General predictions for the neutron star crustal moment of inertia Article Swipe
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· 2019
· Open Access
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· DOI: https://doi.org/10.1103/physrevc.100.055803
· OA: W2894417874
The neutron star crustal EoS and transition point properties are computed\nwithin a unified meta-modeling approach. A Bayesian approach is employed\nincluding two types of filters: bulk nuclear properties are controlled from low\ndensity effective field theory (EFT) predictions as well as the present\nknowledge from nuclear experiments, while the surface energy is adjusted on\nexperimental nuclear masses. Considering these constraints, a quantitative\nprediction of crustal properties can be reached with controlled confidence\nintervals and increased precision with respect to previous calculations:\n{$\\approx 11\\%$} dispersion on the crustal width and {$\\approx 27\\%$}\ndispersion on the fractional moment of inertia. The crust moment of inertia is\nalso evaluated as a function of the neutron star mass, and predictions for mass\nand radii are given for different pulsars. The possible crustal origin of Vela\npulsar glitches is discussed within the present estimations of crustal\nentrainment, disfavoring a large entrainment phenomenon if the Vela mass is\nabove $1.4M_\\odot$. Further refinement of the present predictions requires a\nbetter estimation of the high order isovector empirical parameters, e.g.\n$K_{sym}$ and $Q_{sym}$, and a better control of the surface properties of\nextremely neutron rich nuclei.\n
