| dc.description | The Monday poster on netPICOmag elicited interest as deduced from people asking UCLA colleagues if we were really able to do what we presented. This is a good sign, but that poster is described in Ian Schofield’s report.
Despite a huge amount of work done before the meeting, it was necessary to take time during the meeting to finalize the poster, which was presented on Thursday. As a deviation from previous practice, which did not seem to lead to easy conversion to the more valuable published paper, this poster was written as a paper. Many of the comments were by co-authors. Valuable input was also had from A. Runov, who is an expert on signatures similar to those observed at the THEMIS spacecraft. At the subsequent THEMIS meeting, useful comments by V. Sergeev will help with tracing of field lines between the Earth and THEMIS regions. It is intended to proceed rather rapidly with the work to a publication, and it is noted that some of the original aspects mentioned in the abstract are in fact secondary, and that the THEMIS B spacecraft was in a rather unique position with regard to the Near-Earth Neutral Line, a significant result that is already under active email discussion with co-authors.
As part of planning discussions at the meeting, the joint plan with University of Calgary and STELAB (Nagoya, Japan) to do optical observations early in 2009 was fleshed out, with our likely participation being at Rabbit Lake, SK. | en |
| dc.description.abstract | AN: SM43A-1686
TI: Solar Wind Influence on the Driven Electrojet System and the Magnetotail
AU: * Connors, M
EM: martinc@athabascau.ca
AF: Athabasca University Geophysical Observatory, 1 University Drive, Athabasca, AB T9S 3A3, Canada
AU: Russell, C
EM: ctrussel@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, UCLA, Los Angeles, CA 90095, United States
AU: McPherron, R
EM: rmcpherron@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, UCLA, Los Angeles, CA 90095, United States
AU: Angelopoulos, V
EM: vassilis@ucla.edu
AF: Institute of Geophysics and Planetary Physics, UCLA, Los Angeles, CA 90095, United States
AU: Glassmeier, K
EM: kh.glassmeier@t-online.de
AF: TU Braunschweig, Mendelssohnstr 3, Braunschweig, 38106, Germany
AU: Rostoker, G
EM: rostoker@space.ualberta.ca
AF: Department of Physics, University of Alberta, Edmonton, AB T6G 2J1, Canada
AU: Boteler, D
EM: DBoteler@NRCan.gc.ca
AF: Natural Resources Canada, 7 Observatory Crescent, Ottawa, ON K1A 0Y3, Canada
AU: Danskin, D
EM: ddanskin@NRCan.gc.ca
AF: Natural Resources Canada, 7 Observatory Crescent, Ottawa, ON K1A 0Y3, Canada
AU: Gleisner, H
EM: hgl@dmi.dk
AF: Section for Geomagnetism & Remote Sensing, Danish Meteorological Institute, Lyngbyvej 100, Copenhagen, DK-2100, Denmark
AU: Keika, K
EM: kunihiro.keika@oeaw.ac.at
AF: Space Research Institute, Austrian Academy of Sciences, Graz, 8042, Austria
AU: Rastaetter, L
EM: Lutz.Rastaetter@nasa.gov
AF: NASA Goddard SFC, Code 674, 8800 Greenbelt Rd, Greenbelt, MD 20771, United States
AU: Donovan, E
EM: edonovan@ucalgary.ca
AF: Department of Astronomy and Physics, University of Calgary, Calgary, AB T2N 1N4, Canada
AB: A substorm onset at approximately 10 UT on December 12 2007 was well observed from both the THEMIS constellation and ground observatories in eastern Canada, most emplaced to support the THEMIS project. Clear step-like changes in the solar wind parameters on this day aid in relating them to magnetospheric responses. With the large set of ground magnetometers available, quantitative inversion can be done using the Automated Regional Modelling (ARM) technique which includes both auroral zone and subauroral stations. Not only can the substorm current wedge parameters be well determined, but the response of the driven system morning electrojet to southward IMF during the growth phase can be quantified. A clear subauroral Y component magnetic bay observed in eastern North America before onset can be attributed to this driving, as can stretching at GOES 11 (W) and evening sector bays. The onset appears to have been triggered by a northward turning. Analysis of tail response to the onset must take into account the fact that simultaneously the solar wind northward velocity component reversed from approximately -30 km/s to +40 km/s. The THEMIS C and B spacecraft, located 12 and 14 Re downtail, respectively, showed slow magnetic field X component reversals around the time of onset that are most likely mainly related to the solar wind Vz velocity blowing the tail across the spacecraft, as opposed to direct effects of the substorm. This result is confirmed by MHD modeling and studied using an event-oriented mapping approach.
DE: 2721 Field-aligned currents and current systems (2409)
DE: 2740 Magnetospheric configuration and dynamics
DE: 2753 Numerical modeling
DE: 2784 Solar wind/magnetosphere interactions
DE: 2790 Substorms
SC: SPA-Magnetospheric Physics [SM]
MN: 2008 Fall Meeting | en |
