All these equations of state have in common the property of describing a 2 M ⊙ star and of being causal within stable neutron stars. In addition, for relativistic models fifteen equations of state including a transition to hyperonic matter at high density are presented. A large set of unified equations of state for purely nucleonic matter is obtained based on twenty-four Skyrme interactions and nine relativistic mean-field nuclear parametrizations. Necessary conditions for causal and thermodynamically consistent matchings between the core and the crust are formulated and their consequences examined. If the pressure functional is obtained matching a crust and a core equation of state based on models with different properties at nuclear matter saturation, the uncertainties can be as large as ∼ 30 % for the crust thickness and 4% for the radius. We first demonstrate the importance of a unified microscopic description for the different baryonic densities of the star. The uncertainties in neutron star radii and crust properties due to our limited knowledge of the equation of state are quantitatively analyzed.
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