Microscopic nuclear equation of state with three-body forces and neutron star structure

Details Microscopic nuclear equation of state with three-body forces and neutron star structure Microscopic nuclear equation of state with three-body forces and neutron star structure

Apr 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..704..473l&link_type=abstract

TOURS SYMPOSIUM ON NUCLEAR PHYSICS V; Tours 2003. AIP Conference Proceedings, Volume 704, pp. 473-482 (2004).

Physics

Nuclear Physics

Nuclear Matter, Nuclear Matter Aspects Of Neutron Stars, Neutron Stars

Scientific paper

The equation of state (EOS) of nuclear matter is discussed within the Brueckner-Bethe-Goldstone approach. First the energy per particle E/A is calculated in the Brueckner-Hartree-Fock limit with the Argonne v18 potential, using the continuous choice as auxiliary potential. Then, the contribution of three-body clusters is determined by solving the Bethe-Faddeev equation, and the equivalence with the same calculations based on the standard choice as auxiliary potential, is demonstrated. In spite of reaching a quite good convergence of the hole-line expansion, the resulting EOS does not fit the empirical saturation density (ρ0 = 0.17 fm-3). To this end, three-body forces (TBF) are introduced. A first class of microscopic TBF comprises effects due to NN virtual excitations via σ and ω-meson exchanges (the main relativistic correction to Brueckner theory), the 2π-exchange, and the virtual excitation of the lowest nucleonic resonance N*(1440). We compare with a phenomenological TBF, involving two parameters adjusted on the saturation density and energy. Next, using microscopic or phenomenological TBF, the symmetry energy of nuclear matter is computed, allowing to determine the EOS of beta-stable and charge neutral matter, and the properties of neutron stars, in particular the mass-radius curve.

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