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Three-dimensional Simulation of the Fast Solar Wind Driven by Compressible Magnetohydrodynamic Turbulence

  • Authors: Munehito Shoda, Takeru Ken Suzuki, Mahboubeh Asgari-Targhi, and Takaaki Yokoyama

2019 The Astrophysical Journal Letters 880 L2.

  • Provider: AAS Journals

Caption: Figure 4.

(a) Snapshot of fractional density fluctuation δρ/ρ in the meridional plane. (b) Growth rate of parametric decay instability (PDI) (γPDI/2, solid line) in units of mHz and the magnitude of density fluctuation (δρrms/ρ, dashed line) vs. radial distance. (c) Reflection rates of antisunward Alfvén waves ωref with and without density fluctuations. The animation of panel (a) runs from simulation time, τ = 0 to 50 minutes, where τ = 0 is when the system reaches a quasi-steady state.

(An animation of this figure is available.)

The video/animation of this figure is available in the online journal.

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