Energy Gap in Neutron-Star Matter

概要

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On exactly taking into account the attractive effect of the ^<3>P_2-^<3>F_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 ^<3>P_2- superfluid state exists is determined as ρsime(2~8)×10^<14>gcm^<-3> . The tensor coupling effect is shown to play an indispensable role on the existence of the ^<3>P_2-gap in neutron-star matter. The ^<1>S_0-gap is also investigated, leading to the result that the ^<1>S_0-superfluid state exists in the density region ρsime(1.0×10^<11>~1.5×10^<14>)gcm^<-3>. On the basis of these results, the region ρsime(1.5~2.0)×10^<14>gcm^<-3> is considered to result in the normal state.
理論物理学刊行会の論文
1972-11-25