AMR和网格拉伸对Icarus中磁化CME模型的影响
The effect of AMR and grid stretching on the magnetized CME model in Icarus
AI总结：
本研究在Icarus模型中应用AMR和网格拉伸模拟磁化CME，发现AMR级别4在保持高分辨率细节的同时，计算效率最优，且到达时间与EUHFORIA接近。
摘要：
背景。日冕物质抛射（CME）是地球附近太阳风扰动的主要驱动因素。当它们朝向地球时，CME的内部磁场可以与地球磁场相互作用并引发地磁暴。为了更好地预测和避免此类事件造成的损害，已实现了优化的日球层模型Icarus。目标。CME对地球的影响很大程度上受其内部磁场结构的影响。本工作的目标是能够在Icarus中模拟CME磁场结构在其传播过程中的演化。研究的重点是CME的整体磁结构及其演化和与太阳风的相互作用。方法。Icarus中实现的磁化CME模型是线性无力球状等离子体（Linear Force-Free Spheromak），并从EUHFORIA导入。应用了先进技术，如网格拉伸和AMR。应用不同的AMR级别以在需要的地方局部获得高分辨率。所有模拟的结果都进行了详细比较，并提供了模拟的墙钟时间。结果。对执行的模拟结果进行了分析。到达时间由EUHFORIA模拟更好地近似，CME激波比AMR级别4和5的模拟分别晚1.6和1.09小时到达。剖面特征和变量强度由AMR级别4和5的Icarus模拟最好地建模。结论。在EUHFORIA模拟中到达时间更接近观测时间，但在Icarus模拟中不同变量的剖面显示出更多特征和细节。考虑到模拟结果的微小差异和计算资源的大差异，AMR级别4的模拟被认为表现最佳。
英文摘要：
Context. Coronal mass ejections (CMEs) are the main driver of solar wind disturbances near Earth. When directed towards us, the internal magnetic field of the CME can interact with the Earth`s magnetic field and cause geomagnetic storms. In order to better predict and avoid damage coming from such events, the optimized heliospheric model Icarus has been implemented. Aims. The impact of a CME at Earth is greatly affected by its internal magnetic field structure. The aim of this work is to enable modelling the evolution of the magnetic field configuration of the CME throughout its propagation in Icarus. The focus of the study is on the global magnetic structure of the CME and its evolution and interaction with the solar wind. Methods. The magnetized CME model that is implemented in Icarus is the Linear Force-Free Spheromak and is imported from EUHFORIA. Advanced techniques, such as grid stretching and AMR are applied. Different AMR levels are applied in order to obtain high resolution locally, where needed. The results of all the simulations are compared in detail and the wall-clock times of the simulations are provided. Results. The results from the performed simulations are analyzed. The arrival time is better approximated by the EUHFORIA simulation, with the CME shock arriving 1.6 and 1.09 hours later than in the AMR level 4 and 5 simulations, respectively. The profile features and variable strengths are best modelled by Icarus simulations with AMR level 4 and 5. Conclusions. The arrival time is closer to the observed time in the EUHFORIA simulation, but the profiles of the different variables show more features and details in the Icarus simulations. Considering the small difference in the modelled results, and the large difference in computational resources, the AMR level 4 simulation is considered to have performed the best.
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