Numerical simulation of the 12 May 1997 interplanetary CME event
Numerical simulation of the 12 May 1997 interplanetary CME event
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DOI：
10.1029/2003ja010135
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发表时间：
2004-02
影响因子：
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通讯作者：
D. Odstrcil;P. Riley;Xuepu Zhao
中科院分区：
文献类型：
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作者：
D. Odstrcil;P. Riley;Xuepu Zhao
[1]只要在太阳附近指定适当的时间相关边界条件，数值三维磁流体动力学模型就能够预测地球上的大规模太阳风结构。由于目前对这些条件的了解不足以直接驱动模型，因此使用了各种近似。本文介绍了一个数值模式的主要特点和近似方法，其中（1）环境太阳风是利用光球磁场观测资料从日冕模式中导出的，（2）瞬变扰动是由日冕物质抛射观测资料的几何和运动学拟合导出的。我们选择了1997年5月12日定义明确的晕-日冕物质抛射事件作为我们的初始事件，因为它的特点是喷出物发射到相对安静的太阳和行星际背景中。数值模拟使我们能够预测的冲击和喷出物的到来，并为我们提供了一个全球性的瞬态扰动与适度快速的太阳风流相互作用的图片。
[1] Numerical three-dimensional magnetohydrodynamic models are capable of predicting large-scale solar wind structures at Earth, provided that appropriate time-dependent boundary conditions are specified near the Sun. Since knowledge of such conditions is at present insufficient to directly drive the models, various approximations are used. In this paper, we introduce the main features and approximations of a numerical model where (1) the ambient solar wind is derived from coronal models utilizing photospheric magnetic field observations and (2) transient disturbances are derived from geometrical and kinematic fitting of coronagraph observations of coronal mass ejections (CMEs). We have chosen the well-defined halo-CME event of 12 May 1997 as our initial event because it is characterized by a relatively quiet solar and interplanetary background into which the ejecta was launched. The numerical simulation has enabled us to predict the arrival of the shock and ejecta and provided us with a global picture of transient disturbance interacting with a moderately fast solar wind stream.