BackForwardInstrument:  GGAK-E/SKL-E 

Instrument details
Acronym GGAK-E/SKL-E
Full name GGAK-E / Solar cosmic rays spectrometer
Purpose To measure electrons and protons in the solar cosmic rays
Short description Spectrometer for energy fluxes in the ranges 0.2-20 MeV (electrons) and 3.5-320 MeV (protons)
Background Part of the GGAK-E (Heliogeophysical Instrument Complex on Electro-L) package, also confirmed for Electro-M (GGAK-E/M) and adapted to Arctica (GGAK-E/A)
Scanning Technique Sun pointing from GEO
Resolution N/A (full disk)
Coverage / Cycle Full solar disk, near continous
Mass Power Data Rate

 

Providing Agency Roscosmos
Instrument Maturity Flown on operational programme
Utilization Period: 2012-01-15 to ≥2039
Last update: 2017-06-05
Detailed characteristics
Satellites this instrument is flying on

Note: a red tag indicates satellites no longer operational, a green tag indicates operational satellites, a blue tag indicates future satellites

Instrument classification
  • Solar and space environment monitors
  • Energetic particle spectrometer
Mission objectives
Primary mission objectives
  • Electron differential directional flux
  • Proton differential directional flux
Secondary mission objectives
  • Solar wind density
  • Solar wind temperature
  • Solar wind velocity
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Tentative Evaluation of Measurements

The following list indicates which measurements can typically be retrieved from this category of instrument. To see a full Gap Analysis by Variable, click on the respective variable.

Note: table can be sorted by clicking on the column headers
VariableRelevance for measuring this variableOperational limitationsExplanation
Electron differential directional flux4 - fairNo specific limitation.Sun pointing, medium and high energy (over 40 to over 400 keV)
Proton differential directional flux4 - fairNo specific limitation.Sun pointing, high energy (over 1000 keV)
Solar wind density2 - very highNo specific limitation.Solar viewing. Inferred by elecron and proton spectroscopy
Solar wind temperature2 - very highNo specific limitation.Solar viewing. Inferred by elecron and proton spectroscopy
Solar wind velocity2 - very highNo specific limitation.Solar viewing. Inferred by elecron and proton spectroscopy