Abstract—

The results of three-dimensional numerical simulation of heat transfer in the outer layers of magnetized neutron stars are presented. Determining the structure of the magnetic field on a neutron star surface is an important task of modern astrophysics. In the presence of strong magnetic fields, the medium becomes anisotropic, and the laws of heat conduction change. The tensor coefficient of thermal conductivity for magnetized degenerate plasma was obtained by Bisnovatyi-Kogan and Glushikhina by solving the Boltzmann equation with the Chapman–Enskog method. In this paper, the temperature distribution on the surface of a magnetized neutron star is obtained for magnetic fields of the dipolar and quadrupolar type, as well as for their superposition. To numerically solve the stationary temperature distribution problem in the outer layers of a magnetized neutron star, the basic (support) operator numerical method was extended to a three-dimensional case. The problem was solved on the grid which consists of tetrahedra.

中文翻译：

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磁化中子星外层各向异性传热的3D模拟

摘要—

给出了磁化中子星外层传热的三维数值模拟结果。确定中子星表面的磁场结构是现代天体物理学的重要任务。在强磁场的作用下，介质变为各向异性，并且热传导定律发生变化。Bisnovatyi-Kogan和Glushikhina通过用Chapman-Enskog方法求解玻尔兹曼方程，获得了磁化简并等离子体的热导张量系数。在本文中，针对偶极和四极类型的磁场以及它们的叠加，获得了磁化中子星表面的温度分布。为了从数值上解决磁化中子星外层的稳态温度分布问题，将基本（支持）算子数值方法扩展到了三维情况。在由四面体组成的网格上解决了该问题。