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

Published online by Cambridge University Press:  24 July 2018

Tomoya Ogawa ,
Mitsue Den ,
Takashi Tanaka  and
Kazuyuki Yamashita
Tomoya Ogawa
Affiliation:
Kitasato University, 1-15-1 Kitasato, Minami-ku, Sagamihara, Kanagawa 252-0373, Japan email: ogawa@kitasato-u.ac.jp
Mitsue Den
Affiliation:
National Institute of Information and Communications Technology, Koganei, Tokyo, Japan
Takashi Tanaka
Affiliation:
National Institute of Information and Communications Technology, Koganei, Tokyo, Japan Kyushu University, Fukuoka, Japan
Kazuyuki Yamashita
Affiliation:
University of Yamanashi, Kofu, Yamanashi, Japan
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Abstract

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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.

Keywords

MHDmethods: numericalSun: coronal mass ejections (CMEs)solar wind
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S335: Space Weather of the Heliosphere: Processes and Forecasts , July 2017 , pp. 314 - 317
Copyright
Copyright © International Astronomical Union 2018 

References

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