Global storm time auroral X-ray morphology and timing and comparison with UV measurements

Details Global storm time auroral X-ray morphology and timing and comparison with UV measurements Global storm time auroral X-ray morphology and timing and comparison with UV measurements

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000jgr...10515757a&link_type=abstract

Journal of Geophysical Research, Volume 105, Issue A7, p. 15757-15778

Physics

14

Ionosphere: Ionospheric Disturbances, Ionosphere: Particle Precipitation, Magnetospheric Physics: Auroral Phenomena, Magnetospheric Physics: Storms And Substorms

Scientific paper

The Polar Ionospheric X-ray Imaging Experiment (PIXIE) on NASA's Polar spacecraft provides the first global images of the auroral oval in X-rays and allows very accurate measurements of the timing of geomagnetic disturbances to a degree of temporal resolution not available from previous imagers due to its photon counting characteristics. On October 19, 1998, a magnetic cloud associated with a CME encountered the Earth's magnetopause near 0500 UT, generating a magnetic storm that reached a minimum value in Dst of -139 nT. The z component of the interplanetary magnetic field (IMF) (Bz) remained remarkably steady for the first 10 hours of the storm as did the solar wind particle pressure. The PIXIE and UVI instruments on the Polar spacecraft were both imaging the auroral oval from 0800 to 1800 UT; six distinct impulsive auroral enhancements were observed by the imagers during this time period. Global imaging combined with geosynchronous particle observations allowed classification of the geomagnetic disturbances associated with the events. Only two of the events were classified as substorms; one was classified as a poleward boundary intensification, one was a convection bay, and one was a pseudobreakup. A sixth event occurred after a dramatic northward turning of the IMF at the end of the 10-hour Bz south period but was very weak and transient. The effects of the northward turning were counteracted by a simultaneous increase in the By component of the IMF. The first sign of significant substorm activity occurred over 8 hours after the cloud encountered the Earth and was not associated with any change in the solar wind magnetic field or particle pressure. The cross polar cap potential remained large (>100 kV), and most of the X-ray emissions observed were associated with enhanced earthward convection caused by large cross-tail electric fields; 50% were collected from the 0000-0600 magnetic local time (MLT) sector.

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