Abstract
The mutual spatial arrangement of coronal mass ejections and eruptive prominences on the Sun is considered. These phenomena occur on different scales and are observed at different heights above the solar surface. In spite of the presumed causal connection between them, they are often widely separated in position angle at epochs of solar minimum. This means that the motion of a prominence in the corona is not strictly radial and has an appreciable component along the surface. This behavior can be explained in a model of a filament as a magnetic flux rope in equilibrium in the coronal magnetic field. The initial trajectory of the filament is determined by the structure of the global field.
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References
F. Crifo, J. P. Picat, and M. Cailloux, Sol. Phys. 83, 143 (1983).
D. G. Sime, R. M. MacQueen, and A. J. Hundhausen, J. Geophys. Res. 89, 2113 (1984).
D. F. Webb, in IAU Coll. No. 167: New Perspectives on Solar Prominences, Ed. by D. Webb, D. Rust, and B. Schmieder (Astron. Soc. Pacific, San Francisco, 1998); ASP Conf. Ser. 150, 463 (1998).
E. W. Cliver and D. F. Webb, in IAU Coll. No. 167: New Perspectives on Solar Prominences, Ed. by D. Webb, D. Rust, and B. Schmieder (Astron. Soc. Pacific, San Francisco, 1998); ASP Conf. Ser. 150, 479 (1998).
N. Gopalswamy, Y. Hanaoka, and H. S. Hudson, Adv. Space Res. 25, 1851 (2000).
R. H. Munro and A. J. Hundhausen, Sol. Phys. 108, 383 (1987).
N. R. Sheeley, Jr., R. A. Howard, M. J. Koomen, and D. J. Michels, Astrophys. J. 272, 349 (1983).
D. F. Webb and A. J. Hundhausen, Sol. Phys. 108, 383 (1987).
O. C. St. Cyr and D. F. Webb, Sol. Phys. 136, 379 (1991).
H. Wang and P. Goode, in Synoptic Solar Physics, Ed. by K. S. Balasubramanian, J. W. Harvey, and D. M. Rabin (Astron. Soc. Pacific, San Francisco, 1998); ASP Conf. Ser. 140, 497 (1998).
G. Yang and Y. Wang, in Proc. COSPAR Colloq., Ser. 14: Magnetic Activity and Space Environment, Ed. by H. N. Wang and R. L. Xu (Pergamon, Boston, 2002), p. 113.
Z. Mouradian, I. Soru-Escaut, and S. Pojoga, Sol. Phys. 158, 269 (1995).
M. M. Molodenskii, B. P. Filippov, and N. S. Shylova, Astron. Zh. 69, 181 (1992) [Sov. Astron. 36, 92 (1992)].
H. R. Gilbert, T. E. Holzer, J. T. Burkepile, and A. J. Hundhausen, Astrophys. J. 537, 503 (2000).
K. Hori and J. L. Culhane, Astron. Astrophys. 382, 666 (2002).
N. Gopalswamy, M. Shimojo, W. Lu, et al., Astrophys. J. 586, 562 (2003).
B. Filippov and S. Koutchmy, Sol. Phys. 208, 283 (2002).
S. Bravo, G. A. Stewart, and X. Blanco-Cano, Sol. Phys. 179, 223 (1998).
B. P. Filippov, N. Gopalswamy, and A. V. Lozhechkin, Sol. Phys. 203, 119 (2001).
B. P. Filippov, N. Gopalsvamy, and A. V. Lozhechkin, Astron. Zh. 79, 462 (2002) [Astron. Rep. 46, 417 (2002)].
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Translated from Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l}\) Zhurnal, Vol. 81, No. 2, 2004, pp. 168–175.
Original Russian Text Copyright © 2004 by Lozhechkin, Filippov.
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Lozhechkin, A.V., Filippov, B.P. Coronal mass ejections and eruptive prominences: Mutual spatial arrangement. Astron. Rep. 48, 145–152 (2004). https://doi.org/10.1134/1.1648078
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DOI: https://doi.org/10.1134/1.1648078