Physics
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..426s&link_type=abstract
Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 426
Physics
4
Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Planetary Bow Shocks, Interplanetary Shocks
Scientific paper
Since the first observations of solar mass ejection events in the early seventies by OSO 7 and Skylab, a few thousand of these remarkable dynamic incidents have been observed, covering about two full solar activity cycles. The mass ejecta mainly include hot coronal plasma and cold prominence material in variable amounts. This is the reason why the often used term CME (for coronal mass ejection) should be replaced by the more neutral term SME (solar mass ejection). The ejecta are often recognized in the form of interplanetary plasma clouds detected in the distant solar wind by appropriately located spacecraft. Clouds which have been energetic enough to drive large scale interplanetary shock waves can be identified most readily, but clouds without associated shocks do also occur. Plasma clouds can be characterized by a variety of signatures, indicating that they actually originate from injections of different material into the ambient solar wind. Quite a few crucial problems still remain to be addressed by the upcoming SOHO mission.
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