The Relationship of Green-Line Transients to White-Light Coronal Mass Ejections |
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| Authors: | S P Plunkett G E Brueckner K P Dere R A Howard M J Koomen C M Korendyke D J Michels J D Moses N E Moulton S E Paswaters O C St Cyr D G Socker D Wang G M Simnett D K Bedford D A Biesecker C J Eyles S J Tappin R Schwenn P L Lamy A Llebaria |
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| Institution: | (1) NASA Goddard Space Flight Center, Universities Space Research Association, Mail Code 682.3, Greenbelt, MD, 20771, U.S.A;(2) Naval Research Laboratory, E.O. Hulburt Center for Space Research, Washington, DC, 20375, U.S.A;(3) School of Physics and Space Research, University of Birmingham, Edgbaston, Birmingham, B15 2TT, U.K;(4) Max Planck Institut für Aeronomie, D-37189 Katlenburg-Lindau, Germany;(5) Laboratoire d'Astronomie Spatiale, F-13376 Marseille Cedex 12, France |
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| Abstract: | We report observations by the Large Angle Spectrometric Coronagraph (LASCO) on the SOHO spacecraft of three coronal green-line
transients that could be clearly associated with coronal mass ejections (CMEs) detected in Thomson-scattered white light.
Two of these events, with speeds >25 km s-1, may be classified as ‘whip-like’ transients. They are associated with the core of the white-light CMEs, identified with
erupting prominence material, rather than with the leading edge of the CMEs. The third green-line transient has a markedly
different appearance and is more gradual than the other two, with a projected outward speed <10 km s-1. This event corresponds to the leading edge of a ‘streamer blowout’ type of CME. A dark void is left behind in the emission-line
corona following each of the fast eruptions. Both fast emission-line transients start off as a loop structure rising up from
close to the solar surface. We suggest that the driving mechanism for these events may be the emergence of new bipolar magnetic
regions on the surface of the Sun, which destabilize the ambient corona and cause an eruption. The possible relationship of
these events to recent X-ray observations of CMEs is briefly discussed.
Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1004981125702 |
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