Volume 434, Number 1, April IV 2005
|Page(s)||329 - 341|
|Published online||01 April 2005|
Early signatures of large-scale field line opening
Multi-wavelength analysis of features connected with a “halo” CME event
Tuorla Observatory/Department of Physics, University of Turku, 21500 Piikkiö, Finland e-mail: email@example.com
2 LESIA, UMR CNRS 8109, Observatoire de Paris, 5 place J. Janssen, 92195 Meudon, France e-mail: firstname.lastname@example.org
3 Dept. of Physics & Astronomy, University of Glasgow, Glasgow G12 8QQ, Scotland, UK e-mail: email@example.com
4 Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens, 15784 Panepistimiopolis Zografos, Athens, Greece e-mail: firstname.lastname@example.org
Accepted: 13 December 2004
A fast “halo”-type coronal mass ejection (CME) associated with a two-ribbon flare, GOES class M 1.3, was observed on February 8, 2000. Soft X-ray and EUV images revealed several loop ejections and one wave-like moving front that started from a remote location, away from the flare core region. A radio type-II burst was observed near the trajectory of the moving soft X-ray front, although association with the CME itself cannot be ruled out. Large-scale dimmings were observed in EUV and soft X-rays, both in the form of disappearing transequatorial loops. We can pinpoint the time and the location of the first large-scale field-line opening by tracing the electron propagation paths above the active region and along the transequatorial loop system, in which large-scale mass depletion later took place. The immediate start of a type-IV burst (interpreted as an upward moving structure) which was located over a soft X-ray dimming region, confirms that the CME had lifted off. We compare these signatures with those of another halo CME event observed on May 2, 1998, and discuss the possible connections with the “magnetic breakout” model.
Key words: Sun: flares / shock waves / Sun: coronal mass ejections
© ESO, 2005
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