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Effective meson masses, effective meson-nucleon couplings and neutron star radii

Kunito Tuchitani·Yasushi Horinouchi·Taihei Iwamitsu·Ken-ichi Makino·Nobuo Noda·Hiroaki Kouno·Akira Hasegawa·Masahiro Nakano
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Abstract

Using the generalized mean field theory, we have studied the relation among the effective meson masses, the effective meson-nucleon couplings and the equation of state (EOS) in asymmetric nuclear matter. If the effective omega-meson mass becomes smaller at high density, the EOS becomes stiffer. However, if we require that the omega-meson mean field is proportional to the baryon density, the effective omega-nucleon coupling automatically becomes smaller at the same time as the effective omega-meson mass becomes smaller. Consequently, the EOS becomes softer. A similar relation is found for the effective rho-meson mass and the effective rho-nucleon coupling. We have also studied the relation among the effective meson masses, the effective meson-nucleon couplings and a radius R of a neutron star. The R depends somewhat on the value of the effective omega-meson mass and the effective omega-nucleon coupling.

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Kunito Tuchitani, Yasushi Horinouchi, Taihei Iwamitsu, Ken-ichi Makino, Nobuo Noda, Hiroaki Kouno, Akira Hasegawa, Masahiro Nakano. 2004-07-01. Effective meson masses, effective meson-nucleon couplings and neutron star radii. https://doi.org/10.1142/s0218301305003673

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