AI 中文总结
该研究提出新方法，结合矢量磁图、磁摩擦法、AWSoM模型与STITCH方法，成功模拟CME从太阳到地球的传播，其IMFR到达时间与磁场特征可反映地球效应。
AI 中文摘要
我们实现了一种用于开展日冕物质抛射（CME）从太阳到地球模拟的新方法，并将其应用于3个具有地球效应的空间天气事件进行测试。利用CME爆发前观测到的矢量磁图作为边界条件，我们采用成熟的磁摩擦法重建太阳活动区的非线性无力场（NLFFF）解。我们发现，在AWSoM模型中，包含NLFFF的爆发前太阳日冕会自发爆发。必要时我们采用光球驱动方法STITCH来增强CME激波的强度。这些爆发在全磁流体力学（MHD）模拟中成功产生了向1天文单位（au）传播的磁通量绳（MFR）。模拟CME的合成白光图像在形状上与观测结果极为相似。行星际磁通量绳（IMFR）到达1au的时间误差为1.5至9小时。将模拟的太阳风等离子体与原位测量结果对比表明，IMFR穿越时可再现南向的Bz分量，且其大小往往能被重现，而这决定了事件的地球效应。
英文摘要
We implement a novel approach to performing Sun-to-Earth coronal mass ejection (CME) simulations and test it on three geo-effective space weather events. Using a vector magnetogram observed prior to the CME as the boundary condition, we reconstruct non-linear force free field (NLFFF) solutions in solar active regions with an established magneto-frictional method. We find a pre-eruption solar corona containing the NLFFF in the AWSoM model, which then spontaneously erupts. We apply STITCH, a photospheric driving method, when needed, to increase the strength of the CME shock. The eruptions successfully produce magnetic flux ropes (MFRs) that propagate to 1 au in the full MHD simulation. The synthetic white light images of the simulated CMEs share a striking resemblance in shape to observations. The interplanetary MFRs (IMFRs) arrive at 1 au with a 1.5- to 9-hour error. A comparison of simulated solar wind plasma with in-situ measurements shows that IMFR crossing can reproduce a southward $B_z$ and often its magnitudes, which determine the geo-effectiveness of the event.
