The crust of neutron stars
نویسنده
چکیده
The structure of the crust of a neutron star is completely determined by the experimentally measured nuclear masses up to a density of the order of 1011 g.cm−3. At higher densities, the composition of the crust still remains uncertain, mainly due to the presence of “free” superfluid neutrons which affect the properties of the nuclear “clusters”. After briefly reviewing calculations of the equilibrium structure of the crust, we point out that the current approach based on the WignerSeitz approximation does not properly describe the unbound neutrons. We have recently abandoned this approximation by applying the band theory of solids. We have shown that the dynamical properties of the free neutrons are strongly affected by the clusters by performing 3D calculations with Bloch boundary conditions.
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