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Magnetic field distribution in magnetars

机译：磁场磁场分布

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Using an axisymmetric numerical code, we perform an extensive study of the magnetic-field configurations in nonrotating neutron stars, varying the mass, magnetic-field strength and the equation of state. We find that the monopolar (spherically symmetric) part of the norm of the magnetic field can be described by a single profile, which we fit by a simple eighth-order polynomial, as a function of the star's radius. This new generic profile applies remarkably well to all magnetized neutron star configurations built on hadronic equations of state. We then apply this profile to build magnetized neutron stars in spherical symmetry, using a modified Tolman-Oppenheimer-Volkoff system of equations. This new formalism produces slightly better results in terms of mass-radius diagrams than previous attempts to add magnetic terms to these equations. However, we show that such approaches are less accurate than the usual, nonmagnetized TOV models, and that consistent models must depart from spherical symmetry. Thus, our "universal" magnetic-field profile is intended to serve as a tool for nuclear physicists to obtain estimates of the magnetic field inside neutron stars as a function of radial depth to deduce its influence on composition and related properties. It possesses the advantage of being based on magnetic-field distributions from realistic self-consistent computations which are solutions of Maxwell's equations.
机译：使用轴对称数值代码，我们对非调节中子恒星中的磁场配置进行了广泛的研究，改变了质量，磁场强度和状态方程。我们发现磁场的标准的单极（球面对称）部分可以由单个轮廓描述，我们通过简单的八阶多项式适合作为星形半径的函数。这种新的通用配置文件非常良好地适用于基于状态的Hadronic方程的所有磁化中子星形配置。然后，我们使用修改的Tolman-Oppenheimer-Volkoff系统来应用此配置文件以在球面对称中构建磁化中子恒星，使用改进的Tolman-Oppenheimer-Volkoff系统。这种新的形式主义在质量半径图方面产生稍微更好的结果，而不是之前尝试向这些方程添加磁性术语。但是，我们表明这种方法比通常的非磁化到D型号的准确性不太准确，并且一致的模型必须脱离球面对称性。因此，我们的“通用”磁场轮廓旨在用作核物理学家的工具，以获得中子恒星内的磁场的估计，作为径向深度，以推导其对组合物和相关性能的影响。它具有基于来自麦克斯韦方程的解决方案的现实自我一致计算的磁场分布的优点。

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