Polar UVI and THEMIS GBO Observations of the Ionospheric and Magnetospheric Response to a Hot Flow Anomaly

Details Polar UVI and THEMIS GBO Observations of the Ionospheric and Magnetospheric Response to a Hot Flow Anomaly Polar UVI and THEMIS GBO Observations of the Ionospheric and Magnetospheric Response to a Hot Flow Anomaly

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm53a1649f&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM53A-1649

Physics

2435 Ionospheric Disturbances, 2704 Auroral Phenomena (2407), 2721 Field-Aligned Currents And Current Systems (2409), 2736 Magnetosphere/Ionosphere Interactions (2431), 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

We present observations of the ionospheric response to a hot flow anomaly (HFA) interacting with the magnetosphere. On 4 July 2007, the THEMIS spacecraft observed a HFA on both sides of the bow shock. The ionospheric response was measured by global auroral images taken over the southern hemisphere by Polar UVI, by ground based magnetometers and photometers in Antarctica, and by the THEMIS Ground Based Observatories (GBOs) in the northern hemisphere. Polar UVI observations show a region of enhanced auroral emission in the morning sector about 10 minutes after the THEMIS spacecraft observed the HFA. This region of enhanced emission was located above South Pole station which observed an increase in the auroral luminosity and magnetic perturbations. The THEMIS GBOs in the conjugate hemisphere also observed magnetic perturbations consistent with a traveling convection vortex. Polar UVI tracked the spatial and temporal development of the region of enhanced emission. Slow anti-sunward motion was observed as the emission weakened and then re-brightened over the course of about 10 minutes. Simultaneously, the THEMIS GBO array observed anti-sunward motion of the magnetic impulse with a velocity much greater than that of the auroral emission. The origin of the magnetic perturbation and resulting auroral emission is suggested to be the deformation of the magnetopause due to the HFA-magnetosphere interaction. The different propagation speeds of the auroral emission in the southern hemisphere and the magnetic perturbation in the northern hemisphere imply either 1) a decoupling of the auroral emission and field-aligned current signature or 2) a decoupling of these processes between the two hemispheres. The large difference in the ionospheric conductivity between the northern (summer) and southern (winter) hemispheres may be an important factor in this decoupling.

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