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arXiv 0805.1007astro-phgr-qc
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超流中子星核的双流体模型

Two-fluid models of superfluid neutron star cores

N. Chamel

备注：
24 pages, 15 figures, accepted for publication in MNRAS
发表信息：
Mon.Not.Roy.Astron.Soc. 388 (2008) 737-752
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摘要：

利用Brandon Carter等人发展的约束变分方法，建立了中子星核的相对论和非相对论双流体模型.我们考虑零温度下的超流中子和超导质子的混合物，考虑相互夹带效应。影响中子星内部组成并对压力有贡献的轻子也包括在内。我们提供了系统的拉格朗日密度的解析表达式，即所谓的主函数，由此可以得到动力学方程。模型的所有微观参数均采用非相对论核能密度泛函理论计算。为了比较，我们也考虑了相对论平均场模型。在最近发展起来的牛顿多流体流体动力学四维协变形式的框架下，讨论了相对论和非相对论流体动力学模型之间的对应关系。我们已经表明，夹带效应可以解释的动力学有效质量，在相对论的情况下比在牛顿的情况下更大。利用本文所考虑的核模型，我们发现在中子星的液核中，中子的相对论有效质量甚至大于裸中子质量。

英文摘要：

Both relativistic and non-relativistic two-fluid models of neutron star cores are constructed, using the constrained variational formalism developed by Brandon Carter and co-workers. We consider a mixture of superfluid neutrons and superconducting protons at zero temperature, taking into account mutual entrainment effects. Leptons, which affect the interior composition of the neutron star and contribute to the pressure, are also included. We provide the analytic expression of the Lagrangian density of the system, the so-called master function, from which the dynamical equations can be obtained. All the microscopic parameters of the models are calculated consistently using the non-relativistic nuclear energy density functional theory. For comparison, we have also considered relativistic mean field models. The correspondence between relativistic and non-relativistic hydrodynamical models is discussed in the framework of the recently developed 4D covariant formalism of Newtonian multi-fluid hydrodynamics. We have shown that entrainment effects can be interpreted in terms of dynamical effective masses that are larger in the relativistic case than in the Newtonian case. With the nuclear models considered in this work, we have found that the neutron relativistic effective mass is even greater than the bare neutron mass in the liquid core of neutron stars.

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