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The LET spectra shown in Figure 29 are applicable to geosynchronous and interplanetary missions where there is no geomagnetic attenuation. The earth’s magnetic field, however, provides significant protection. Due to the basic interaction of charged particles with a magnetic field, the charged particles tend to follow the geomagnetic field lines. Near the equator the field lines tend to be parallel to the earth’s surface. Thus all but the most energetic ions are deflected away. In the polar regions the field lines tend to point toward the earth’s surface, which allows much deeper penetration of the incident ions.

An example of this is shown in Fig. 95 MeV differential electron fluxes for 6 levels of geomagnetic activity [Gu96]. It is seen that the flux changes are much larger for the smaller L-shell values shown. The current CRESSELE model, which is valid for solar maximum, features flux profiles ranging for 6 levels of geomagnetic activity, an average profile, and a worst-case profile encountered during the mission. Figure 22. 95 MeV during the CRRES mission for 6 different 15-day running average values of the Ap geomagnetic index.

Probability plot of encountering a given > 1 MeV electron flux at a given L-value during the declining phase of solar cycle 22 [Pe01]. The observations made of the slot region with instrumentation onboard the UARS satellite are consistent with recent results obtained from the TSX5 mission over an approximately 4 year period [Br04]. 2 MeV electron fluxes in this region. The distribution shows the probability that a daily averaged flux exceeds the threshold flux shown on the x-axis. The well-known “Halloween-2003” storm occurred during this mission and is shown for reference along with results for the AE-8 model.

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Modeling the Space Radiation Environment and Effects on Microelectronic Devices and Circuits by NSREC 2006

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