Abstract
Timing and locating interplanetary (IP) shocks in the heliosphere constitutes a major task in space weather forecasting, as they are source of solar energetic particles and the leading signal of an upcoming magnetic cloud/interplanetary coronal mass ejection (MC/ICME) that causes major geomagnetic and aurora disturbances. Such a task is often complicated by the nonlinear interaction of the shock with its riding solar wind and, in some events, with other IP shocks. Using magnetohydrodynamics numerical simulation, we will discuss following issues. (1) How IP shocks are initiated near the Sun? (2) How IP shocks are evolving in the non‐uniform solar wind medium? (3) How IP shocks are interacting with each other? (4) How IP shocks are accelerating and decelerating? In addition, we will also compare simulation results with in‐situ observations.
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