BackForwardInstrument:  MUSE 

Instrument details
Acronym MUSE
Full name Monitor of Ultraviolet Solar Energy
Purpose To observe time variations of the UV solar radiation
Short description UV radiometer operating in five channels: 121.6 nm (H Lyman-alpha), 180 nm, 210 m, 260 nm and 280 nm, indicative of several processes in the solar chromosphere and photosphere
Background The channels in the unit of Nimbus-4 were slightly different from those on Nimbus-3: channels 210 and 280 nm replaced 160 and 200 nm, that did not work properly
Scanning Technique Sun pointing from a sunsynchronous orbit
Resolution N/A (full disk)
Coverage / Cycle Full disk in 50 s
Mass Power Data Rate

 

Providing Agency NASA
Instrument Maturity Flown on an R&D satellite
Utilization Period: 1969 to 1980
Last update: 2017-05-19
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
  • Solar activity monitor
WIGOS Subcomponents
  • Subcomponent 2
  • Solar magnetograph, solar EUV/X-ray imagery and EUV/X-ray irradiance, both on the Earth-Sun line and off the Earth-Sun line
  • Solar UV imager [from L1, GEO, LEO]
Mission objectives
Primary mission objectives
  • Solar Lyman-alpha flux
  • Solar UV flux
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
Note: * Primary mission objective.
VariableRelevance for measuring this variableOperational limitationsExplanation
Solar Lyman-alpha flux*2 - very highNo specific limitation.H-Ly-alpha at 121.6 nm (EUV/UV boundary)
Solar UV flux*2 - very highNo specific limitation.Several channels, moderate dynamic range