Imprints of high-density nuclear symmetry energy on the crustal fraction of neutron star moment of inertia

Abstract

The density dependence of nuclear symmetry energy $E_{\mathrm{sym}}(\rho )$ remains the most uncertain aspect of the equation of state (EOS) of supradense neutron-rich nucleonic matter. Implications of observational crustal fraction of neutron star (NS) moment of inertia $\Delta I/I$ on the $E_{\mathrm{sym}}(\rho )$ are examined in the present work, utilizing an isospin-dependent parameterization of NS EOS. We find that symmetry energy parameters significantly influence the $\Delta I/I$, while the EOS of symmetric nuclear matter has a negligible effect. An increase in the slope $L$ and skewness $J_{\mathrm{sym}}$ of symmetry energy results in a larger $\Delta I/I$, whereas an increase in the curvature $K_{\mathrm{sym}}$ leads to a reduction in $\Delta I/I$. Additionally, we discuss the imprints of observational $\Delta I/I$ on the symmetry energy for NSs with masses of 1.0 M${}_{\odot }$ or 1.4 M${}_{\odot }$. Our results indicate that the $\Delta I/I$ has the potential to set a lower limit of symmetry energy at densities exceeding $3{\rho }_0$, particularly when $L$ is constrained to values less than $60$ MeV, thereby enhancing our understanding of supradense NS matter.

arXiv comment10 pages, 5 figures, published on Particles

References in corpus (63)

• GW170817: Measurements of Neutron Star Radii and Equation of State
• Neutron Star Structure and the Equation of State
• Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar
• Determination of the Equation of State of Dense Matter
• Neutron Star Observations: Prognosis for Equation of State Constraints
• Masses, Radii, and Equation of State of Neutron Stars
• A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
• Equations of state for supernovae and compact stars
• Gravitational-wave constraints on the neutron-star-matter Equation of State
• Refined Mass and Geometric Measurements of the High-Mass PSR J0740+6620
• Constraints on a phenomenologically parameterized neutron-star equation of state
• The Equation of State of Hot, Dense Matter and Neutron Stars
• A study of 315 glitches in the rotation of 102 pulsars
• Measuring the neutron star equation of state using X-ray timing
• Pulsar Constraints on Neutron Star Structure and Equation of State
• Constraining the neutron-proton effective mass splitting using empirical constraints on the density dependence of nuclear symmetry energy around normal density
• Neutron star radii and crusts: uncertainties and unified equations of state
• Nuclear Matter and its Role in Supernovae, Neutron Stars and Compact Object Binary Mergers
• Symmetry Parameter Constraints From A Lower Bound On The Neutron-Matter Energy
• Neutron Stars and the Nuclear Equation of State
• Pulsar glitches: The crust is not enough
• The equation of state for dense nucleonic matter from a metamodeling. I. Foundational aspects
• The Compression-Mode Giant Resonances and Nuclear Incompressibility
• Nuclear constraints on properties of neutron star crusts
• Gravitational waves from neutron star mergers and their relation to the nuclear equation of state
• Core-crust transition in neutron stars: predictivity of density developments
• Neutron conduction in the inner crust of a neutron star in the framework of the band theory of solids
• Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817
• The Radius of the High-mass Pulsar PSR J0740+6620 with 3.6 yr of NICER Data
• The equation of state for dense nucleonic matter from a meta-modeling. II. Predictions for neutron stars properties
• Combined Constraints on the Equation of State of Dense Neutron-Rich Matter from Terrestrial Experiments and Observations of Neutron Stars
• Pulsar Glitches: The Crust may be Enough
• Extracting Nuclear Symmetry Energies at High Densities from Observations of Neutron Stars and Gravitational Waves
• The Radius of PSR J0740+6620 from NICER with NICER Background Estimates
• Locating the inner edge of neutron star crust using terrestrial nuclear laboratory data
• Bayesian Inference of High-density Nuclear Symmetry Energy from Radii of Canonical Neutron Stars
• The nuclear symmetry energy and stability of matter in neutron star
• Phases of dense matter in compact stars
• Sensitivity of the Moment of Inertia of Neutron Stars to the Equation of State of Neutron-Rich Matter
• Bayesian Inference of the Symmetry Energy of Super-Dense Neutron-Rich Matter from Future Radius Measurements of Massive Neutron Stars
• Bayesian analysis of the crust-core transition with a compressible liquid-drop model
• Implications of the mass $M=2.17_{-0.10}^{+0.11}$M${}_{\odot }$ of PSR~J0740+6620 on the Equation of State of Super-Dense Neutron-Rich Nuclear Matter
• Interdependence of different symmetry energy elements
• Why is the nuclear symmetry energy so uncertain at supra-saturation densities?
• Imprints of the nuclear symmetry energy on the tidal deformability of neutron stars
• How tightly is nuclear symmetry energy constrained by unitary Fermi gas?
• The diffusive instability of kaon condensate in neutron star matter
• Constraints on the nuclear symmetry energy from asymmetric-matter calculations with chiral NN and 3N interactions
• Delineating Effects of Nuclear Symmetry Energy on the Radii and Tidal Polarizabilities of Neutron Stars
• Constraints on the skewness coefficient of symmetric nuclear matter within the nonlinear relativistic mean field model
• Impact of NICER's Radius Measurement of PSR J0740+6620 on Nuclear Symmetry Energy at Suprasaturation Densities
• Observational constraints on neutron star crust-core coupling during glitches
• Nuclear fourth-order symmetry energy and its effects on neutron star properties in the relativistic Hartree-Fock theory
• Inference of neutron-star properties with unified crust-core equations of state for parameter estimation
• Efficacy of crustal superfluid neutrons in pulsar glitch models
• Constraints on the muon fraction and density profile in neutron stars
• Exact versus Taylor-expanded energy density in the study of the neutron star crust-core transition
• Impact of Symmetry Energy on Sound Speed and Spinodal Decomposition in Dense Neutron-Rich Matter
• Nuclear incompressibility and sound speed in uniform matter and finite nuclei
• Impact of The Newly Revised Gravitational Redshift of X-ray Burster GS 1826-24 on The Equation of State of Supradense Neutron-Rich Matter
• Effects of the equation of state on the core-crust interface of slowly rotating neutron stars
• The key factor to determine the relation between radius and tidal deformability of neutron stars: slope of symmetry energy
• Neutron star crustal properties from relativistic mean-field models and bulk parameters effects

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