【摘 要】
：
The solar wind is permeated by all kinds of fluctuations ranging broadly inscales from those of the solar corona and inner heliosphere down to the local ionand electron plasma kinetic scales.
【机 构】
：
Institute for Experimental and Applied Physics,Christian-Albrechts-University at Kiel,D-24118 Kiel,G
【出 处】
：
The Fourteenth International Solar Wind Conference (第十四届国际太阳
论文部分内容阅读
The solar wind is permeated by all kinds of fluctuations ranging broadly inscales from those of the solar corona and inner heliosphere down to the local ionand electron plasma kinetic scales.
其他文献
Quasi-periodic,fast-propagating wave trains(QFPs;Liu et al.2011,2012 ApJ) are a new observational phenomenon recently discovered in the corona by SDO/AIA with extreme ultraviolet(EUV) imaging observat
It was recently reported that the spectral slope and the correlation function of the magnetic field in the solar wind turbulence are anisotropic when they are based on continuous time series with loca
The solar wind is a turbulent medium characterized by a high degree of Alfvénicity,namely,a high correlation between velocity and magnetic field components andequipartition between the kinetic and mag
The slow solar wind turbulence has recently been considered as fully evolved turbulence which can be described by GS theory.However,here we present new findings that support a different understanding.
The solar wind plasma is only weakly collisional and during its expansion in interplanetary space can deviate significantly from thermodynamical equilibrium.
We will present results from a two-dimensional,large-scale hybrid expanding box simulation of the solar wind plasma turbulence.We impose an initial ambient magnetic field perpendicular to the simulati
The Solar wind is observed to expand outward non-adiabatically.The energy source for the non-adiabatic behavior is commonly attributed to the solar wind turbulence.
The problem of the turbulent dissipation and heating of the solar wind at kinetic scales represents nowadays a top priority subject in space plasma physics.Here,kinetic effects in the turbulent interp
The transition range of solar wind turbulence is the range of scales close to the ion gyroscale kρi～1,where turbulence properties undergo significant changes:turbulence becomes dispersive and kinetic
High speed streams are often characterized by a core proton temperature anisotropy such that Tp⊥＞Tp‖ and by a minority population of alpha particles such that(v)α‖＞(v)p‖,where(v)‖ is the component of