Abstract
We present a numerical simulation of the fast magnetosonic shock wave formation during a two-current-loop collision by using a magnetohydrodynamical model. It is shown that the rarefaction waves are generated in the initial stage when the two current loops start to collide. After the rarefaction waves propagate away from the excited region, the fast magnetosonic waves with density enhancement can be produced for the simulation when the current strength of the loop is weak. As the current becomes strong enough, the magnetosonic shock waves can be generated in the direction perpendicular to that of the two-loop collision.
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References
De Jager, C.: 1988,20th Int. Cosmic Ray Conf. 7, 66.
Hender, T. C., Gimblett, C. G., and Robinson, D. C.: 1989,Nuclear Fusion 29, 1279.
Koide, S.: 1990,J. Phys. Soc. Japan 59, 3952.
Ohsawa, Y. and Sakai, J.: 1988,Astrophys. J. 332, 439.
Ramaty, R. and Marphy, R. J.: 1987,Space Sci. Rev. 45, 213.
Sakai, J. and Ohsawa, Y.: 1987,Space Sci. Rev. 46, 13.
Sakai, J.: 1990,Astrophys. J. Suppl. 73, 321.
Sakai, J. and de Jager, C.: 1991,Solar Phys. 134, 329.
Takahashi, M., Sakai, J. I., and Yohkoh Group: 1992,Proceeding of Annual Fall Meeting of Japan Astronomical Society.
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Koide, S., Sakai, JI. Formation of fast magnetosonic shock waves during a two-current-loop collision in solar flares. Sol Phys 151, 137–145 (1994). https://doi.org/10.1007/BF00654087
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DOI: https://doi.org/10.1007/BF00654087