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Tom Bridgman
Movie   ID   Title
Plasmasphere plume passes and we see the electron enhancement move across Canada and the U.S. (no dates)   3316   Zoom-in to plasmapause-induced TEC enhancement - April 2001 (Version 2)
Equatorial view of the plasmapause.   3315   Tour of the Plasmapause - April 2001
Plasmasphere plume extending along the Earth's geomagnetic field lines.   3314   Time-varying Plasmapause and Electron data - April 2001
View of the electron enhancement plume across the northeastern U.S. and up through Canada.   3313   Ionosphere Total Electron Content - November 2003
The plasmasphere during the storm. The plume is the structure to the right, constrained to move along the magnetic field lines.   3312   The 'Big Picture' View of the Plasmapause and Ionospheric Electron Content - April 2001
The plasmasphere plume passes below the observer, enhancing the electron content of the ionosphere below it (no dates).   3311   Zoom-in to plasmapause-induced TEC enhancement - April 2001
The high electron density plume (dark red) sweeps over the U.S and Canada.   3310   Ionosphere Total Electron Content - April 2001
Another angle of the model showing a number of active regions.   3287   Rotating Tour of Solar Coronal Loops
We pass over another group of active regions.   3286   Flight through the Coronal Loops
NASA's Earth Observing Fleet   3227   NASA's Orbiting Earth Observing Fleet (improved background)
The PFSS model is a poor match for the TRACE coronal loops.   3212   Space Weather Forecasting: Active Times Ahead
In this case, we see the PFSS model matches the TRACE coronal loops very well.   3211   Space Weather Forecasting: Quiet Times Ahead
VIDEO WITH MUSIC AND CAPTIONS   3181   A Tour of the Cryosphere
Closeup of AR 10720. Blue high-energy emission marks the footpoints of the coronal loops. The lower-energy red emission is from the loop structure. See note below under ImageMods.   3162   RHESSI and TRACE View of January 20, 2005 Solar Flare
TRACE ultraviolet view of AR 10720   3161   TRACE Ultraviolet View of January 20, 2005 Solar Flare
AR 10720 launches a flare.   3160   January 2005 Solar Flares from SOHO/EIT
The CME in question is so fast, it appears in only one LASCO/C2 camera frame.   3159   SOHO/LASCO View of January 2005 Solar Events
More energetic electrons are cleared out, created a more well-defined gap between the belts.   3115   Gaps in the Earth's Radiation Belts
Four months of TGFs as seen by RHESSI.   3111   Connections: Terrestrial Gamma Flashes and Lightning?
As the belts return to their quiescent state, radiation levels at the satellite decrease.   3052   Earth's Radiation Belts with Safe Zone Orbit
A portion of the plasmasphere convects out to the magnetopause where it terminates.   3051   Plasmapause Convects to the Magnetopause During Halloween Solar Storm
A view of the plasmasphere above the north geographic pole.   3050   Tour of the Plasmasphere and Plasmapause
As particle-induced electric fields increase, the low-energy electrons of the plasmasphere are convected towards the magnetopause, depleting the region near the Earth and enabling the hotter particles from the radiation belts to move closer to the Earth.   3049   Radiation Belts and Plasmapause Fluctuate Under Solar Storm
During the pre-storm time, the inner region of the belts has a relatively low particle flux and for this scaling of the data, a distinct inner belt is not visible as a separate structure.   3048   Earth's Radiation Belts Tremble Under Impact of Solar Storm
A rendering of the model of the Earths magnetosphere. The flat ribbons represent charged particles entering the influence of the magnetosphere and being deflected. The curved lines visible to the right represent the magnetic field lines extending out from the Earth. The force from the sun pushes these lines into a distinctive tail-like shape. Finally, the green surface represents a constant value for the magnetic field strength.   3028   A 3-Dimensional Model of the Magnetosphere (WMS)

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