论文标题
中子星形地壳中的磁场演变：超越大厅效应
Magnetic Field Evolution in Neutron Star Crusts: Beyond the Hall Effect
论文作者
论文摘要
中子星是我们在宇宙中知道的最强磁场。它们的磁场是产生辐射的主要手段，无论是磁层还是通过地壳。此外，磁场的演变与磁场的爆炸性事件密切相关，后者的磁场及其持续的热发射。在霍尔效应和欧姆耗散的框架内，已经描述了中子恒星地壳中磁场的演变。然而，这种描述受到以下事实的限制：麦克斯韦在强磁性中子星的地壳上施加的麦克斯韦应力可能导致衰竭和温度变化。在前一种情况下，失败的外壳不能完全满足大厅效应的必要条件。在后者中，温度的变化与磁场演化密切相关。最后，恒星温度的尖锐梯度可能会激活电池项并改变磁场结构，尤其是在弱磁性的中子恒星中。在这篇评论中，我们讨论了这些影响的最新进展。我们认为，这些现象可能会为我们对中子恒星及其可观察的特性的理解提供新的见解。
Neutron stars host the strongest magnetic fields that we know of in the Universe. Their magnetic fields are the main means of generating their radiation, either magnetospheric or through the crust. Moreover, the evolution of the magnetic field has been intimately related to explosive events of magnetars, which host strong magnetic fields, and their persistent thermal emission. The evolution of the magnetic field in the crusts of neutron stars has been described within the framework of the Hall effect and Ohmic dissipation. Yet, this description is limited by the fact that the Maxwell stresses exerted on the crusts of strongly magnetised neutron stars may lead to failure and temperature variations. In the former case, a failed crust does not completely fulfil the necessary conditions for the Hall effect. In the latter, the variations of temperature are strongly related to the magnetic field evolution. Finally, sharp gradients of the star's temperature may activate battery terms and alter the magnetic field structure, especially in weakly magnetised neutron stars. In this review, we discuss the recent progress made on these effects. We argue that these phenomena are likely to provide novel insight into our understanding of neutron stars and their observable properties.
