邀请团队:　太阳活动和CME理论研究组

摘要:　　　The physical causes of coronal mass ejections (CMEs) have been debated by the solar community for over three decades now. The vast majority of proposed models agree that CMEs are the result of catastrophic loss of mechanical equilibrium or stability of the coronal magnetic field due to changes in the distribution of magnetic flux elements at the photosphere. These models usually involve idealized physical circumstances with either dipolar or quadrupolar underlying magnetic field geometries. The real Sun, however, demonstrates cases far more sophisticated than those idealized configurations. Therefore, studying the actual magnetic field geometries involved during CMEs is crucial for understanding the dynamical time scales of the eruption, acceleration profiles, etc. This talk summarizes the simulated dynamics of actual CME events and associated shock waves, and their comparison with observations. We discuss the influence of the global magnetic field on the geometry of the CME-driven shock waves, and the possible implications for the production of solar energetic particles.