Energy spectrum transfer equations of solar wind turbulence

Details Energy spectrum transfer equations of solar wind turbulence Energy spectrum transfer equations of solar wind turbulence

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..233t&link_type=abstract

Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 233

Computer Science

1

Particle Emission, Solar Wind, Interplanetary Magnetic Fields, Plasma Turbulence, Magnetohydrodynamic Waves

Scientific paper

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, Alfvén 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 Alfvén waves with weak turbulent interactions, or a superposition of outward Alfvén 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].

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