The heliospheric magnetic field (HMF) is the extension of the coronal magnetic field carried out into the solar system by the solar wind. It is the means by which the Sun interacts with planetary magnetospheres and channels charged particles propagating through the heliosphere. As the HMF remains rooted at the solar photosphere as the Sun rotates, the large-scale HMF traces out an Archimedean spiral. This pattern is distorted by the interaction of fast and slow solar wind streams, as well as the interplanetary manifestations of transient solar eruptions called coronal mass ejections. On the smaller scale, the HMF exhibits an array of waves, discontinuities, and turbulence, which give hints to the solar wind formation process. This review aims to summarise observations and theory of the small- and large-scale structure of the HMF. Solar-cycle and cycle-to-cycle evolution of the HMF is discussed in terms of recent spacecraft observations and pre-spaceage proxies for the HMF in geomagnetic and galactic cosmic ray records.

中文翻译：

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日球磁场

日球磁场（HMF）是太阳风将日冕磁场扩展到太阳系中的作用。它是太阳与行星磁层相互作用并通过带电粒子传播通过日球层的通道。随着HMF在太阳旋转时仍植根于太阳光层，大型HMF会追踪出阿基米德螺旋线。快速和慢速太阳风的相互作用以及被称为日冕物质抛射的瞬态太阳喷发的星际表现都使这种模式扭曲了。在较小的规模上，HMF表现出一系列的波，不连续性和湍流，这为太阳风的形成过程提供了提示。这篇综述旨在总结HMF规模结构的观察和理论。