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By Nuclear and Space Radiation Effects Conference Short Course 1997

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Fluxes for E >30 MeV as a function of B/B. for several L values. 2 shows Increasing B/B. represents moving from the magnetic equator down the field line to the mirror point. Notice the sharp cutoff at low L values where particles are close to their mirror points. OrrnidiractimalIntagral l%ton Fluxes ClmichctionalIntegalPm@Fluxesat E >30 at MagneticEquator ‘“’~ — 108 . ----- L= 1,2 107 i. - L= 1,16 ,“...... L= 1,15 105 \ 104 1 \ \ \ \ 103 \ K? 1: Variationof proton flux levels with radial distance.

In these cases, the upset rates will be very high because the intensity of the primary proton spectrum is orders of magnitude higher that the spectra of the secondaq I-36 particles. The difference between solar minimum and solar maximum fluxes depends on the energy of the particle and the location in the magnetosphere. Analyses Daily Orbit-Integrated of data from the DMSP satellite showed EoS that the proton fluxes change at a rate of about 67o model the phase. average levels over the solar cycle — ...

The fluxes from the models represent averages that one would expect over the solar cycle phase for missions of 6 months duration or greater. Other than reflecting variations in the particle fluence levels due to the solar cycle phases, the models are static and do not reflect variations caused by the slowly changing geomagnetic field or due to magnetic storms and substorms. Uncertainty factors of 2 have been defined for the AP-8 and AE-8 [48,49]. the statistical uncertainty These represent from combining data from several datasets and do not reflect either For limited durations, short term excursions long or short term variations in the environment.

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Applying Computer Simulation Tools to Radiation Effects Problems by Nuclear and Space Radiation Effects Conference Short Course 1997


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