole polarizability of Ca and implications for the neutron skin
- Reconstructing the Neutron-Star Equation of State from Astrophysical Measurements
- A highly resistive layer within the crust of X-ray pulsars limits their spin periods
- Quantum Monte Carlo calculations of neutron matter with chiral three-body forces
- Using Neutron Star Observations to Determine Crust Thicknesses, Moments of Inertia, and Tidal Deformabilities
- Neutron Matter from Low to High Density
- Astrophysical and theoretical physics implications from multimessenger neutron star observations
- Neutron skins of atomic nuclei: per aspera ad astra
- Probing the Equation of State of Nuclear Matter via Neutron Star Asteroseismology
- Constraints on Neutron Star Crusts From Oscillations in Giant Flares
- A survey of the parameter space of the compressible liquid drop model as applied to the neutron star inner crust
- Dipole polarizability of 120Sn and nuclear energy density functionals
- Upper limits on the observational effects of nuclear pasta in neutron stars
- Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817
- New equations of state constrained by nuclear physics, observations, and QCD calculations of high-density nuclear matter
- Confronting gravitational-wave observations with modern nuclear physics constraints
- Combining Electromagnetic and Gravitational-Wave Constraints on Neutron-Star Masses and Radii
- Towards mitigation of apparent tension between nuclear physics and astrophysical observations by improved modeling of neutron star matter
- Bayesian analysis of the crust-core transition with a compressible liquid-drop model
- Equation of state constraints from nuclear physics, neutron star masses, and future moment of inertia measurements
- Isovector properties of the Gogny interaction
- Microscopic calculation of the equation of state of nuclear matter and neutron star structure
- Neutron star crusts from mean field models constrained by chiral effective field theory
- Constraints on the maximum mass of neutron stars with a quark core from GW170817 and NICER PSR J0030+0451 data
- Uncertainties in the pasta-phase properties of catalysed neutron stars
- Symmetry energy constraints from GW170817 and laboratory experiments
- The impact of the crust equation of state on the analysis of GW170817
- Nuclear symmetry energy and the r-mode instability of neutron stars
- Sensitivity of the neutron star r-mode instability window to the density dependence of the nuclear symmetry energy
- Influence of the crust on the neutron star macrophysical quantities and universal relations
- Constraints on the phase transition and nuclear symmetry parameters from PSR and multimessenger data of other neutron stars
- General predictions for the neutron star crustal moment of inertia
- The cooling of the Cassiopeia A neutron star as a probe of the nuclear symmetry energy and nuclear pasta
- The nuclear symmetry energy from neutron skins and pure neutron matter in a Bayesian framework
- Resonant Shattering Flares as Multimessenger Probes of the Nuclear Symmetry Energy
- Simultaneous Fitting of Neutron Star Structure and Cooling Data
- Nuclear skin and the curvature of the symmetry energy
- Ramifications of the Nuclear Symmetry Energy for Neutron Stars, Nuclei, and Heavy-Ion Collisions
- Laboratory Probes of the Neutron-Matter Equation of State