|Reference : Hot-cold plasma interactions and the generation of transient dayside sub-auroral proton ...|
|Scientific congresses and symposiums : Unpublished conference|
|Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics|
|Hot-cold plasma interactions and the generation of transient dayside sub-auroral proton precipitation|
|Fuselier, S. A. [Lockheed Martin ATC, 3251 Hanover St Dept L9-42, Bldg 255, Palo Alto, CA 94304 United States;]|
|Gary, S. P. [Los Alamos National Laboratory, NIS-1 MS D466, Los Alamos, NM 87545 United States;]|
|Thomsen, M. F. [Los Alamos National Laboratory, NIS-1 MS D466, Los Alamos, NM 87545 United States;]|
|Claflin, E. S. [Lockheed Martin ATC, 3251 Hanover St Dept L9-42, Bldg 255, Palo Alto, CA 94304 United States;]|
|Hubert, Benoît [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP) >]|
|Immel, T. J. [Space Sciences Laboratory, University of California, Berkeley, Berkeley, CA 94720 United States;]|
|Sandel, B. R. [Lunar and Planetary Laboratory, University of Arizona 1040 East Fourth Street, Room 901, Tucson, AZ 85721 United States;]|
|[en] 2139 Interplanetary shocks ; 2736 Magnetosphere/ionosphere interactions ; 2778 Ring current ; 7867 Wave/particle interactions|
|[en] The IMAGE spacecraft obtained the first global images of the proton aurora. One of the discoveries from these images was proton precipitation equatorward of the nominal auroral oval. This precipitation can be observed for approximately 10 minutes immediately following a large solar wind pressure pulse. Various mechanisms have been proposed for producing this precipitation. Here, precipitation due to scattering from electromagnetic ion cyclotron (EMIC) waves is investigated using data from the IMAGE FUV and EUV imagers and in situ data from the Los Alamos geosynchronous spacecraft. In the proposed EMIC wave mechanism, the compression of the dayside magnetosphere enhances the growth rate of the wave instability. These waves scatter hot, ring current protons into the atmospheric loss cone, reducing the proton temperature anisotropy (the free energy source of the waves). Two features of the proton precipitation from these waves require explanation. First, the precipitation pattern may peak at any local time on the dayside between about 09 and 15. Second, the precipitation pattern has limited latitudinal extent (typically less than about 10 degrees) and is often separated from the main auroral oval. The local time peak in the precipitation pattern is related to the characteristics of the solar wind pressure pulse that causes EMIC wave growth. The separation of the precipitation pattern from the main auroral oval is related to properties of the hot and cold plasma within the magnetosphere that enhance EMIC wave growth.|
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