1988 Volume 60 Issue 6 Pages 406-418
The basic properties of the solar wind and its interaction with the earth's magnetosphere are reviewed in comparison with recent spacecraft observations. It is emphasized that the plasma distribution function of the solar wind is grossly consistent with the idea that the solar wind can be treated macroscopically as a fluid, whereas the existence of high speed streams requires a heat source which is probably due to certain microscopic processes such as dissipations of MHD waves. The observation of solar wind interaction with the earth's magnetosphere suggests that the basic concept of magnetic field reconnection would be correct, but the theories should be modified to accomodate the complexity of the real flow configurations.
