Solar wind — a plasma stream flowing out of the solar corona — is interesting both as a carrier of solar activity and as an example of a collisionless plasma. We present the main results of Russian studies in recent years. The original MHD model allows interpreting the bifurcation of the heliospheric current sheet during maximum activity years as occurring due to the quadrupole component of the heliomagnetic field. On a scale of the order of millions of kilometers, the solar wind consists of transient solar formations. On these scales, one of the basic geomagnetic forecast problems has been solved: it was shown that the interplanetary magnetic field can be assumed stable at times of about three hours. At small scales (hundreds to thousands of kilometers), local structures are formed that can be regarded, both individually and statistically, as turbulent cascades.

太阳风——从日冕中流出的等离子体流——作为太阳活动的载体和无碰撞等离子体的一个例子都很有趣。我们介绍近年来俄罗斯研究的主要成果。原始的 MHD 模型允许将日球层电流片在最大活动年期间的分叉解释为由于日磁场的四极分量而发生。在数百万公里的规模上，太阳风由瞬态太阳形成组成。在这些尺度上，基本的地磁预报问题之一已经得到解决：表明行星际磁场可以假设在大约三个小时的时间是稳定的。在小尺度（数百到数千公里）上，形成了可以单独和统计地看待的局部结构，.