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Refilling of the Plasmasphere as seen by IMAGE EUV Bill R. Sandel & William T. Forrester

Refilling of the Plasmasphere as seen by IMAGE EUV Bill R. Sandel & William T. Forrester Lunar and Planetary Laboratory The University of Arizona. Introduction. Refilling of the plasmasphere—the ionosphere tries to establish equilibrium.

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Refilling of the Plasmasphere as seen by IMAGE EUV Bill R. Sandel & William T. Forrester

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  1. Refilling of the Plasmasphere as seen by IMAGE EUV Bill R. Sandel & William T. Forrester Lunar and Planetary Laboratory The University of Arizona

  2. Introduction Refilling of the plasmasphere—the ionosphere tries to establish equilibrium. A topic legitimized by its durability, having been discussed at the first Yosemite Meeting. Lots of modeling and measurements before and since then. Recent ground-based measurements (e.g. ULF resonance techniques) Recent satellite measurements (Reinisch et al. JGR 2004, Huegerich et al., (Yosemite 2002), Smith et al. (Yosemite 2004)). IMAGE EUV can contribute a global view, and sample many radial profiles simultaneously. IMAGE EUV cannot directly attack the important problem of the distribution of plasma along field lines.

  3. Solar Wind and Magnetic Activity A moderate erosion event followed by quiet conditions leads to an example of refilling unconfused by other phenomena. 26 June 1 July

  4. 2001-177/10:00 (-15 h) 2001-178/01:30 (0 h) 2001-178/14:30 (+13 h)

  5. 2001-179/05:30 (+28 h) 2001-179/18:30 (+42 h) 2001-180/08:30 (+55 h)

  6. 2001-180/22:30 (+69 h) 2001-181/11:30 (+82 h)

  7. Binning 0.5 L Variable in magnetic longitude 2001-179/05:30 (+28 h)

  8. Computing Refilling Rate from Column Abundance Curves: Fake inversion to obtain equatorial density Use an effective path length Weakly L-dependent Depends on radial distribution of plasma Difference the equatorial densities, divide by time

  9. +00 h +13 h +28 h +41 h +55 h +69 h

  10. Chi et al., GRL preprint Wilson et al., JGR, 92 Sojka & Wrenn, 1985 Inferred Refilling Rates +00 h +13 h +28 h +41 h +55 h +69 h

  11. +00 h +13 h +28 h +41 h +55 h +69 h

  12. +00 h +13 h +28 h +41 h +55 h +69 h

  13. +00 h +13 h +28 h +41 h +55 h +69 h

  14. Conclusions IMAGE EUV observations can be used to estimate refilling rates in the plasmasphere. EUV may be able to contribute a new perspective on the question. Initial results from an azimuthal average are roughly consistent with the conventional wisdom from models and previous measurements. Global imaging reveals important departures from average conditions that may reflect structure in the ionosphere.

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