Magnetars are a kind of pulsars powered mainly by superhigh magnetic fields. They are popular sources with many unsolved issues in themselves but are also linked to various high‐energy phenomena, such as quasi periodic oscillations (QPOs), giant flares, fast radio bursts, and superluminous supernovae. In this work, we first review our recent works on the dissipation of toroidal magnetic fields in magnetars and rotationally powered pulsars and then review the spin‐down evolution of young and strongly magnetized pulsars, especially of magnetars. We present an interesting and important relation between the magnetization parameter and magnetic field in the magnetar crust. Finally, we introduce our two works in progress: to explain the magnetar “antiglitch” events in the thermal plastic flow model and to revisit the expression of braking index n, which is independent of the second derivative of spin frequency of a pulsar, and give some proposals for our future work.

中文翻译：

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环形磁场的耗散以及年轻和强磁脉冲星的自旋向下演化

磁星是一种主要由超高磁场驱动的脉冲星。它们是受欢迎的资源，其本身有许多未解决的问题，但也与各种高能现象相关，例如准周期性振荡（QPO），巨大的耀斑，快速的无线电脉冲爆发和超发光的超新星。在这项工作中，我们首先回顾了我们最近关于磁星和旋转动力脉冲星中的环形磁场耗散的工作，然后回顾了年轻的和强磁化的脉冲星，特别是磁星的自旋向下演化。我们提出了磁化壳中磁化参数与磁场之间有趣且重要的关系。最后，我们介绍了我们正在进行的两项工作：解释了热塑性流动模型中的电磁“前倾”事件，并重新探讨了制动指数的表达。n，它独立于脉冲星自旋频率的二阶导数，并为我们的未来工作提出了一些建议。