Received date: 2002-08-07
Revised date: 2002-09-12
Online published: 2002-12-01
The solar wind turbulence was found in the early days of spacecraft observations. Although many international scientists studied on this topic for many years, the nature of the solar wind turbulence had not yet been discovered till the middle of 1980s. The solar wind turbulence is different from the fluid turbulence. Many observations could not be explained by the previous theory. Tu Chuanyi et al［1~5］pointed out that non-linear turbulent interactions exist in the solar wind fluctuations. However the solar wind turbulence is not a developed turbulence. It is in a state of transition from Alfven waves to developed turbulence. This new idea combined the Alfven wave propagation theory with the turbulence transfer theory and led to a few theoretical development, which discovered the nature of the solar wind turbulence and explain several important observations.
Key words： Solar wind; MHD; Solar wind turbulence.
TU Chuan-yi . THE NATURE OF SOLAR WIND TURBULENCE[J]. Advances in Earth Science, 2002 , 17(6) : 806 -810 . DOI: 10.11867/j.issn.1001-8166.2002.06.0806
［1］Tu C Y, Pu Z Y, Wei F S. The Power spectrum of interplanetary Alfvenic fluctuations: Derivation of the governing equation and its Solution［J］.Journal of Geophysical Research，1984, 89：9 695-9 702.
［2］Tu C Y. The damping of interplanetary Alvenic fluctuations and the heation of the solar wind［J］. Journal of Geophysical Research, 1988, 93：7-20.
［3］Tu Chuanyi, Marsch E. MHD structures, waves and turbulence in the solar wind: observations and theories［J］. Space Science Review, 1995, 73：1-210.
［4］Tu Chnanyi, Marsch E. MHD Structures, Waves and Turbulence in the Solar Wind Observations and Theories［M］. Dordrecht, The Netherlands: Kluwer Academic Publisher, 1995.
［5］Tu Chuauyi, Marsch E, Rosenbauer H. An extended structure-function model and its application to the analysis of solar wind intermittency properties［J］. Annales Geophysicae, 1996,14: 270-285.
［6］ Kraichnan R H. Inertial-range spectrum of hydromagnetic turbulence ［J］. Physical of Fluids, 1965, 8:1 385.
［7］ Coleman P J Jr. Turbulence, viscosity and dissipation in the solarwind plasma［J］. Astrophysical Journal, 1968, 153:371.
［8］ Belcher J W, L Davis Jr. Large-amplitude［J］. Journal of Geophysical Research, 1971, 76:3 534.
［9］ Dobrowolny M, Mangeney A, Veltri P. Fully developed anisotropic turbulence in interplanetary space ［J］. Physical Research Letters, 1980, 45:144.
［10］Bavassano B, Dobrowolny M, Mariani F, et al.Radial evolution of power spectra of interplanetary Alfvenic turbulence［J］.Journal of Geophysical Research, 1982, 87:3 617.
［11］Matthaeus W H, Zhou Y. Turbulence and Nonlinear Dynamics in MHD Flows［M］. North-Holland: Elser Science Publishers, 1989.
［12］Matthaeus W H, Zhou Y, Oughton S, et al. Solar WindSeven［A］. In: Marsch E, Schwenn R, et al, eds. Proceedings of 3rd COSPAR Colloquium Held in Goslar［C］.Germany: Pergaman Press, 1992. 511-516.
［13］Bruno R Bavassano B. Origin of low cross-helicity regions in the inner solar wind［J］. Journal of Geophysical Research, 1991, 96:7 841-7 851.
［14］Zhou Ye, Mattheaus W H. Non-WKB evolution of solar wind fluctuations: a turbulence modeling approach［J］. Geophysical Research Letter, 1989, 16: 755-758.
［15］Grappin R, Mangeney A. Can we understand Alfvenicturbulence via simulation of the MHD equations?［A］. In: Winterhalter D, et al, eds. Solar Wind Eight AIP Conference Proceedings［C］. 1996, 382: 252-255.
［16］Goldstein M, Roberts D A. Magnetohydrodynamic turbulence in the solar wind［J］. Annual Review of Astronomy and Astrophysics, 1995, 33: 283-325.
［17］Feynman J ，Ruzmaikin A A, Smith E J. Radial evolution of thehigh/low frequency breakpoint in magnetic field spectra［A］. In: Winterhalter D, et al,eds. Solar Wind Eight AIP Conference Proceedings［C］. 1996, 382: 347-350.
［18］Schwartz S J,Feldman W C, Gary S P. The source of proton anisotropy in the high-speed solar wind［J］. Journal of Geophysical Research, 1981,86: 541.
［19］Marsch E. MHD turbulence in the solar wind［A］. In: Schwenn R, Marsch E, eds. Physics of Inner Heliosphere II［C］. Berlin: Springer-Verlag, 1991. 152-241.
［20］Feldman W C, Marsch E. Kinetic phenomena in the solar wind［A］. In: Jokippit J R, Sonett C P, Giampapa M S, eds［A］. Cosmic Winds and the Heliosphere［C］. Tucson: University of Arizona Press, 1997. 617-675.
［21］Hu Y-Q, Habbal S R. Resonant acceleration and heating of solarwind ions by dispersive ion cyclotron waves［J］. Journal of Geophysical Research, 1999, 104: 17 045-17 056.
［22］Mangeney A, Grappin R Velli M. MHD turbulence in the solar wind［A］. In: Priest E R, Hood A W, eds. Advances in Solar System Magnetohydro-Dynamics［C］. Cambridge: Cambridge University Press, 1991.327-336.
［23］Marsch F. Satructure functions and intermittency of velocity fluctuations in the inner solar wind［J］.Annual Geophysicae, 1993, 11:227-238.
［24］Carbone V, Bruno R. Cancellation exponents and multifractal scaling laws in the solar wind magnetohydrodynamic turbulence［J］. Annual Geophysicae, 1996, 14: 777-785
［25］Horbury T S, Balogh A, Forsyth R J, et al.Ulysses observations of intermittent heliospheric turbulence［J］. Advance Space Research, 1997, 19: 847-850.
［26］Horbury T, Tsurutani B. Ulysses measurements of waves, turbulence and discontinuities［A］. In: Balogh A, et al,eds. The Heliosphere Near Solar Minimum［C］. Springer and Praxis Publishing, 2002. 167-226.
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