The effect of the energy functional on the pasta-phase properties of catalysed neutron stars
arXiv:2111.04374 · doi:10.1140/epja/s10050-021-00605-6
Abstract
Nuclear pasta, that is an inhomogeneous distribution of nuclear matter characterised by non-spherical clustered structures, is expected to occur in a narrow spatial region at the bottom of the inner crust of neutron stars, but the width of the pasta layer is strongly model dependent. In the framework of a compressible liquid-drop model, we use Bayesian inference to analyse the constraints on the sub-saturation energy functional and surface tension imposed by both ab-initio chiral perturbation theory calculations and experimental measurements of nuclear masses. The posterior models are used to obtain general predictions for the crust-pasta and pasta-core transition with controlled uncertainties. A correlation study allows extracting the most influential parameters for the calculation of the pasta phases. The important role of high-order empirical parameters and the surface tension is underlined.
15 pages, 11 figures. Contribution to the EPJ A topical issue "CompOSE: a repository for Neutron Star Equations of State and Transport Properties"
References in corpus (14)
- Core-crust transition in neutron stars: predictivity of density developments
- Disordered nuclear pasta, magnetic field decay, and crust cooling in neutron stars
- Incompressibility of neutron-rich matter
- Probing the Equation of State of Nuclear Matter via Neutron Star Asteroseismology
- Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. II. Pasta phases in semi-classical approximation
- Uncertainties in the pasta-phase properties of catalysed neutron stars
- Crystallization of the inner crust of a neutron star and the influence of shell effects
- Liquid-gas coexistence vs. energy minimization with respect to the density profile in the inhomogeneous inner crust of neutron stars
- Fast neutrino cooling of nuclear pasta in neutron stars: molecular dynamics simulations
- Systematic analysis of inner crust composition using the extended Thomas-Fermi approximation with pairing correlations
- Nuclear pasta and symmetry energy in the relativistic point-coupling model
- Neutron star inner crust: effects of rotation and magnetic fields
- Parametrization of the surface energy in the ETF approximation
- The equation of state of neutron stars and the role of nuclear experiments
Cited by in corpus (16)
- Nucleonic metamodelling in light of multimessenger, PREX-II and CREX data
- Inference of neutron-star properties with unified crust-core equations of state for parameter estimation
- Detectability of a phase transition in neutron star matter with third-generation gravitational wave interferometers
- Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. IV. Role of the symmetry energy in pasta phases
- Quark-hadron pasta phase in neutron stars: the role of medium-dependent surface and curvature tensions
- The proto-neutron star inner crust in the liquid phase
- Anisotropic electron transport in the nuclear pasta phase
- Strong magnetic fields and pasta phases revisited
- Crust (Unified) Tool for Equation-of-state Reconstruction (CUTER) v2
- Light clusters in the liquid proto-neutron star inner crust
- Stability of spherical nuclei in the inner crust of neutron stars
- Bayesian inference of neutron star crust properties using an ab initio-benchmarked meta-model
- Elasticity of neutron star mantle: improved compressible liquid drop model for cylindrical phases
- Nuclear physics inputs for dense-matter modelling in neutron stars. The nuclear equation of state
- Light clusters as a possible source of crustal impurities: a quasi-particle approach
- The nuclear matter density functional under the nucleonic hypothesis