Energy spectrum transfer equations of solar wind turbulence
- Max-Planck-Institut fuer Aeronomie, Katlenburg-Lindau (Germany)
Recent studies of transfer equations for solar wind MHD turbulence are reviewed. Emphasis is placed on the comparison of theoretical with observational results. The Helios, Voyager and Ulysses missions provide opportunities to study the radial evolution of the power spectra, cross-helicity, Alfven ratio and minimum variance direction. Spectrum tranfer equations are a tool to explore theoretically the radial evolution of the fluctuations. The transfer equations are derived from the incompressible MHD equations. Generally, one needs to make assumptions about the nature of the fluctuations and their turbulent interactions, in order to derive models from which numerical results that can be compared with the observations are obtained. Results for special simple models, which involve only structures and assume strong mixing, or consider Alfven waves with weak turbulent interactions, or a superposition of outward Alfven waves with convected structures, are briefly discussed. The differences between various approaches for deriving and approximating the general transfer equations are elucidated. The references in this short review are not complete. An exhaustive list of papers can be found in the recent review of Tu and Marsch [1995a]. A related discussion may be also found in a detailed review by Goldstein et al. [1995a].
- OSTI ID:
- 21163477
- Journal Information:
- AIP Conference Proceedings, Vol. 382, Issue 1; Conference: 8. international solar wind conference: Solar wind eight, Dana Point, CA (United States), 25-30 Jun 1995; Other Information: DOI: 10.1063/1.51390; (c) 1996 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
- Country of Publication:
- United States
- Language:
- English
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