The Latitudinal Structure of Solar Wind Streams from Radio Scintillation Observations

摘要

A comparison of spacecraft and IPS(Interplanetary Scintillations) measurements of the solar wind velocity for 1973-75 are presented, when the large scale velocity structure was very stable. From this comparison we infer a prototype distribution across a high speed stream for the electron density fluctuations, delta n sub e, in the spatial frequency range 1/10,000 - 1/100/km. The 'microturbulence' is mre closely related to the velocity structure in a stream than to the bulk density; enhancements in delta n sub e occur wherever high speed wind overtakes low speed wind. The distribution of delta n sub e is closely matched by the distribution of magnetic field fluctuations approx. 1/1,000,000/km.