Hostname: page-component-586b7cd67f-tf8b9 Total loading time: 0 Render date: 2024-11-26T13:39:46.358Z Has data issue: false hasContentIssue false
  • English
  • Français

Disappearances of High-Latitude Filaments as Sources of High-Latitude CMEs

Published online by Cambridge University Press:  12 April 2016

E.W. Oliver  and
D.F. Webb
E.W. Oliver
Affiliation:
Air Force Research Laboratory, Hanscom Air Force Base, Massachusetts 01731-3010, USA
D.F. Webb
Affiliation:
Institute for Scientific Research, Boston College, Chestnut Hill, Massachusetts 02467, 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.

From a statistical comparison of high-latitude coronal mass ejections (CMEs) and disappearing solar filaments (DSFs), we find: (1) Beginning with the “rush to the poles”, DSFs arise at an increasing rate from the “emerging” or polar crown relative to the “true” polar crown. At maximum, these “opposite polarity” filaments are the dominant source of high-latitude DSFs. Following polarity reversal, the emergent polar crown becomes the true polar crown and the source of virtually all highlatitude DSFs. (2) At the last two solar maxima, we estimate that there were ~ 4 times as many high-latitude (≥ 60°) CMEs as high-latitude (≥ 45°) DSFs. Possible reasons for this discrepancy include the following: (a) DSFs, particularly small ones, are under-reported, (b) propagation effects, whereby radially propagating CMEs appear at higher latitudes than their underlying source regions, are more important than currently thought, or (c) some combination of these effects.

Type
Global Patterns
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 479 - 483
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Burkepile, J.T. and St, O.C.. Cyr 1993, NCAR/TN-369+STRGoogle Scholar
Cliver, E.W., Cyr, O.C.St., Howard, R.A. and McIntosh, P.S. 1994, Solar Coronal Structures, (eds.) Rusin, V. et al., Veda, Bratislava, p. 83 Google Scholar
Howard, R.A., Sheeley, N.R. Jr., Koomen, M.J. and Michels, D.J. 1985, J. Geophys. Res., 90, 8173 Google Scholar
Hundhausen, A.J. 1993, J. Geophys. Res., 98, 13177 Google Scholar
McAllister, A.H. et al. 1996, J. Geophys. Res., 101, 27625 Google Scholar
McIntosh, P.S. 1992, in The Solar Cycle, (ed.) Harvey, K., ASP Conf. Ser. Vol.27, San Francisco, p. 14 Google Scholar
McIntosh, P.S. 1979, Annotated Atlas of Hα Synoptic Charts, UAG-70, WDC-AGoogle Scholar
Mouradian, Z., Soru-Escaut, I., and Pojoga, S. 1995, Solar Phys., 158, 269 Google Scholar
Webb, D.F. and Howard, R.A. 1994, J. Geophys. Res., 99, 4201 Google Scholar
Webb, D.F. and Hundhausen, A.J. 1987, Solar Phys., 108, 383 Google Scholar
Wright, C.S. 1991, Catalog of Solar Filament Disappearances, UAG-100, WDCAGoogle Scholar