Young and rotation-powered neutron stars (NSs) are commonly observed as rapidly-spinning pulsars. They dissipate their rotational energy by emitting pulsar wind with electromagnetic radiation and spin down at a steady rate, according to the simple steadily-rotating magnetic dipole model. In reality, however, multiwavelength observations of radiation from the NS surface and magnetosphere have revealed that the evolution and properties of NSs are highly diverse, often dubbed as 'NS zoo'. In particular, many of young and highly magnetized NSs show a high degree of activities, such as sporadic electromagnetic outbursts and irregular changes in pulse arrival times. Importantly, their magnetic field, which are the strongest in the universe, makes them ideal laboratories for fundamental physics. A class of highly-magnetized isolated NSs is empirically divided into several subclasses. In a broad classification, they are, in the order of the magnetic field strength (B) from the highest, 'magnetars' (historically recognized as soft gamma-ray repeaters and/or anomalous x-ray pulsars), 'high-B pulsars', and (nearby) x-ray isolated NSs. This article presents an introductory review for non-astrophysicists about the observational properties of highly-magnetized NSs, and their implications. The observed dynamic nature of NSs must be interpreted in conjunction with transient magnetic activities triggered during magnetic-energy dissipation process. In particular, we focus on how the five fundamental quantities of NSs, i.e. mass, radius, spin period, surface temperature, and magnetic fields, as observed with modern instruments, change with evolution of, and vary depending on the class of, the NSs. They are the foundation for a future unified theory of NSs.

中文翻译：

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磁化中子星的观测多样性

年轻的自转中子星 (NSs) 通常被观察为快速旋转的脉冲星。根据简单的稳定旋转磁偶极子模型，它们通过发射带有电磁辐射的脉冲星风来耗散旋转能量，并以稳定的速率自旋。然而，实际上，对来自 NS 表面和磁层的辐射的多波长观测表明，NS 的演化和特性是高度多样化的，通常被称为“NS 动物园”。特别是，许多年轻且高度磁化的 NS 表现出高度的活动，例如零星的电磁爆发和脉冲到达时间的不规则变化。重要的是，它们的磁场是宇宙中最强的，使它们成为基础物理学的理想实验室。一类高度磁化的孤立 NS 根据经验分为几个子类。在广义的分类中，按照磁场强度 (B) 从最高的顺序，它们是“磁星”（历史上被认为是软伽马射线中继器和/或异常 X 射线脉冲星）、“高 B 脉冲星” '，和（附近）X 射线隔离的 NS。本文为非天体物理学家介绍了关于高磁化 NS 的观测特性及其影响的介绍性评论。观察到的 NS 的动态性质必须结合磁能耗散过程中触发的瞬态磁活动来解释。我们特别关注现代仪器观察到的 NS 的五个基本量，即质量、半径、自旋周期、表面温度和磁场，随 NS 的演变而变化，并因 NS 的类别而异。它们是未来 NS 统一理论的基础。