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| Main Authors: | , |
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| Format: | Preprint |
| Published: |
2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2411.06238 |
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Table of Contents:
- The density dependence of nuclear symmetry energy $E_{\rm sym}(ρ)$ 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 $ΔI/I$ on the $E_{\rm sym}(ρ)$ are examined in the present work, utilizing an isospin-dependent parameterization of NS EOS. We find that symmetry energy parameters significantly influence the $ΔI/I$, while the EOS of symmetric nuclear matter has a negligible effect. An increase in the slope $L$ and skewness $J_{\rm sym}$ of symmetry energy results in a larger $ΔI/I$, whereas an increase in the curvature $K_{\rm sym}$ leads to a reduction in $ΔI/I$. Additionally, we discuss the imprints of observational $ΔI/I$ on the symmetry energy for NSs with masses of 1.0 M$_\odot$ or 1.4 M$_\odot$. Our results indicate that the $ΔI/I$ has the potential to set a lower limit of symmetry energy at densities exceeding $3ρ_0$, particularly when $L$ is constrained to values less than $60$ MeV, thereby enhancing our understanding of supradense NS matter.