中子星中互连的中子涡旋和质子通量管阵列的稳定性：平衡位形
Stability of interlinked neutron vortex and proton flux tube arrays in a neutron star: equilibrium configurations
摘要：
本文采用Gross-Pitaevskii方程（GPE）对旋转谐波阱中中子超流涡旋与质子超导通量管之间的相互作用进行了三维数值模拟，描述了中子星外核的理想模型。低能态的中子凝聚体的计算通过在虚时间中的规定的，静态的，直线通量管阵列的存在下发展的GPE。的计算进行作为一个功能的全球磁和旋转轴之间的角度，和中子和质子凝聚体之间的电流和密度耦合的振幅和符号。结果表明，系统在涡-涡排斥和涡-通量管吸引（钉扎）的作用下，会出现涡旋缠结和"玻璃态"行为，表现为多个亚稳态在能量上的紧密分布.模拟中的无量纲参数按照人们对中子星的预期进行排序，但动态范围比实际小很多个数量级，因此在评估天体物理意义时必须谨慎。然而，结果表明，纠缠涡可能是地方性的中子星外核。
英文摘要：
Three-dimensional, Gross-Pitaevskii equation (GPE) simulations are presented of the interaction between neutron superfluid vortices and proton superconductor flux tubes in a rotating, harmonic trap, representing an idealised model of the outer core of a neutron star. Low-energy states of the neutron condensate are calculated by evolving the GPE in imaginary time in the presence of a prescribed, static, rectilinear flux tube array. The calculations are carried out as a function of the angle between the global magnetic and rotation axes, and the amplitude and sign of the current-current and density couplings between the neutron and proton condensates. It is found that the system is frustrated by the competition between vortex-vortex repulsion and vortex-flux-tube attraction (pinning), leading to the formation of vortex tangles and "glassy" behaviour characterized by multiple metastable states spaced closely in energy. The dimensionless parameters in the simulations are ordered as one expects in a neutron star, but the dynamic range is many orders of magnitude smaller than in reality, so caution must be exercised when assessing the astrophysical implications. Nevertheless the results suggest that tangled vorticity may be endemic in neutron star outer cores.
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