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AMR-MHD Simulation of CME Propagation in Solar Wind Generated on Split Dodecahedron Grid

  • Tomoya Ogawa (a1), Mitsue Den (a2), Takashi Tanaka (a2) (a3) and Kazuyuki Yamashita (a4)

Abstract

We perform simulations of the interplanetary coronal mass ejections relating to the magnetic storm on 17 March 2015. A hierarchical mesh structure is used, which is controlled by an adaptive mesh refinement technique, with fine-scale cells where it matters, the structure of the running shock waves of the coronal mass ejections and co-rotating interactive regions. The initial and the inner-boundary conditions are derived from another simulation, which uses a split dodecahedron grid. The resulting shock-wave with the models adjusted to the observed ejection speed on the sky plane show delays by 20% in the arrival time at the Earth from the observed data. By contrast, the model adjusted to the observed arrival time at the Earth needs the ejection speed 30% higher than that in the above models.

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References

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Den, M., Tanaka, T., Kubo, Y. & Watari, S. 2015, 34th Int. Cosmic Ray Conf., 184
Khokhlov, A. M., 1998, J.Comput.Phys., 143, 519
Nakamizo, A., Tanaka, T., Kubo, Y., Kamei, S. & Shimazu, H., 2009, J. Geophys. Res., 114, A07109
Odstrcil, D. & Pizzo, V. J., 1999, J. Geophys. Res., 104, 483
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AMR-MHD Simulation of CME Propagation in Solar Wind Generated on Split Dodecahedron Grid

  • Tomoya Ogawa (a1), Mitsue Den (a2), Takashi Tanaka (a2) (a3) and Kazuyuki Yamashita (a4)

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