乱流モデルからみた太陽風乱流のアルヴェーン比(宇宙流体(3),一般講演)

概要

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A turbulence model based on a statistical analysis of magnetohydrodynamic (MHD) turbulence with the flow-expansion effects incorporated is applied to the solar wind. In the model, the dynamics of the turbulent MHD residual energy (difference between the kinetic and magnetic energies) and the turbulent cross helicity (velocity-magnetic-field correlation) are simultaneously solved with those of the turbulent MHD energy and its dissipation rate. The observed radial behaviors of the solar-wind turbulence, i.e., the decay of the cross helicity and the stationariness of the Alfven ratio (γ_A, the ratio of kinetic to magnetic-field energies) are reproduced by using a numerical simulation of the model. The stationary value of γ_A≃0.5 far from the Sun is elucidated as a stationary solution of the turbulence model.
日本流体力学会の論文
2007-08-06