From neutron skins and neutron matter to the neutron star crust by William G. Newton, Rebecca Preston, Lauren Balliet, Michael Ross

“…Using a compressible liquid drop model with an extended Skyrme energy-density functional, we obtain the most stringent constraints to date on the transition pressure Pcc=0.33−0.07+0.07 MeV fm−3 and chemical potential μcc=12.6−1.9+1,8 MeV (which control the mass, moment of inertia and thickness of a neutron star crust), the proton fractions that bracket the pasta phases yp=0.115−0.017+0.016 and ycc=0.041−0.006+0.007, as well as the relative mass and moment of inertia ΔMp/ΔMc≈ΔIp/ΔIc=0.54−0.09+0.05 and thickness ΔRp/ΔRc=0.129−0.030+0.019 of the layers of non-spherical nuclei (nuclear pasta) in the crust.…”
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