Superfluid State in Neutron Star Matter. II : Properties of Anisotropic Energy Gap of ^3P_2 Pairing

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概要

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• By applying the formulation developed in I and using several semiphenomenological twonucleon potentials, properties of the ^<3>P_2 pairing originating from spin-orbit forces are investigated at high density (ρgsim2×10^<14>gcm^<-3>) in neutron star matter. All the possible types of solutions are obtained by solving a coupled integral gap equation through an iterative procedure. Two of these five solutions represent axially symmetric energy gap. By a kind of self-consistency implied in the coupled gap equation the most general solution shows remarkable deviation from axial symmetry as a result of the mixing mainly of mj=±2,0 components but the resulting gap is nodeless. The total energy shifts are very close for all the types of solutions. Although calculations show the largest energy shift for the most general solution, this conclusion is a delicate quantitative one. The ^<3>P_2 gap at high densities depends critically on the effective mass and short-range behavior of nuclear forces, especially on the strong repulsive core of two-nucleon forces. In any case there exists neutron superfluidity due to the ^<3>P_2 pairing at least in the density region ρcong(2〜5)×10^<14>gcm^<-3>. Consequences of the calculated results are discussed, and an argument is given to the connection between the mass of the pulsar and the strong density dependence of neutron superfluidity.

• 理論物理学刊行会の論文
• 1971-07-25

著者

• Tamagaki Ryozo

  Research Institute For Fundamental Physics Kyoto University

• Takatsuka Tatsuyuki

  Department Of Nuclear Engineering Kyoto University

関連論文

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• Chapter II Typical Realization of Alpha-Particle Model Aspects in Beryllium Region
• Chapter I Formation of the Viewpoint, Alpha-Like Four-Body Correlations and Molecular Aspects in Nuclei
• Interaction between Nucleon-Clusters with Full Exchange Effects : An Equivalent Local Potential in a Soluble Model
• Energy Gap in Neutron-Star Matter
• Superfluid State in Neutron Star Matter. II : Properties of Anisotropic Energy Gap of ^3P_2 Pairing
• On the Inner Repulsive Effect Due to the Pauli Principle between Nuclear Composite Particles
• Superfluid State in Neutron Star Matter. III : Tensor Coupling Effect in ^3P_2 Energy Gap

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