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From the crust to the core of neutron stars on a microscopic basis

  • Elementary Particles and Fields
  • Theory
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Abstract

Within a microscopic approach the structure of Neutron Stars is usually studied by modelling the homogeneous nuclear matter of the core by a suitable Equation of State, based on a many-body theory, and the crust by a functional based on a more phenomenological approach. We present the first calculation of Neutron Star overall structure by adopting for the core an Equation of State derived from the Brueckner-Hartree-Fock theory and for the crust, including the pasta phase, an Energy Density Functional based on the same Equation of State, and which is able to describe accurately the binding energy of nuclei throughout the mass table. Comparison with other approaches is discussed. The relevance of the crust Equation of State for the Neutron Star radius is particularly emphasised.

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Authors and Affiliations

  1. INFN Sezione di Catania, and Dipartimento di Fisica e Astronomia, Università di Catania, Catania, Italy

    M. Baldo & G. F. Burgio

  2. Departament d’Estructura i Constituentes de la Matèria and Institut de Ciències del Cosmos, Facultat de Física, Universitat de Barcelona, Barcelona, Spain

    M. Centelles, B. K. Sharma & X. Viñas

Authors
  1. M. Baldo
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  2. G. F. Burgio
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  3. M. Centelles
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  4. B. K. Sharma
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  5. X. Viñas
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Correspondence to M. Baldo.

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The text was submitted by the authors in English.

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Baldo, M., Burgio, G.F., Centelles, M. et al. From the crust to the core of neutron stars on a microscopic basis. Phys. Atom. Nuclei 77, 1157–1165 (2014). https://doi.org/10.1134/S1063778814080031

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  • DOI: https://doi.org/10.1134/S1063778814080031

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