Abstract
The major progress made in recent years in the study of solar wind turbulence may be summarized as follows: 1) The evolution of the solar wind fluctuations with heliocentric distance has been established. 2) The wave description and the turbulence description have been combined together to develop a uniform picture and phenomenological theory for a turbulent magnetofluid. 3) The existence of inward propagating fluctuations and their resulting nonlinear interactions and of a cascade process in the Alfvenic fluctuations has been widely accepted. 4) Blsasser variables has been introduced to the data analysis. By their means the morphology of the spectra e± and eR in the inner solar system has been clearly established. This progress has been briefly reviewed in this paper.
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