REG NASA-LLIS-0647-2000 Lessons Learned Solar Flare Proton and Heavy Ion Modeling for Single Event Effects.pdf

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1、Best Practices Entry: Best Practice Info:a71 Committee Approval Date: 2000-03-01a71 Center Point of Contact: JPLa71 Submitted by: Wil HarkinsSubject: Solar Flare Proton and Heavy Ion Modeling for Single Event Effects Practice: Practice: Operational spacecraft can experience adverse effects from impi

2、nging high energy radiation. A single event upset (SEU) occurs when a single particle, usually a heavy ion or proton, deposits enough charge at a sensitive node in a microcircuit to cause that circuit to change state. In general, these effects are temporary and appear as “soft failures“ such as anom

3、alous bit flips or spurious commands. In extreme cases, latch-up can occur and result in the destructive failure of the part.The practice is to formulate an energetic particle environment model for calculating single event effect rates by utilizing the JPL statistical models for solar proton, alpha

4、particle and heavy ion fluence. This predicted rate, which is a function of cumulative probability, is a useful measure when specifying shielding thickness to protect susceptible components, employing mitigating software, or both to reduce the risk to an acceptable level. Note that this assessment d

5、oes not consider concentration of particle radiation due to the Earths magnetic field, (ref. 1), and factors which are not influenced by shielding thickness, such as GCR (Galactic Cosmic Rays).Abstract: Preferred Practice for Design & Test. Non-use of the updated JPL solar flare proton and heavy ion

6、 models could force designers to over-design, based on the predictions from the Adams worst case model which predicts unrealistically high single event effects.Formulate an energetic particle environment model for calculating single event effect rates by utilizing the JPL statistical models for sola

7、r proton, alpha particle and heavy ion fluence. This predicted rate, which is a function of cumulative probability, is a useful measure when specifying shielding thickness to protect susceptible components, employing mitigating software, or both to Provided by IHSNot for ResaleNo reproduction or net

8、working permitted without license from IHS-,-,-reduce the risk to an acceptable level. Programs that Certify Usage: Programs That Certified Usage: Cassini, Multi-Angle Imaging Spectroradiometer (MISR), Atmospheric Infrared Sounder (AIRS), NASA SEP Technology Application Readiness (NSTAR), Hermes, Ad

9、vanced Composition Explorer (ACE), Mars Missions.Center to Contact for Information: JPLImplementation Method: This Lessons Learned is based on Reliability Practice No. PD-EC-1105 from NASA Technical Memorandum 4322A, NASA Reliability Preferred Practices for Design and Test.Benefits:Shielding thickne

10、ss can be realistically assessed by considering the cumulative probability of component failure due to radiation of solar particles.Implementation Method:JPL computer codes (ref. 2 & 3), simulate the transport of ion fluxes determined from the particle models through specified shielding thicknesses

11、of aluminum to obtain resultant spectra. These spectra are used to calculate device single event effect rates when applied to the laboratory measured cross sections. For low linear energy transfer (LET) threshold devices, proton upset cross sections vs. energy are used to determine upset rates from

12、the proton energy spectra. For higher LET threshold devices the measured upset cross section vs. LET is used with the Heinrich flux for heavy ions to determine single event effect rates.Technical Rationale:Penetrating ions create ionization tracks in silicon components. The heavier ions produce dens

13、er ionization tracks. Disposition of the created charge, which depends on the electric field configuration within the device, can lead to the following effects:1. Recombination without single event effects,Provided by IHSNot for ResaleNo reproduction or networking permitted without license from IHS-

14、,-,-2. Single event upsets,3. Device latch up, and4. Spurious signals.Measurements of proton solar event fluences and alpha particle solar event fluences have been obtained for many solar flares. Organizing these data in a statistical manner according to cumulative probability of occurrence for a sp

15、ecified particle event fluence level constitutes the proton and alpha particle models.Solar flare heavy ion data are more difficult to obtain because the lower flux levels and the need for mass discrimination requires more sophisticated instrumentation. The paucity of available data creates the need

16、 for a heavy ion model based on solar abundances. A solar heavy ion model (ref. 4) has been constructed based on the work of Breneman and Stone (ref. 5) who analyzed heavy ion data from 10 solar flares between 1977 and 1982.It has been assumed that the average alpha fluence is predictable from the h

17、eavy ion model relative to the other ion species. However, the proton fluence is not predictable from the heavy ion model. The heavy ions are normalized to the alpha particle probability of occurrence fluence levels by requiring that the integrated alpha fluence level from the heavy ion model match

18、the fluence level from the measured alpha statistical distribution model. Complete ion flux spectra are specified in this manner. These spectra can be introduced into transport software to determine shielding requirements and software to determine single event effect rates.Related Practices:1. Envir

19、onmental Factors, Practice No. PD-EC-1101References:1. SSP 30425 (SSP Natural Environment Definition), Chapter 6.2. Feynman, J., Spitale, G., Wang, J., Interplanetary Proton Fluence Model: JPL 1991, Jet Propulsion Laboratory IOM 5217-92-23, February 6, 1992.3. Spitale, G., Feynman, J., Wang, J., Sol

20、ar Alpha Particle Model: Progress and Problems, Jet Propulsion Laboratory IOM 5217-92-60, March 5, 1992.4. Croley, D.R., Solar Flare Heavy Ion Model, IEEE Transactions on Nuclear Science, June 22, 1992.5. Breneman, H., Stone, E. (1985). Solar and Photospheric Abundance from Solar Energetic Particle

21、Measurements, Astrophysical Journal, 299, L57-L61.6. Adams, et. al., (1981). Cosmic Ray Effects on Microelectronics, Part I: The Near-Earth Particle Environment. NRL Memorandum Report 4506, Naval Research Laboratory, Washington, D.C.Provided by IHSNot for ResaleNo reproduction or networking permitte

22、d without license from IHS-,-,-Impact of Non-Practice: Impact of Nonpractice: Non-use of the updated JPL solar flare proton and heavy ion models could force designers to over-design, based on the predictions from the Adams worst case model (ref. 6) which predicts unrealistically high single event effects.Related Practices: N/AAdditional Info: Approval Info: a71 Approval Date: 2000-03-01a71 Approval Name: Eric Raynora71 Approval Organization: QSa71 Approval Phone Number: 202-358-4738Provided by IHSNot for ResaleNo reproduction or networking permitted without license from IHS-,-,-