Merging of coronal and heliospheric numerical two-dimensional MHD models D. Odstrcil, et al., J. Geophys. Res., 107, 2002. 2004 年 10 月 14 日太陽雑誌会 ( 速報.

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Merging of coronal and heliospheric numerical two-dimensional MHD models D. Odstrcil, et al., J. Geophys. Res., 107, 年 10 月 14 日太陽雑誌会 ( 速報 ) 西田

Introduction Space weather research involves a chain of various phenomena occurring simultaneously on different spatial and temporal scales. An integrated modeling approach is necessary for space weather research. This paper presents a demonstration of merged coronal and heliospheric 2-D MHD models.

Numerical Models Coronal Model –2-D axisymmetric resistive MHD equations –Semi-implicit finite difference scheme using staggered values Heliospheric Model –2-D axisymmetric ideal MHD equations –Explicit finite difference total-variation- diminishing high-resolution Lax-Friendrichs (TVDLF) scheme using cell-centered values

Merged numerical grid Fig. 1 Coronal Model –200x300 grid points –Nonuniform mesh for the streamer Heliospheric Model –340x240 grid points The output from the coronal model is used as a boundary condition for the heliospheric solutions

Fig. 2 Ambient State in the corona

Fig. 3 Ambient State in the heliosphere

Fig. 4. Blue: 70°, Red: 80°, Black: 90°

Transient Disturbances The streamer products strongly sheared field lines that are nearly aligned with the neutral line; it is just a convenient mechanism. The sharing phase lasts 5.2 days. We reduce the magnetic flux at the photosphere to create a flux rope. After ~18 hours the arcade erupts.

Fig. 5

Fig. 6. Blue: 70°, Red: 80°, Black: 90°

Fig. 7

Fig. 8

Fig. 9

Fig. 10. Blue: 70°, Red: 80°, Black: 90°

Conclusions (1/2) The merging of coronal and heliospheric MHD models has been successfully implemented for a 2-D ambient state and a transient disturbance. Different mathematical models, numerical methods, and computational grids were used in this work, and thus the merging of the numerical models was demonstrated for a quote general case.

Conclusions (2/2) Merged coronal and heliospheric models have enabled the simulation of transient disturbances. The solar wind and magnetic parameters at 1 AU resulting from the coupled computations can provide input for geo- effectivity models.

Fig. A1