BackForwardInstrument:  RMU 

Instrument details
Acronym RMU
Full name Radiation Monitor Unit (also referred to as NGRM)
Purpose For Space Weather. RMU measures protons from 2 MeV up to 200 MeV, electrons from 100 keV up to 7 MeV as well as the Linear Energy Transfer spectrum of ions.
Short description

Direction sensitive particle spectroscopy for: - electrons (e-) in the energy ranges of 0.1 to 7 MeV; 8 quasi-logarithmic channels - protons (p+) in the energy ranges 2 to 200 MeV; 8 quasi-logarithmic channels - Heavy Ions: LET spectrum 0.1 to 10 MeV cm²/mg; 8 quasi-logarithmic channels. 
Background

This sensor is mounted on several ESA/EUMETSAT satellites in support of space weather applications.
Scanning Technique

N/A
Resolution N/A
Coverage / Cycle N/A
Mass 1.17 kg Power 1 W Data Rate

 

Providing Agency ESA
Instrument Maturity Flown on operational programme
Utilization Period: 2019 to 2046
Last update: 2024-03-04
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
WIGOS Subcomponents No WIGOS subcomponents have been defined.
Mission objectives
Primary mission objectives
  • Electron differential directional flux
  • Proton differential directional 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
Electron differential directional flux*4 - fairNo specific limitation.Sun pointing, medium and high energy (over 40 to over 400 keV)
Proton differential directional flux*4 - fairNo specific limitation.Sun pointing, medium and high energy (over 40 to 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