Energy Gap in Neutron-Star Matter

Details Energy Gap in Neutron-Star Matter Energy Gap in Neutron-Star Matter

Nov 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972pthph..48.1517t&link_type=abstract

Progress of Theoretical Physics, Vol. 48, No. 5, pp. 1517-1533

Physics

77

Scientific paper

On exactly taking into account the attractive effect of the ^3P_2 - ^3F_2 coupling due to the two-nucleon tensor force and the effect of the one-body potential, the density region in the neutron-star matter where the ^3P_2-superfluid state exists is determined as ρ ≃ (2 ˜ 8) × 1014 gcm-3. The tensor coupling effect is shown to play an indispensable role on the existence of the ^3P_2-gap in neutron-star matter. The ^1S_0-gap is also investigated, leading to the result that the ^1S_0-superfluid state exists in the density region ρ ≃ (1.0×1011 ˜ 1.5 × 1014) gcm-3. On the basis of these results, the region ρ ≃ (1.5 ˜ 2.0) × 1014 gcm-3 is considered to result in the normal state.

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