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Title: The crust of neutron stars

Abstract

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 Wigner-Seitz 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.

Authors:
 [1]
  1. Institut d'Astronomie et d'Astrophysique, Universite Libre de Bruxelles, CP226, Boulevard du Triomphe, 1050 Brussels (Belgium)
Publication Date:
OSTI Identifier:
21056765
Resource Type:
Journal Article
Resource Relation:
Journal Name: AIP Conference Proceedings; Journal Volume: 891; Journal Issue: 1; Conference: 6. Symposium on nuclear physics, Tours (France), 5-8 Sep 2006; Other Information: DOI: 10.1063/1.2713540; (c) 2007 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
73 NUCLEAR PHYSICS AND RADIATION PHYSICS; APPROXIMATIONS; BAND THEORY; BOUNDARY CONDITIONS; CLUSTER MODEL; DENSITY; EQUILIBRIUM; MASS; NEUTRON STARS; NEUTRONS; NUCLEAR MATTER; SUPERFLUIDITY; THREE-DIMENSIONAL CALCULATIONS

Citation Formats

Chamel, N. The crust of neutron stars. United States: N. p., 2007. Web. doi:10.1063/1.2713540.
Chamel, N. The crust of neutron stars. United States. doi:10.1063/1.2713540.
Chamel, N. Mon . "The crust of neutron stars". United States. doi:10.1063/1.2713540.
@article{osti_21056765,
title = {The crust of neutron stars},
author = {Chamel, N.},
abstractNote = {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 Wigner-Seitz 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.},
doi = {10.1063/1.2713540},
journal = {AIP Conference Proceedings},
number = 1,
volume = 891,
place = {United States},
year = {Mon Feb 26 00:00:00 EST 2007},
month = {Mon Feb 26 00:00:00 EST 2007}
}
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