Abstract

A 3-D numerical magnetohydrodynamic model is used to investigate the temporal and spatial evolution of large-scale solar wind (SW) disturbances. A tilted-dipole outflow configuration is specified at the inner boundary near the Sun, and a structured, corotating SW flow is established by dynamic relaxation between 0.14 and 1.04 AU. Time-dependent variation of the pressure and velocity at the inner boundary is applied to simulate injection of a coronal mass ejection (CME) near the streamer belt with a monopolar interplanetary magnetic field (IMF). Numerical results show that the motion and appearance of a CME are affected by its interaction with the velocity and density structure of the background SW. This 3-D dynamic interaction also affects the orientation and magnitude of the IMF.

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