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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tolerance

Tincture

否認(rèn)

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

不規(guī)則的跳動

Merited

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.

buoyant

粗鄙的人

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

Soliloquy

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

Overthrow