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ISO trapped particle environment

The following plots of trapped proton and electron fluxes in the ISO orbit are based on the static AP8 and AE8 models (accessible, e.g. via the SPENVIS package) corresponding to solar minimum and maximum conditions, respectively. The year 1996 has been chosen here for the solar minimum condition case, which is recommended to be used in any ISO radiation effect calculations. Solar maximum results are included for comparison only.

 

Solar minimum conditions (use these for calculations) Solar maximum conditions

Electrons

 

AE8 trapped electron positional fluxes AE8 trapped electron positional fluxes
AE8 trapped electron orbit averaged spectra AE8 trapped electron orbit averaged spectra

Protons

 

AP8 trapped proton positional fluxes AP8 trapped proton positional fluxes
AP8 trapped proton orbit averaged spectra AP8 trapped proton orbit averaged spectra

Note that the AP8 and AE8 models yield averaged values and are therefore not able to reproduce the dynamic nature of especially the outer electron belt environment. Electron, proton, and X-ray data from these other experiments are here included:

Additionally, absorbed radiation dose data as a function of ISO orbit time is available:

Figure 1. AE8 trapped electron integral fluxes >200 keV and >2 MeV in the ISO orbit for solar minimum conditions.

Figure 2. AE8 averaged trapped electron spectra in the ISO orbit for solar minimum conditions.

Figure 3. AP8 trapped proton integral fluxes >10 MeV and >100 MeV in the ISO orbit for solar minimum conditions.

Figure 4. AP8 averaged trapped proton spectra in the ISO orbit for solar minimum conditions.

Figure 5. AE8 trapped electron integral fluxes >200 keV and >2 MeV in the ISO orbit for solar maximum conditions.

Figure 6. AE8 averaged trapped electron spectra in the ISO orbit for solar maximum conditions.

Figure 7. AP8 trapped proton integral fluxes >10 MeV and >100 MeV in the ISO orbit for solar maximum conditions.

Figure 8. AP8 averaged trapped proton spectra in the ISO orbit for solar maximum conditions.

For questions, comments, and further information, please contact P. Nieminen at ESA/ESTEC.

 

 

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