Post-Eruption Arcades and Interplanetary Coronal Mass Ejections

We compare the temporal and spatial properties of posteruption arcades (PEAs) associated with coronal mass ejections (CMEs) at the Sun that end up as magnetic cloud (MC) and non-MC events in the solar wind. We investigate the length, width, area, tilt angle, and formation time of the PEAs associated...

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Bibliographic Details
Published in:Solar physics 2013-05, Vol.284 (1), p.5-15
Main Authors: Yashiro, S., Gopalswamy, N., Mäkelä, P., Akiyama, S.
Format: Article
Language:English
Subjects:
Astrophysics and Astroparticles
Atmospheric Sciences
Corona
Fluctuations
Flux-Rope Structure of Coronal Mass Ejections
Magnetic fields
Physics
Physics and Astronomy
Solar flares
Solar physics
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Spacecraft
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Summary:We compare the temporal and spatial properties of posteruption arcades (PEAs) associated with coronal mass ejections (CMEs) at the Sun that end up as magnetic cloud (MC) and non-MC events in the solar wind. We investigate the length, width, area, tilt angle, and formation time of the PEAs associated with 22 MC and 29 non-MC events and we find no difference between the two populations. According to current ideas on the relation between flares and CMEs, the PEA is formed together with the CME flux-rope structure by magnetic reconnection. Our results indicate that at the Sun flux ropes form during CMEs in association with both MC and non-MC events; however, for non-MC events the flux-rope structure is not observed in the interplanetary space because of the geometry of the observation, i.e. the location of the spacecraft when the structure passes through it.
ISSN:0038-0938
1573-093X
DOI:10.1007/s11207-013-0248-1