共查询到17条相似文献,搜索用时 422 毫秒
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针对宇航用大容量SRAM器件抗单粒子效应性能的试验评估需要,利用重离子加速器对抗辐射加固32 M Bulk CMOS工艺SRAM和16 M SOI CMOS工艺SRAM进行了单粒子效应模拟试验研究,获得SRAM器件单粒子效应特性并进行在轨翻转率预估;对单粒子翻转试验中重离子射程的影响,不同SEU类型的翻转截面差异,在轨翻转率预估的有关因素等进行了分析讨论。结果表明,这2款抗辐射加固SRAM器件都达到了较高的抗单粒子效应性能指标。试验结果可以为SRAM器件的单粒子效应试验评估提供参考。 相似文献
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《航天返回与遥感》2018,(6)
文章利用重离子地面模拟源,采用图像分析方法,开展了CCD视频信号处理器件单粒子效应系统性试验与测试研究。首先介绍了器件单粒子效应(SEE)试验方案、试验测试系统组成;然后通过试验研究获得了器件单粒子翻转(SEU)和单粒子锁定(SEL)特征参数,评估了视频信号处理器件单粒子翻转、单粒子锁定效应对系统成像性能的影响。试验结果表明:地面试验测试系统可有效实时判断、统计该器件单粒子效应发生事件,并能直观实时观察到单粒子事件发生时遥感图像的变化;视频信号处理器件随着重离子LET值增大,其单粒子截面呈增加趋势,器件对重离子诱发的单粒子效应比较敏感;单粒子锁定对光学遥感器成像任务的危害程度高于单粒子翻转。最后给出了采取单粒子锁定防护建议。 相似文献
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针对空间用SRAM型FPGA器件抗单粒子效应性能全面测试评估的要求,研究内部不同资源电路结构的单粒子效应敏感性及测试方法,利用重离子加速器开展抗辐射加固SRAM型FPGA单粒子效应模拟辐照试验,对配置存储器、块存储器、触发器等敏感单元的单粒子翻转、单粒子功能中断、单粒子锁定特性进行研究。试验结果表明,所提出测试方法能有效地覆盖测试SRAM型FPGA单粒子效应敏感资源,所测试抗辐射加固SRAM型FPGA器件具有良好的抗单粒子锁定性能,但对单粒子翻转和单粒子功能中断非常敏感,静态测试模式下对单粒子翻转更为敏感。有关测试方法和结果可以为SRAM型FPGA的单粒子效应评估及防护提供参考。 相似文献
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通过在某新型卫星立项攻关上的设计实例,介绍了一种设计方法;通过80C31单片机系统对有效载荷的温度变化进行及时采集监测,并根据卫星运行规律和温度控制要求对百叶窗进行及时有效的控制,在线路设计上采用了双CPU系统控制和备份通道控制三套备份设计,极大地提高了控制线路工作的可靠性,能满足卫星工作的要求。 相似文献
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以40 nm和65 nm CMOS工艺SRAM为样品,进行质子辐照单粒子效应试验研究,以建立空间质子引起单粒子效应的地面等效评估试验方法。分别进行低能质子直接电离、高能质子核反应和重离子直接电离引起的单粒子翻转试验;根据获得的试验数据,分析讨论给出空间质子引起半导体器件单粒子效应的地面等效评估试验方法:对低能质子直接电离引起的单粒子效应,基于LET等效采用重离子进行试验;对高能质子非直接电离引起的单粒子效应,采用高能质子进行试验;根据地面质子和重离子辐照试验数据,结合空间辐射环境模型,预计由空间质子辐射引起的器件在轨单粒子翻转率。 相似文献
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SRAM型FPGA单粒子效应试验研究 总被引:6,自引:0,他引:6
针对军品级SRAM型FPGA的单粒子效应特性,文中采用重离子加速设备,对Xilinx公司Virtex-II系列可重复编程FPGA中一百万门的XQ2V1000进行辐射试验。试验中,被测FPGA单粒子翻转采用了静态与动态两种测试方式。并且通过单粒子功能中断的测试,研究了基于重配置的单粒子效应减缓方法。试验发现被测FPGA对单粒子翻转与功能中断都较为敏感,但是在注入粒子LET值达到42MeV·cm 2/mg时仍然对单粒子锁定免疫。本文对翻转敏感度、测试方法与减缓技术进行了讨论,试验结果说明SRAM型FPGA对单粒子效应比较敏感,利用重配置技术的减缓方法能够有效降低敏感度,实现空间应用。
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星载数字电子设备的辐射加固技术(一) 总被引:9,自引:0,他引:9
对国外星载电子设备特别是常用的CMOS器件在空间环境下的抗辐射性能进行大量调研和长期跟踪,在此基础上总结了国外近年来对大规模集成电路辐射失效机理的研究成果,对比了各种器件工艺集成电路的抗辐射性能,重点分析了星载电子系统总剂量辐射损坏、单粒子翻转和单粒子锁定机理,针对这三种由空间辐射引起的星载电子系统失效这一特殊问题,分别介绍了国内外行之有效的辐射加固技术,最后提出了设计星载电子系统的一些建议。 相似文献
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NASA is concerned with protecting astronauts from the effects of galactic cosmic radiation and has expended substantial effort in the development of computer models to predict the shielding obtained from various materials. However, these models were only developed for shields up to about 120 g/cm2 in mass thickness and have predicted that shields of this mass thickness are insufficient to provide adequate protection for extended deep space flights. Consequently, effort is underway to extend the