Modeling Coronal Mass Ejections by CESE MHD Model

  • Xueshang FengEmail author
Part of the Atmosphere, Earth, Ocean & Space book series (AEONS)


Coronal mass ejections (CMEs) consist of large-scale eruptions of magnetized plasma from the Sun, and they are considered to be the major drivers of adverse space weather disturbances that strongly affect our high-tech activities of humankind. Even the fastest CMEs require almost a day to arrive at Earth and initiate a geomagnetic storm. This allows, in principle, sufficient time to predict their impact. The geoeffectiveness of CMEs, that is, of the associated interplanetary CME (ICME) or magnetic cloud (MC), is primarily dependent on their Earth-side magnetic field direction (Bz), their velocity, and their associated ram pressure upon arrival at the magnetosphere. It is therefore highly expected to predict these parameters before an ICME (and the shock that potentially precedes it) arrives at Earth. A promising tool for such purpose is magnetohydrodynamic (MHD) numerical simulations. An accurate modeling of their onset and propagation up to 1 AU represents a key issue for more reliable space weather forecasts. To this end, a lot of CME-related models have been developed to describe their pre-eruption structures, their initiations, and their eruptions, and also the propagation of CMEs from the Sun to the Earth has been numerically investigated. In this chapter, after we briefly introduce the CME models so far, we numerically study the time-dependent evolution and propagation of the CME from the Sun to Earth using the 3D SIP-CESE MHD model introduced in Chap.  4, compare the simulation results with spacecraft observations and analyze in detail the CME’s propagation characteristics.


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© Springer Nature Singapore Pte Ltd. 2020

Authors and Affiliations

  1. 1.SIGMA Weather Group, State Key Laboratory of Space Weather, National Space Science CenterChinese Academy of SciencesBeijingChina

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