Abstract
Abstract On the basis of selective measurements of proton and α-particle bulk parameters and magnetic field on board the Prognoz 7 satellite the structure of the solar wind is studied and is compared with a possible structure of the solar corona. For that purpose the magnetic field value, proton temperature, ratio of thermal and magnetic pressures and relative helium abundance are represented as distributions on the n - V p (density - proton velocity) plane. Values and different behaviour of these parameters on this plane allow to identify 5 types of the solar wind streams which may be connected with the solar corona structure: (1) the heliospheric current sheets, (2) streams from closed coronal magnetic field regions (streamers), (3) streams from open magnetic field regions (coronal holes), (4) disturbed solar wind streams at large angles relative to the solar meridians of non-stationary events in the corona, and (5) disturbed streams at small angles relative to meridians of non-stationary events including coronal mass ejection matter.
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