Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-26T14:40:09.806Z Has data issue: false hasContentIssue false
  • English
  • Français

Are Prominences Formed by Flux Convergence?

Published online by Cambridge University Press:  12 April 2016

K. Galsgaard  and
A.W. Longbottom
K. Galsgaard
Affiliation:
Department of Mathematical and Computational Sciences, University of St. Andrews, St. Andrews, North Haugh, KY16 9SS, Scotland
A.W. Longbottom
Affiliation:
Department of Mathematical and Computational Sciences, University of St. Andrews, St. Andrews, North Haugh, KY16 9SS, Scotland

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 3D resistive MHD experiments are used to investigate the dynamical properties of a quadrupolar magnetic field, as the two dipolar regions are pushed together. A current concentration is formed between the approaching flux concentrations and, when reconnection starts, material is lifted against gravity. As it rises the material spreads out along the polarity inversion line and forms a prominence-like structure.

Type
Birth and Death of Filaments
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 282 - 285
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Galsgaard, K. and Longbottom, A.W. 1998, ApJ, in preparationGoogle Scholar
Longbottom, A.W. et. al. 1997, A&AS, submittedGoogle Scholar
Martin, S.F. 1990, in Dynamics of Quiescient Prominences, (eds.) Ruzdjah, V. and Tandberg-Hansen, E., Springer-Verlag, New York, p. 1 Google Scholar
MacKay, D. et al. 1997, ApJ, 486, 534 Google Scholar