Single Event Upset Results from the Radiation Hardened Electronic Memory Experiment in a Polar Orbit

Alexander, David; Vera, Alonzo; Love, Jeff; Morris, W.; Gifford, David; Daniels, Zach; Major, Katharine; McHarg, Matthew; Gresham, Patrick; Moffett, Ian; Cress, Ryan; Maldonado, Carlos A.; Wilson, G. S.; Harley, J.

doi:10.1109/redw51883.2020.9325847

Cited by 2 publications

(1 citation statement)

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“…Many of these monitors are based on sophisticated radiation monitors that can detect different kinds of particles and resolve their energy [1,2]. Others are based on low-cost detectors, e.g., static random access memories (SRAMs) that can characterize the radiation environment by measuring single-event upsets (SEU) or single-event latchups (SEL) [3][4][5][6][7][8][9][10][11][12][13][14][15][16][17]. Often these radiation monitors can also be used to characterize beams at facilities.…”

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confidence: 99%

The CELESTA CubeSat In-Flight Radiation Measurements and Their Comparison With Ground Facilities Predictions

Coronetti,

Zimmaro,

García Alía

et al. 2024

IEEE Trans. Nucl. Sci.

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The CELESTA CubeSat has employed radiation monitors developed by the Conseil Europeeene pour la Recherche Nucleaire (CERN), used for measuring the radiation environment at accelerators, to measure the space radiation field in a medium-Earth orbit (MEO). The technology is based on three static random access memories (SRAMs) that are sensitive to singleevent upsets (SEUs) and single-event latchups (SELs). The measurements were performed for the duration of 2 months. A statistically significant amount of SEUs and SELs were collected. No solar proton event effects were observed in the data during this period. The in-flight rates were compared with respect to estimations coming from the environmental space fluxes available in the Outil de Modelisation de l'Environmment Radiative Externe (OMERE) tool suite and ground facility measurements done with ions and protons. The analysis emphasizes the importance of employing more sophisticated satellite shielding models for the calculation of the fluxes reaching the detectors as well as the need to know accurately the proton energy threshold of the SEU cross section Weibull response of the devices. Both observations mainly arise from the peculiar spectral distribution of protons in this MEO peaking at 10-20 MeV, which differs from those of a low-Earth orbit environment.

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