On interplanetary coronal mass ejection identification at 1 AU
- Institute of Geophysics and Planetary Physics and the Department of Earth and Space Sciences University of California Los Angeles (United States)
- Los Alamos National Laboratory, Los Alamos, New Mexico (United States)
Coronal mass ejections are believed to be produced in the corona from closed magnetic regions not previously participating in the solar wind expansion. At 1 AU their interplanetary counterparts (ICMEs) generally have a number of distinct plasma and field signatures that distinguish them from the ambient solar wind. These include heat flux dropouts, bi-directional streaming, enhanced alpha particle events, times of depressed proton temperatures, intervals of distorted or enhanced magnetic field, and times of large magnetic field rotations characteristic of magnetic clouds. The first three of these signatures are phenomena that occur at some point within the ICME, but do not necessarily persist throughout the entire ICME. The large scale magnetic field rotations, distortions and enhancements, and the proton temperature depressions tend to mark more accurately the beginning and end of the ICME proper. We examine herein the reliability with which each of these markers identifies ICMEs utilizing ISEE-3 data from 1978{endash}1980. {copyright} {ital 1999 American Institute of Physics.}
- OSTI ID:
- 679160
- Report Number(s):
- CONF-9810104-; ISSN 0094-243X; TRN: 99:009354
- Journal Information:
- AIP Conference Proceedings, Vol. 471, Issue 1; Conference: 9. international conference on solar wind, Nantucket, MA (United States), 5-9 Oct 1998; Other Information: PBD: Jun 1999
- Country of Publication:
- United States
- Language:
- English
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