Coronal mass ejections, magnetic clouds, and relativistic magnetospheric electron events: ISTP

• Published in: Journal of Geophysical Research: Space Physics Vol. 103; no. A8; pp. 17279 - 17291
• Main Authors: Baker, D. N., Pulkkinen, T. I., Li, X., Kanekal, S. G., Blake, J. B., Selesnick, R. S., Henderson, M. G., Reeves, G. D., Spence, H. E., Rostoker, G.
• Format: Journal Article
• Language: English
• Published: Blackwell Publishing Ltd 01-08-1998
• ISSN: 0148-0227; 2156-2202
• DOI: 10.1029/97JA03329

The role of high‐speed solar wind streams in driving relativistic electron acceleration within the Earth's magnetosphere during solar activity minimum conditions has been well documented. The rising phase of the new solar activity cycle (cycle 23) commenced in 1996, and there have recently been a number of coronal mass ejections (CMEs) and related “magnetic clouds” at 1 AU. As these CME/cloud systems interact with the Earth's magnetosphere, some events produce substantial enhancements in the magnetospheric energetic particle population while others do not. This paper compares and contrasts relativistic electron signatures observed by the POLAR, SAMPEX, Highly Elliptical Orbit, and geostationary orbit spacecraft during two magnetic cloud events: May 27–29, 1996, and January 10–11, 1997. Sequences were observed in each case in which the interplanetary magnetic field was first strongly southward and then rotated northward. In both cases, there were large solar wind density enhancements toward the end of the cloud passage at 1 AU. Strong energetic electron acceleration was observed in the January event, but not in the May event. The relative geoeffectiveness for these two cases is assessed, and it is concluded that large induced electric fields (∂B/∂t) caused in situ acceleration of electrons throughout the outer radiation zone during the January 1997 event.