非正压多流体中子星的磁流体平衡
Hydromagnetic equilibrium in non-barotropic multifluid neutron stars
摘要：
传统上，中子星的磁流体平衡问题是在标准磁流体力学的背景下解决的，物质服从正压状态方程。在本文中，我们采取了一个更现实的处理问题的一步，考虑中子星与内部超流组件。在这个多流体模型分层与不同的物质组成（相对质子中子密度分数）进入作为一种天然成分，导致非正压系统。在将超流/超导中子星的磁流体平衡问题转化为微扰问题之后，我们着重研究了由超流中子和正常质子、电子组成的三流体系统的特殊情况。我们确定了具有混合极面-环面成分的偶极磁场的平衡结构。我们发现，相对于正压模型，分层的通用效果，导致平衡与较高比例的储存在环形分量的磁能。然而，即使在具有强分层的模型中，极向分量和环向分量也是相当的，前者贡献了大部分的磁能。
英文摘要：
Traditionally, the subject of hydromagnetic equilibrium in neutron stars has been addressed in the context of standard magnetohydrodynamics, with matter obeying a barotropic equation of state. In this paper we take a step towards a more realistic treatment of the problem by considering neutron stars with interior superfluid components. In this multifluid model stratification associated with a varying matter composition (the relative proton to neutron density fraction) enters as a natural ingredient, leading to a non-barotropic system. After formulating the hydromagnetic equilibrium of superfluid/superconducting neutron stars as a perturbation problem, we focus on the particular case of a three-fluid system consisting of superfluid neutrons and normal protons and electrons. We determine the equilibrium structure of dipolar magnetic fields with a mixed poloidal-toroidal composition. We find that, with respect to barotropic models, stratification has the generic effect of leading to equilibria with a higher fraction of magnetic energy stored in the toroidal component. However, even in models with strong stratification the poloidal and toroidal components are comparable, with the former contributing the bulk of the magnetic energy.
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