TY - GEN
T1 - Microscopic nuclear equation of state with three-body forces and neutron star structure
AU - Lombardo, U.
AU - Burgio, G. F.
AU - Schulze, H. J.
AU - Zuo, W.
AU - Zhou, X. R.
N1 - Publisher Copyright:
© 2004 American Institute of Physics.
PY - 2004/4/12
Y1 - 2004/4/12
N2 - 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.
AB - 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.
UR - https://www.scopus.com/pages/publications/85052112955
U2 - 10.1063/1.1737143
DO - 10.1063/1.1737143
M3 - 会议稿件
AN - SCOPUS:85052112955
SN - 0735401772
T3 - AIP Conference Proceedings
SP - 473
EP - 482
BT - Tours Symposium on Nuclear Physics V; Tours 2003
A2 - Wada, T.
A2 - Munzenberg, G.
A2 - Arnould, M.
A2 - Ohta, M.
A2 - Yamagata, T.
A2 - Lewitowicz, M.
A2 - Utsunomiya, H.
A2 - Akimune, H.
PB - American Institute of Physics Inc.
T2 - Tours Symposium on Nuclear Physics V; Tours 2003
Y2 - 26 August 2003 through 29 August 2003
ER -