Dynamo magnetic fields are primarily generated by thermochemical convection of electrically conductive liquid metal within planetary cores. Convection can be sustained by secular cooling and may be bolstered by compositional buoyancy associated with core solidification. Additionally, mechanical stirring of core fluids and external perturbations by large impact events, tidal effects, and orbital precession can also contribute to sustaining dynamo fields. Convective dynamos cease when the core-mantle heat flux becomes subadiabatic or if specific crystallization regimes inhibit core fluid flows. Therefore, exploring the histories of magnetic fields across the Solar System provides a window into the thermal and chemical evolution of planetary interiors. Here we review how recent spacecraft-based studies of remanent crustal magnetism, paleomagnetic studies of rock samples, and planetary interior models have revealed the magnetic and evolutionary histories of Mercury, Earth, Mars, the Moon, and several planetesimals, as well as discuss avenues for future exploration and discovery.

发电机磁场主要由行星核心内导电液态金属的热化学对流产生。对流可以通过长期冷却来维持，并且可以通过与核心凝固相关的成分浮力来支持。此外，大撞击事件、潮汐效应和轨道进动对核心流体的机械搅拌和外部扰动也有助于维持发电机场。当核幔热通量变为亚绝热或特定的结晶状态抑制核流体流动时，对流发电机停止。因此，探索整个太阳系的磁场历史为了解行星内部的热和化学演化提供了一个窗口。在这里，我们回顾了最近基于航天器的地壳剩磁研究，