Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-26T04:52:25.227Z Has data issue: false hasContentIssue false
  • English
  • Français

Simulation Studies of Solar Prominence Formation

Published online by Cambridge University Press:  12 April 2016

G.S. Choe  and
C.Z. Cheng
G.S. Choe
Affiliation:
Tongmyong University of Information Technology, Pusan 608-080, Korea
C.Z. Cheng
Affiliation:
Princeton Plasma Physics Laboratory, Princeton University, Princeton, NJ 08543, USA

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.

A series of numerical simulations are presented for formation of solar prominences. We have investigated the dynamic and thermodynamic evolution of coronal plasma in response to photospheric horizontal motions. In three different setups of field configurations and footpoint motions, different types of prominences are found to be formed by thermal instability.

Type
Birth and Death of Filaments
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 278 - 281
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Anzer, U. 1979, in Physics of Solar Prominences, Jensen, E. Maltby, P. and Q.|Orrall, F., Institute of Theoretical Astrophysics, Blindern:Oslo, p. 322 Google Scholar
Choe, G.S. 1995, Ph.D. Thesis, University of Alaska: Fairbanks Google Scholar
Choe, G.S. and Lee, L.C. 1992, Solar Phys., 138, 291 Google Scholar
Martin, S.F. 1990, in Dynamics of Quiescent Prominences, (eds.) Ruždjak, V. and Tandberg-Hanssen, E., Springer-Verlag:Berlin, p. 1 Google Scholar
Rompolt, B. and Bogdan, T. 1986, Coronal and Prominence Plasmas, (ed.) Poland, A., NASA CP 2442, Washington, D.C., p. 81 Google Scholar