“NetPICOMAG: a low-cost turn-key magnetometer for aurora detection”

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