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Neutron star properties with nuclear BHF equations of state

M. Baldo·G. F. Burgio·H. Q. Song·F. Weber
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Abstract

We study the properties of static and rotating neutron stars adopting non-relativistic equations of state (EOS) for asymmetric nuclear matter based on the Brueckner-Hartree-Fock (BHF) scheme. The BHF calculation, with the continuous choice for the single particle potential, appears to be very close to the full EOS, which includes the three-hole line contribution calculated by solving the Bethe-Fadeev equations within the gap choice for the single particle potential. Three-body forces are included in order to reproduce the correct saturation point for nuclear matter. A comparison with fully relativistic many-body calculations of nuclear matter EOS is made.

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M. Baldo, G. F. Burgio, H. Q. Song, F. Weber. 1998-02-18. Neutron star properties with nuclear BHF equations of state. https://arxiv.org/abs/nucl-th/9802055

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