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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

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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

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