Multi-point observations of large-amplitude electric fields during substorms obtained by THEMIS

Details Multi-point observations of large-amplitude electric fields during substorms obtained by THEMIS Multi-point observations of large-amplitude electric fields during substorms obtained by THEMIS

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm41a1685o&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM41A-1685

Physics

[2736] Magnetospheric Physics / Magnetosphere/Ionosphere Interactions, [2790] Magnetospheric Physics / Substorms

Scientific paper

Large-amplitude electric fields over 100 mV/m have been observed around the equatorial magnetosphere. These electric fields may contribute to energy transport and particle acceleration in the magnetosphere [e.g., Wygant et al., 2000, 2002], and seem to be related to fast plasma flows with a size of a few Re [Nakamura et al., 2001]. In order to understand their macroscopic characteristics and the effects to magnetic activities, it is important to observe both fields and particles simultaneously at multiple locations within several Re. Five THEMIS probes can frequently provide such chances. In this paper, we show the several events with large-amplitude electric fields during substorms obtained by THEMIS. One of the events is found in 05:50-06:00 UT on 11 March 2008, when TH-D (Xsm=-10.7 Re, Ysm=4.8 Re) and TH-E (Xsm=-10.3 Re, Ysm=5.6 Re) observed intense electric fields. At 05:54 UT, THEMIS GBO-s clearly showed the auroral onset signature. The great intensification was near the SNKQ station, and this structure moved westward with the speed of ~6 km/s. It corresponds to ~200 km/s, as mapped to the TH-D/E location. The footprints of TH-A (Xsm=-6.8 Re, Ysm=-0.4 Re), D, and E were close to the site of the aurora. The location of TH-D was beside that of TH-E, and TH-A was located earthward and eastward from the former two. The enhanced electric fields observed by TH-D and E were associated with magnetic dipolarization and earthward high-speed plasma flow. They were also associated with the depletion of electron density estimated by the spacecraft potential. These features are consistent with the model of plasma bubbles [e.g., Pontius and Wolf, 1990]. The Y components of plasma flows were 200-300 km/s, roughly consistent with the westward auroral motion as mapped to the equatorial magnetosphere. Also, we found that Poynting flux of low frequency was efficient to illuminate the auroral emissions. This fact suggests that electromagnetic energy is transported to the ionosphere. On the other hand, TH-A also observed the large-amplitude electric field greater than TH-D/E. However, TH-A did not detect the high-speed plasma flow nor the depletion of the electron density. In the drift electric field, VxB, estimated from particle and magnetic field observations, TH-D and E detected intense fields, but TH-A found almost zero. This result shows a difference in the role of the electric fields in location of TH-D/E and TH-A. We will show the possible contribution from other factors, such as pressure gradient, current system, and the ionospheric conductivity.

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