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Space Weather


SVS >> Space Weather
Movie ID Title
As the CME moves out, the leading edge appears bright while the trailing edge appears dark in difference images. 3406 STEREO Coronal Mass Ejection: From the EUVI to HI-2
Opening with a view of the aurora borealis, we zoom out to reveal the proposed orbital configuration of the five THEMIS satellites and fade in a GGCM magnetosphere model. 3356 THEMIS Mission and Substorm Simulation
Push-in through the plasmasphere to view ionospheric electron enhancements. 3317 Zoom-in to plasmapause-induced TEC enhancement - April 2001
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
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
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
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 snapshot of a high-intensity time in the storm. The bright linear structure in the upper left is an artifact created by the edge of the instrument field-of-view. 2964 IMAGE Views of the Aurora from Space
The particle flux increases dramatically over the polar cap, as they are carried Earthward along the magetic field lines. 2963 The NOAA POES Satellite Detects Record Particle Flows into the Earth's Upper Atmosphere
In the case of low solar wind pressure, the sunward side of the ionosphere is thick (the red region) and some of the atmosphere can be seen trailing off behind the planet. 2962 Computer Simulations of the Martian Atmosphere Interacting with the Solar Wind
10104 Substorms

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