By C.-Y. Tu
This is the 1st e-book to offer a entire evaluation of modern observational and theoretical effects on sun wind buildings and fluctuations and magnetohydrodynamic waves and turbulence, choice being given to phenomena within the internal heliosphere. Emphasis is put on the development made long ago decade within the realizing of the character and beginning of particularly small-scale, compressible and incompressible fluctuations. Turbulence types describing the spatial delivery and spectral move of the fluctuations within the internal heliosphere are mentioned. Intermittency of sunlight wind fluctuations and their statistical distributions are investigated. reviews of the heating and acceleration results of the turbulence at the heritage wind are severely surveyed. eventually, open questions about the foundation, nature and evolution of the fluctuations are indexed, and views for destiny examine are defined.
The e-book is for graduate scholars and researchers within the box. different goal teams are scientists and pros attracted to house plasma physics and/or MHD turbulence.
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Additional info for MHD Structures, Waves and Turbulence in the Solar Wind: Observations and Theories
Example text
3-7. Left: cartoon to show the idea about the occurrence of Alfven waves and convective structures in the solar wind. Right: cartoon to show the idea about the angular affect in the sampling of solar wind fluctuations (adopted from TIl and Marsch, 1992). scale variations along the magnetic field lines. Since the corresponding magnetic stress tensor is too small to drive the fluid to move with a considerable speed during the expansion time (Jokipii and Kota, 1989), the large-scale variations are just convected by the solar wind.
The spacecraft, the beginning time of the data set (year, day), and the distance from the Sun are written on the top of the figures. 06 hours for each data set. The average plasma parameters for these periods are given at the top. The upper and middle panel are adopted from Th et al. (1989b). -Y. TV AND E. MARSCH Vp km/s 100 6Va~ ~ ~. 0 I 1 O~--------------------------------------------~ , 180 ' 90 0 -90 ap deg '20 deg as deg -180 0 -20 -]0 .......... -, ·v ... -,... - -___ . ~ - 0 Coo deg ~--------------------------------------------_1-]0 0 -45 -90 ~----------------------------------------------------------------------~·20 '20~--------------------------------------------~-20 o .
Intriligator (1981) gave a review on these previous studies. Electron density spectra have also been obtained and widely studied by using interplanetary scintillation data. Woo and Armstrong (1979), Woo (1981) and Woo (1993) gave detailed reviews of these studies. 3 AU and out to 1 AU. Coles and Harmon (1989) and Coles et al. (1991a) found that within 20 R 0 , density fluctuation spectra are Kolmogorov-like in the scale range of 103_106 km, while in the smaller scales the spectra have a local flattening.
