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Titlebook: MHD Structures, Waves and Turbulence in the Solar Wind; Observations and The C.-Y. Tu,E. Marsch Book 1995 Springer Science+Business Media D

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書目名稱MHD Structures, Waves and Turbulence in the Solar Wind
副標題Observations and The
編輯C.-Y. Tu,E. Marsch
視頻videohttp://file.papertrans.cn/621/620156/620156.mp4
圖書封面Titlebook: MHD Structures, Waves and Turbulence in the Solar Wind; Observations and The C.-Y. Tu,E. Marsch Book 1995 Springer Science+Business Media D
描述This is the first book to give a comprehensive overview ofrecent observational and theoretical results on solar wind structuresand fluctuations and magnetohydrodynamic waves and turbulence,preference being given to phenomena in the inner heliosphere. Emphasisis placed on the progress made in the past decade in the understandingof the nature and origin of especially small-scale, compressible andincompressible fluctuations. Turbulence models describing the spatialtransport and spectral transfer of the fluctuations in the innerheliosphere are discussed. Intermittency of solar wind fluctuationsand their statistical distributions are investigated. Studies of theheating and acceleration effects of the turbulence on the backgroundwind are critically surveyed. Finally, open questions concerning theorigin, nature and evolution of the fluctuations are listed, andperspectives for future research are outlined. .The book is for graduate students and researchers in the field. Othertarget groups are scientists and professionals interested in spaceplasma physics and/or MHD turbulence. .
出版日期Book 1995
關鍵詞Heliosphere; MHD; Plasma; Solar wind; solar
版次1
doihttps://doi.org/10.1007/978-94-015-8541-5
isbn_softcover978-90-481-4520-1
isbn_ebook978-94-015-8541-5
copyrightSpringer Science+Business Media Dordrecht 1995
The information of publication is updating

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ons and magnetohydrodynamic waves and turbulence,preference being given to phenomena in the inner heliosphere. Emphasisis placed on the progress made in the past decade in the understandingof the nature and origin of especially small-scale, compressible andincompressible fluctuations. Turbulence mod
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The Heating and Acceleration Effects on the Solar Wind,c moment ../., which should be conserved in a collisionless double-adiabatic plasma. However, it is found observationally that ../. increases with increasing heliocentric distance. These results are interpreted as evidence that solar wind protons in high-speed streams are heated between 0.3 and 1 AU. Yet, the heat source remains to be determined.
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Introduction,so connected with basic MHD turbulence theory. The solar wind can be considered as a natural laboratory for the investigation of MHD turbulence in supersonic flow. So, studying the properties of interplanetary fluctuations has always been among the major research topics in solar wind physics from th
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Data Analysis and Basic Observational Results,rgodic random function of time. At least it can be meaningfully viewed as a’weakly’ stationary random function (i.e., the stationarity of the average and the two-pointtime correlation function is ensured). The time averages of the products of turbulent fields at fixed points in space are equivalent
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