磁星的磁场分布
Magnetic field distribution in magnetars
摘要：
利用轴对称数值程序，我们对非旋转中子星的磁场结构进行了广泛的研究，改变了质量、磁场强度和状态方程。我们发现，单极（球对称）的规范的磁场的一部分，可以描述为一个单一的配置文件，我们适合一个简单的八阶多项式，作为一个函数的恒星的半径。这个新的一般轮廓非常适用于所有的磁化中子星的强子状态方程的配置。然后，我们应用此配置文件，以建立磁化中子星的球对称性，使用修改后的托尔曼-奥本海默-沃尔科夫（TOV）方程组。这种新的形式主义产生的质量-半径图方面稍好的结果比以前的尝试，以增加磁条款，这些方程。然而，我们表明，这种方法是不准确的比通常的，非磁化TOV模型，一致的模型必须离开球对称。因此，我们的“通用”磁场分布图旨在作为核物理学家的一种工具，以获得中子星内部磁场的估计，作为径向深度的函数，以推断其对组成和相关性质的影响。它具有的优点是基于磁场分布从现实的自洽计算，这是麦克斯韦方程组的解决方案。
英文摘要：
Using an axisymmetric numerical code, we perform an extensive study of the magnetic field configurations in non-rotating 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, that 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-Volkov (TOV) 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 usual, non-magnetized 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 magnetic field inside neutron stars, as a function of radial depth, in order 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.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
