Various Aspect of the Field Line Resonance Phenomena Observed at the South Pole Station

Details Various Aspect of the Field Line Resonance Phenomena Observed at the South Pole Station Various Aspect of the Field Line Resonance Phenomena Observed at the South Pole Station

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm43a1909t&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM43A-1909

Physics

[2407] Ionosphere / Auroral Ionosphere, [2431] Ionosphere / Ionosphere/Magnetosphere Interactions, [2704] Magnetospheric Physics / Auroral Phenomena, [2736] Magnetospheric Physics / Magnetosphere/Ionosphere Interactions

Scientific paper

We investigate a relationship among quasi-stationary auroral patches (QSAPs), Pc 5 pulsations, and poleward moving auroral arcs (PMAAs) simultaneously observed with all-sky imagers and fluxgate magnetometer at the South Pole Station (-74.3CGLAT) on July 8, 2004, and interpret it in terms of the field line resonance (FLR) theory. This is the second step of the research by Ebihara et al. (J. Geophys. Res., 112, A01201, 2007). Ebihara et al. (2007) reported that QSAPs observed at the South Pole Station in the interval 9-14 MLT kept their form, location, and luminosity for up to several hours. The QSAPs showed periodic fluctuations of their drift velocity and the fluctuations were well correlated with Pc 5 pulsations. It was also demonstrated that the relationship between the drift velocity of QSAPs (corresponding to the ionospheric electric filed) and Pc 5 pulsations was explained quantitatively by the Ohm's law in the ionosphere. In this study, we further analyzed the poleward moving auroral arcs (PMAAs) appeared simultaneously during this period. The PMAAs showed one-to-one correspondence with Pc 5 pulsations. Further, it was found that the drift velocity of QSAPs was primarily eastward on the high-latitude side of PMAAs and westward on the low-latitude side. To interpret the observed results, we calculated the magnetosphere - ionospheric coupling process by the numerical simulation. It was assumed that the FLR occurred in the magnetosphere and the Alfven waves expected from the FLR were incident on the ionosphere. We used a simplified two-dimensional model, but it includes the auroral acceleration region and the ionosphere with the realistic conductivity. The ionospheric conductivity is changed by the electron precipitations due to the QSAPs and the PMAAs. The simulation results were qualitatively consistent with the observed relationship among the fluctuations of QSAPs, Pc 5 pulsations, and PMAAs. Therefore, it was concluded that the QSAP’s fluctuations, Pc 5 pulsations, and PMAAs are the various aspects of the FLR phenomena.

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