The formation of a current-carrying non-force-free magnetic loop is studied by threedimensional magnetohydrodynamic simulation. The effects of the plasma pressure and the gravitational force are considered for the first time. The results show that the twist motion of the footpoints of magnetic field lines at the photosphere will form magnetic loop in the corona. The magnetic loop expands mainly in both the vertical and horizontal directions along the magnetic neutral line at the photosphere bases.
Key words
magnetic loops /
formation and evolution
{{custom_keyword}} /
{{custom_sec.title}}
{{custom_sec.title}}
{{custom_sec.content}}
References
[1] R. Kano and S. Tsuneta, Astrophys. J. 454 (1995) 934.
[2] E.R. Priest, Physics of Magnetic Fluz Ropes, eds C.T. Russel et al., American GeophysicalUnion, Washington DC (1990) p. 1.
[3] M. Ugai, Phys. Plasmas 3 (1996) 4172.
[4] K. Shibata, T. Tajima, et al., Astrophys. J. 345 (1989) 584.
[5] S. Poedts and G.C. Boynton, Astron. Astrophys. 306 (1996) 610.
[6] J.A. Klimchuk and P.A. Sturrock, Astrophys. J. 385 (1992) 344.
[7] T. Amari, J.F. Luciani, et al., Astrophys. J. 466 (1996) L39.
[8] M. Ozaki and T.' Sato, Astrophys. J. 481 (1997) 524.
[9] J.I. Sakai and C. de Jager, Solar Phys. 173 (1997) 347.
[10] B.C. Low, Astrophys. J. 399 (1992) 300.
[11] J.D. Ramshaw, J. Compt. Phys. 52 (1983) 592.
{{custom_fnGroup.title_en}}
Footnotes
{{custom_fn.content}}
Funding
The project supported by National Natural Science Foundation of China (No. 19573009) and Ministry of Science and Technology of China
{{custom_fund}}
PDF(310 KB)
