Reference : Electron and Proton Auroral Dynamics
Scientific congresses and symposiums : Unpublished conference
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/61422
Electron and Proton Auroral Dynamics
English
Mende, S. B. mailto [Space Sciences Laboratory, University of California, Berkeley, Centennial Drive at Grizzly Peak Blvd, Berkeley, CA 94720 United States ;]
Frey, H. U. [Space Sciences Laboratory, University of California, Berkeley, Centennial Drive at Grizzly Peak Blvd, Berkeley, CA 94720 United States ;]
Carlson, C. [Space Sciences Laboratory, University of California, Berkeley, Centennial Drive at Grizzly Peak Blvd, Berkeley, CA 94720 United States ;]
Immel, T. [Space Sciences Laboratory, University of California, Berkeley, Centennial Drive at Grizzly Peak Blvd, Berkeley, CA 94720 United States ;]
Gérard, Jean-Claude mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP) >]
Hubert, Benoît mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP) >]
Fuselier, S. [Lockheed-Martin Palo Alto Research Laboratories, 3251 Hanover Street, Palo Alto, CA 94304 United States ;]
Spann, J. [NASA HQ Code SR, Cod SR, Washington, DC, 20546 United States ;]
Gladstone, R. [Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228 United States ;]
Burch, J. L. [Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78228 United States ;]
1-May-2001
No
International
[en] 2704 Auroral phenomena (2407) ; 2716 Energetic particles ; precipitating ; 2784 Solar wind/magnetosphere interactions ; 2788 Storms and substorms
[en] Data from the IMAGE Wide-band Imaging Camera (WIC),sensitive to far ultraviolet auroras and from the Spectrographic Imager (SI) channel SI12, sensitive to proton precipitation induced Lyman alpha, were analyzed during a high altitude orbit segment of the IMAGE spacecraft. This segment began during the expansive phase of a substorm. The aurora developed into a double oval configuration, consisting of a set of discrete poleward forms and a separate diffuse auroral oval equatorwards. Although IMF Bz was negative, considerable activity could be seen poleward of the high latitude arcs in the polar cap region. The optical signature of precipitating protons showed that the proton aurora was on the equatorward side of the diffuse aurora and there was a lack of intense energetic proton fluxes in the poleward arcs. A simultaneous FAST pass provided a diagnostic of the particle types in the various regions. These data showed that lower intensity protons were present throughout the entire double oval configuration but with insufficient intensity to produce aurora that could be observed by IMAGE. The FAST data also showed that the bright poleward discrete arcs were accelerated by electrostatic processes, and the wave accelerated electrons were located on the poleward edge of these features.
http://hdl.handle.net/2268/61422
http://adsabs.harvard.edu/abs/2001AGUSM..SM22B07M

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