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High Speed Solar Wind Forecast Model from the Solar Surface to 1AU Using Global 3D MHD Simulation

Published online by Cambridge University Press:  24 July 2018

Mitsue Den ,
Takashi Tanaka ,
Yuki Kubo  and
Shinichi Watari
Mitsue Den
Affiliation:
National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795, Japan email: [email protected]
Takashi Tanaka
Affiliation:
National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795, Japan email: [email protected] Kyushu University, 744 Motooka, Nishi-ku, Fukuoka 819-0395, Japan
Yuki Kubo
Affiliation:
National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795, Japan email: [email protected]
Shinichi Watari
Affiliation:
National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795, Japan email: [email protected]
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Abstract

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Emanating from coronals holes (CHs), high speed streams (HSSs) cause recurrent geomagnetic disturbances in the Earth’s magnetosphere. For this reason being able to predict the occurrence and timing of the high speed solar wind is one of the more important issues in space weather forecasting. Currently, it is still difficult to estimate the effect of a CH in case that it extends from high latitudes to lower ones. To monitor the global solar wind condition we have therefore developed a three-dimensional MHD simulation code, the REProduce Plasma Universe (REPPU) code, that is driven by the solar magnetic field from the solar surface to 1AU. The connectivity of magnetic field lines from CHs to Earth’s orbit via HSSs has been investigated. Simulation results are presented and the usefulness of our model is discussed.

Keywords

Space weatherMHDmethods: numericalSun: corona (Sun:) solar windsolar-terrestrial relations
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. 272 - 275
Copyright
Copyright © International Astronomical Union 2018 

References

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