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Solar Physics

, 294:143 | Cite as

Parametric Study of ICME Properties Related to Space Weather Disturbances via a Series of Three-Dimensional MHD Simulations

  • Junmo An
  • Tetsuya MagaraEmail author
  • Keiji Hayashi
  • Yong-Jae Moon
Article

Abstract

Interplanetary coronal mass ejections (ICMEs) are important drivers of space-weather disturbances observed at the Earth. We use a parameterized ICME model to investigate the relation between the physical properties of an ICME and these disturbances. Compared to those studies focused on deriving a best set of ICME parameter values matched with observed disturbances, this study is aimed at investigating the role of each parameter in producing space-weather disturbances. Toward this end, we performed a series of three-dimensional magnetohydrodynamic (MHD) simulations with different sets of ICME parameter values. These parameters are the location, speed, mass, magnetic field strength, and magnetic field orientation of a spheromak-shaped ICME, which is injected into the solar wind reconstructed from near-Sun data and interplanetary scintillation (IPS) data via an MHD-IPS tomography method. By comparing simulation results to in situ observations near the Earth we discuss how the physical properties of an ICME affect space-weather disturbances at the Earth.

Keywords

Coronal mass ejections, interplanetary Magnetic fields, interplanetary Solar wind, disturbances 

Notes

Acknowledgements

The authors wish to thank Kyung Hee University for general support of this work. J.A. thanks Gwangson Choe for his instructive comments. J.A. thanks Soojeong Jang and Jihye Kang for providing the data and information used in this work. J.A. also thanks Takashi Tanaka for providing the REPPU code and useful comments on the code. The CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between ESA and NASA. The authors used the synoptic charts of solar-surface magnetic fields provided by Wilcox Solar Observatory (WSO), Stanford University (http://wso.standford.edu). We also acknowledge use of NASA/GSFC Space Physics Data Facility OMNIWeb service, and OMNI data. Figure 3 was created using VAPOR (Clyne and Rast, 2005; Clyne et al., 2007). J.A. thanks the researchers at NICT for their detailed comments, suggestions, and constant support. This work was supported by the National Research Foundation of Korea (NRF) grant funded by the Korean government (MSIT) (NRF-2017R1A2B4002383, PI: T. Magara), as well as the BK21 plus program through the NRF.

Disclosure of Potential Conflicts of Interest

The authors declare that there are no conflicts of interest.

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Copyright information

© Springer Nature B.V. 2019

Authors and Affiliations

  1. 1.School of Space ResearchKyung Hee UniversityYonginRepublic of Korea
  2. 2.Department of Astronomy and Space ScienceKyung Hee UniversityYonginRepublic of Korea
  3. 3.NWRABoulderUSA
  4. 4.Institute of Space-Earth Environmental ResearchNagoya UniversityNagoyaJapan
  5. 5.HEPLStanford UniversityStanfordUSA

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