range of these models to thicker shields and experimental data is required to help confirm the resulting code. In this paper empirically obtained effective dose measurements from aircraft flights in the atmosphere are used to obtain the radiation shielding function of the Earth's atmosphere, a very thick, i.e. high mass, shield. Obtaining this result required solving an inverse problem and the method for solving it is presented. The results are shown to be in agreement with current code in the ranges where they overlap. These results are then checked and used to predict the radiation dosage under thick shields such as planetary regolith and the atmosphere of Venus. 相似文献
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为了提高宇航用存储器的抗单粒子翻转能力,本文对传统的单错误修正、双错误探测(Single Error Correction and Double Error Detection, SEC DED)码的构造进行了改进和优化,给出了构建单错校正、双错检测、相邻双错校正(Single Error Correction, Double Error Detection and Double Adjacent Error Correction, SEC DED DAEC)码奇偶校验矩阵的构造规则。通过适当地增加奇偶校验矩阵列向量的权重和、改变奇偶校验矩阵列向量顺序的方式,提出了一种具有新特征结构的SEC DED DAEC码,它可以修正任意相邻两位错误。实验结果表明,提出的SEC DED DAEC码是一种有效的宇航用存储器抗单粒子翻转加固措施,其冗余开销基本与传统的SEC DED码相同,误码率低于国际同类文献的结果。 相似文献
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Based on the analysis of solar events on August 18, 1995 (SN/C1.9 limb event) and September 23, 1998 (3B/M6.9 disk event) we suggest a new scenario of a solar flare with a surge in which the return motion of a surge is a cause of additional energy release and formation of a second system of solar flare ribbons. Observations in Hα line and data on X-ray emission fluxes in the range 1–8 Å and 0.5–4 Å are supplemented for the second case by the data in line 1550 Å. The scenario specifies two stages of development. During the first one the energy release proceeds in the current layer, which makes provisions both for acceleration of eruption upward from the solar surface and for the flare itself, including flare region heating, and radiation and thermal conductance losses. The second stage of the flare is supplied with energy due to a fall of the surge substance onto the chromosphere. The second pair of flare ribbons observed at this stage is suggested as a chromospheric criterion of realization of this scenario for disk flares. The energy released during the first stage of the flare on September 23, 1998 was equal to ~3 · 1031 erg. Its part consumed on flare processes is about ~0.5 · 1031 erg. The remaining part representing the eruption energy is consistent in order of magnitude with a calculated value of the flare energy on the second stage, which does not contradict the suggested scenario. Early recognition of such a scenario for flares on the disk can be used for prompt space weather forecast. In particular, a flare with a surge allows one to predict the absence of a bright core in a coronal mass ejection. 相似文献