Hostname: page-component-5c6d5d7d68-sv6ng Total loading time: 0 Render date: 2024-08-26T11:22:37.117Z Has data issue: false hasContentIssue false
  • English
  • Français

Formation of Solar Prominences with Normal and Inverse Polarities

Published online by Cambridge University Press:  12 April 2016

G. S. Choe  and
L. C. Lee
G. S. Choe
Affiliation:
Geophysical Institute, University of Alaska Fairbanks, AK 99775-0800, U.S.A.
L. C. Lee
Affiliation:
Geophysical Institute, University of Alaska Fairbanks, AK 99775-0800, U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Numerical simulations of solar prominence formation are presented employing photospheric horizontal motions as boundary conditions. Three different combinations of magnetic field configurations and footpoint motions are considered: (1) a bipolar arcade with a footpoint shear, (2) an arcade exposed to a shearing and converging motion, (3) two adjacent arcades undergoing a shearing and converging motion. In each case, it is found that the dynamic evolution of magnetic fields can force the plasma into a thermal instability leading to the formation of a prominence.

Type
Session 2. Theory of Active Region Structure
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 138 - 142
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Choe, G.S. & Lee, L.C. 1992, Solar Phys. 138, 291 CrossRefGoogle Scholar
Hildner, E. 1974, Solar Phys. 35, 123 CrossRefGoogle Scholar
Inhester, B., Birn, J., & Hesse, M. 1992, Solar phys. 138, 257 CrossRefGoogle Scholar
Kippenhahn, R. & Schlüter, A. 1957, Zs. Ap. 43, 36 Google Scholar
Kuperus, M. & Raadu, M.A. 1974, Astr. Ap. 31, 185 Google Scholar
Lee, L.C. 1990, a presentation given in the ‘Workshop on Solar Flares and Magnetospheric Substorms’, Hawaii (unpublished)Google Scholar
Lee, L. C., Choe, G. S., & Akasofu, S.-I. 1992, in Ashour-Abdalla, M. & Chang, T. (eds.), Micro/Meso Scale Phenomena in Space Plasmas, AGU, Washington, D.C. (in press)Google Scholar
Lee, L.C. & Fu, Z.F. 1986, J. Geophys. Res. 91, 6807 CrossRefGoogle Scholar
Leroy, J.L. 1989, in Priest, E. R. (ed.), Dynamics and Structure of Quiescent Solar Prominences, Kluwer Academic Publishers, Dordrecht, Holland, p. 77 Google Scholar
Low, B.C. 1992, Astr. Ap. 253, 311 Google Scholar
Martin, S.F. 1990, in Ruzdjak, V. & Tandberg-Hanssen, E. (eds.), Dynamics of Quiescent Prominences, IAU Colloquium 117, Springer-Verlag, Berlin, p.l Google Scholar
Rompolt, B. & Bogdan, T. 1986, in Poland, A. (ed.), Coronal and Prominence Plasmas, NASA Conference Publication 2442, Washington, D.C., p. 81 Google Scholar
Tang, F. 1987, Solar Phys. 107, 233 CrossRefGoogle Scholar