Reference : Two types of localized auroral UV emission on the dayside

	Document type :	Scientific congresses and symposiums : Unpublished conference
	Discipline(s) :	Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
	To cite this reference:	http://hdl.handle.net/2268/33848

Title :	Two types of localized auroral UV emission on the dayside
Language :	English
Author, co-author :	Frey, H. U. [UC Berkeley, SSL, Berkeley, CA 94720 United States ;]
	Mende, S. B. [UC Berkeley, SSL, Berkeley, CA 94720 United States ;]
	Immel, T. J. [UC Berkeley, SSL, Berkeley, CA 94720 United States ;]
	Gérard, Jean-Claude [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP) >]
	Hubert, Benoît [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP) >]
	Fuselier, S. A. [LMMS, ATC, Palo Alto, CA 94304 United States ;]
Publication date :	1-Dec-2001
Audience :	International
Event name :	Fall Meeting 2001
Event organizer :	American Geophysical Union
Keywords :	[en] 2704 Auroral phenomena (2407) ; 2716 Energetic particles ; precipitating ; 2724 Magnetopause ; cusp ; and boundary layers ; 2784 Solar wind/magnetosphere interactions
Abstract :	[en] The FUV instrument on IMAGE frequently observes localized ultraviolet emission on the high latitude dayside, poleward of the normal auroral oval. There are two different types of these localized emissions. One is especially distinct in the observations of Doppler shifted Lyman alpha emission from proton precipitation. This type occurs during northward IMF and high solar wind dynamic pressure. We interpret this emission as the optical signature of proton precipitation into the cusp after lobe reconnection at the magnetopause. The second type of localized emission is visible in the wide-band (WIC) and oxygen (SI13) imagers, but is absent in the proton imager. This emission occurs during northward IMF but very low solar wind density and dynamic pressure. We interpret this emission as the optical signature of electron acceleration after reconnection.
Target :	Professionals ; Researchers
Permalink :	http://hdl.handle.net/2268/33848
	also: http://hdl.handle.net/2268/61419
Other URL :	http://adsabs.harvard.edu/abs/2001AGUFMSM31B0761F

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