Abstract—The paper studies the magnetic field structures of chemically peculiar magnetic stars. There is a great variety of structures and parameters of magnetic configurations associated with the similar variety of initial conditions in protostellar clouds. It is thought that destruction of a magnetic field does not occur in the non-stationary phase of evolution, and the conditions allow the initial large-scale configurations to be preserved. No matter how tangled a magnetic field in a protostar is, the common vector always corresponds to a poloidal field which is weak relative to local values. By the time a star arrives at the ZAMS, small-scale configurations are destroyed mainly as a result of ohmic dissipation in a time proportional to l², where \(l\) is the characteristic size of the magnetic field inhomogeneity. Due to ohmic dissipation and field-line tension, magnetic configurations become simpler up to the structure of a poloidal field which, with enough approximation, can be described by a magnetic dipole. Owing to high conductivity of the stellar matter, magnetic configurations practically do not change during the entire stay on the Main Sequence; theoretically, due to the enormous size of a star and the high conductivity of plasma, a magnetic field can persist until an age of \({{10}^{{10}}}\)–\({{10}^{{11}}}\) years. The magnetic star rotates solidly.

摘要——本文研究了化学奇异磁星的磁场结构。与原恒星云中类似的各种初始条件相关的磁配置的结构和参数种类繁多。人们认为磁场的破坏不会发生在进化的非静止阶段，并且条件允许保留初始的大规模配置。无论原恒星中的磁场多么纠结，公共矢量总是对应于相对于局部值较弱的极向场。当一颗恒星到达 ZAMS 时，小尺度结构主要由于欧姆耗散在与l ²成正比的时间内被破坏，其中\(l\)是磁场不均匀性的特征尺寸。由于欧姆耗散和磁力线张力，磁配置变得更简单，直到极向场的结构，具有足够的近似值，可以用磁偶极子来描述。由于恒星物质的高导电性，磁性配置在整个停留在主序带期间几乎不会发生变化；理论上，由于恒星的巨大尺寸和等离子体的高导电性，磁场可以持续到\({{10}^{{10}}}\) – \({{10}^{ {11}}}\)年。磁星稳固旋转。