Note: CMIT-LFM simulation runs submitted before October 31, 2018 used solar wind data propagated to the model run's upstream (sunward) boundary (typically at X_max=30 R_E).
However, the model assumes solar wind to be propagated to X=0 instead, causing features in the solar wind to occur in the LFM model simulation a few minutes earlier than expected (for example, 8 minutes earlier for V_x=-400 km/s and X_max=30 R_E).
The propagation has been adjusted in the run request system for "event" runs with CMIT-LFM where solar wind data are obtained automatically from one of the available solar wind monitor spacecraft or data sources (solar wind data in uploaded file are not propagated and need to be adjusted before file upload to make LFM runs comparable to runs of the other magnetosphere models).

Output Data

View Magnetosphere

Create Timeseries in Magnetosphere

View 2D Ionosphere Electrodynamics

New: Create Timeseries in 2D Ionosphere

• View pre-computed timeseries data:
  • Northern hemisphere polar cap flux and area
  • Southern hemisphere polar cap flux and area
  • Magnetopause standoff and closest approach within 30 deg. of Sun-Earth line (local noon)
  • Polar cap boundary at 24 magnetic local times in northern hemisphere
  • Polar cap boundary at 24 magnetic local times in southern hemisphere
  • Ionospheric dissipation
  • View Quick look graphics for the run
  View model outputs along satellite trajectories (result of postprocessing on usually longer magnetosphere 3D output time cadence):
  • Cluster-1
  • Cluster-2
  • Cluster-3
  • Cluster-4
  • Moon

• Perform model data comparison for this run using VMR tools (formerly the Virtual Model Repository at the University of Michigan)

Quick Look Graphics (?)

• Click on an image to view it in full size
• Quick look graphics has been designed by the model developers to enable quick evaluation of the results of the run. To find more information regarding this option please contact the CCMC staff.