Next Generation Radiation Monitor
For Space Weather. NGRM 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.
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.
More details: https://space-env.esa.int/r-and-d/instrumentation/ngrm-next-generation-radiation-monitor/
This sensor is mounted on several ESA/EUMETSAT satellites in support of space weather applications.
Coverage / Cycle
Flown on operational programme
2019 to ≥2027
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
Solar and space environment monitors Energetic particle spectrometer
Subcomponent 1 Electron sensor at GEO Proton sensor at GEO Heavy ion sensor at GEO Electron sensor at LEO Proton sensor at LEO Heavy ion sensor at LEO
Primary mission objectives
Electron differential directional flux Proton differential directional flux Secondary mission objectives Solar wind density Solar wind temperature Solar wind velocity Show all Show fewer
Tentative Evaluation of Measurements
The following list indicates which measurements can
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
Variable Relevance for measuring this variable Operational limitations Explanation
Electron differential directional flux 4 - fair No specific limitation. Sun pointing, medium and high energy (over 40 to over 400 keV)
Proton differential directional flux 4 - fair No specific limitation. Sun pointing, medium and high energy (over 40 to over 1000 keV)
Solar wind density 2 - very high No specific limitation. Solar viewing. Inferred by elecron and proton spectroscopy
Solar wind temperature 2 - very high No specific limitation. Solar viewing. Inferred by elecron and proton spectroscopy
Solar wind velocity 2 - very high No specific limitation. Solar viewing. Inferred by elecron and proton spectroscopy