空间高能粒子与器件布线层核反应后次级粒子LET分布研究

空间高能质子和重离子是导致元器件发生单粒子效应的根本原因,为准确评估元器件在轨遭遇的单粒子效应风险,必须清楚高能质子、重离子与器件材料发生核反应的物理过程及生成的次级重离子LET（Line EnergyTransfer）分布规律。针对典型CMOS工艺器件模拟计算了不同能量质子和氦核粒子在器件灵敏单元内产生的反冲核、平均能量及线性能量转移值,并分析了半导体器件金属布线层中重金属对次级重离子LET分布的影响规律。计算结果表明：高能粒子与器件相互作用后产生大量次级重离子,且高能质子作用后产生的次级粒子的LET值主要分布为0～25MeV·cm²/mg;高能氦核粒子作用后产生的次级粒子的LET值主要分布为0～35 MeV·cm²/mg;有重金属钨（W）存在时能提高次级粒子的LET值,增加了半导体器件发生单粒子效应的概率,该研究结果可为元器件单粒子效应风险分析、航天器抗单粒子效应指标确定提供重要依据。     

质子引发的单粒子翻转率估算的研究

根据质子单粒子翻转事件的物理本质,及空间高能质子环境特性,给出了一种基于重离子单粒子翻转实验数据基础之上的估算质子引发的单粒子翻转的方法.利用这种方法计算了几种器件的翻转情况,与地面模拟实验及飞行观测结果符合得非常好.      

基于TCAD和Geant 4的SRAM单粒子效应评估

基于Geant4和TCAD (Technology-Computer Aided-Design)建立了一套评估静态存储器(SRAM)单粒子效应的方法. 该方法利用TCAD软件模拟半导体存储单元对粒子能量沉积的响应, 获得SRAM的重离子单粒子翻转截面, 并应用蒙特卡罗工具包Geant 4计算质子与硅材料的核反应以及次级粒子在灵敏体积内的能量沉积, 进而获得质子的单粒子翻转率. 利用该方法, 计算了TSMC 0.18 μm未加固SRAM的重离子和质子翻转率, 通过与同工艺SRAM的重离子实验结果进行比较, 初步验证了该方法的有效性. 该方法不依赖于地面模拟实验, 可以用来评估处于设计阶段的抗辐射加固器件.      

半导体器件单粒子效应的机理,试验和预计

介绍了空间高能粒子环境及单粒子效应的机理、模拟试验方法和错误率计算方法。空间高能粒子环境由银河宇宙射线、太阳宇宙射线及地磁捕获粒子组成。单个高能粒子可在半导体中通过库仑作用或核反应电离出大量电子—空穴对,从而引起半导体器件逻辑紊乱或失效。用加速器产生的高能粒子进行模拟试验可获得器件对单粒子效应的敏感参数;由E.L.Peterson 等人的经验公式或CREME 程序预计器件在特定环境下的出错率。     

质子单粒子翻转截面计算方法

在分析质子与硅反应的基础上,建立了质子单粒子翻转截面理论计算模型,提出了模拟计算方法。计算得到了不同能量的高能质子与硅反应产生的次级粒子种类、截面、能谱和双微分截面。采用Monte Carlo方法模拟质子与硅的反应;应用TRIM程序计算次级粒子的射程;计算得到次级粒子在存储单元的灵敏区内沉积的能量,产生的电荷。通过与临界电荷的比较,判断是否导致单粒子翻转,从而得到单粒子翻转截面。计算得到的单粒子翻转截面与实验数据符合较好。     

SRAM型FPGA单粒子翻转效应加固方法

应用重离子加速器和皮秒脉冲激光器开展Virtex-Ⅱ FPGA（Field Programmable Gate Array）单粒子效应加固方法有效性研究.实验结果表明,同时应用三模冗余和动态刷新加固方法能够完全纠正单粒子效应产生的功能错误.实验获得数据加密算法在不同单粒子效应加固方法下功能错误截面,发现少量的存储位翻转就可以导致程序功能错误;程序功能对存储位翻转较敏感.分析Virtex-Ⅱ FPGA不同加固方法在不同卫星轨道的有效性,同时应用动态刷新和三模冗余加固方法,可以完全校正由于存储位翻转造成的功能错误.重离子加速器和脉冲激光器实验结果同时表明,脉冲激光可以模拟重离子加速器研究单粒子效应加固方法有效性.     

太阳质子事件对太阳同步轨道空间辐射环境影响分析

介绍了南大西洋异常区的辐射环境及其特点，重点研究了发生于2000年7月14日的太阳质子事件对太阳同步轨道空间环境造成的影响，太阳质子事件期间，抵达近地空间的高能电子、质子及重离子对太阳同步轨道空间环境造成剧烈地扰动，并且不同种类不同能量的粒子扰动特征不尽相同。     

宇宙辐射,是资源还是祸害?

不是所有的东西都能成为太空家园的资源.有些不仅不是资源反而是祸害,宇宙辐射就是其中一例。 太空中的宇宙辐射对人体危害最大的主要是银河宇宙线和太阳宇宙辐射。银河宇宙线的主要成分是高能质子和原子序为偶数的重离子。太阳粒子事件产生大量的高能粒子,其中主要是质子、重粒子和电子。对人体危害最大的是质子,其次是重粒子。     

脉冲激光模拟空间载荷单粒子效应研究进展

脉冲激光作为模拟测试空间探测载荷半导体器件的单粒子效应现象的一种较新型手段,具有可以定位器件对单粒子效应敏感的具体单元以及动态测试电路系统对单粒子效应的时间响应特性的特点,能够满足工程部门、器件研发部门的不同需求。通过实验与理论研究,建立单粒子锁定与翻转效应的激光阈值能量与重离子LET值的对应关系,解决了脉冲激光模拟测试的激光结果如何定量的关键问题,据此可以定量摸底评估器件的单粒子效应敏感度,使脉冲激光测试载荷的结果更具评价以及指导意义,这对建立统一的脉冲激光单粒子效应评估试验标准以及对脉冲激光试验的推广具有重要意义。空间探测载荷发生单粒子效应后器件功能特性及电路系统的影响、防范单粒子效应电路条件影响的手段下电路系统的抗单粒子效应设计措施是的有效性,以及为空间探测专门研制的抗辐射ASIC电路评价,都需要更加精细的单粒子效应测试方法。通过建立便捷、低成本的脉冲激光定量试验的手段,解决了空间探测载荷上述单粒子效应试验的问题。     

外辐射带动态演化的粒子模拟研究

运用计算机实验方法即三维电磁粒子模拟方法初步研究了暴时扰动情况下外辐射带粒子环境的动态演化特性。模拟计算了暴时辐射带粒子环境的演化情况。模拟计算结果显示，高能质子、电子注入午辐射滞后，两者一方面沿磁力线做弹跳运动，向高纬扩展，部分注入质子和电子沉降于南北两极区域；另一方面，注入质子和电子还经历顺时针和逆时针方向的漂移运动，粒子能量越大，漂移速度越快。暴时多次注入引起整个辐射带粒子能量的大幅增强；粒子注入颗次和强度越大，辐射带粒子通量增幅越大。本项研究为开发研制完整的辐射带动态模式积累了有益的经验。     

Geomagnetically trapped heavy ions resulting from the anomalous cosmic rays

Blake and Freisen painted out that if the anomalous cosmic rays are only singly charged they can penetrate deeply into the Earth's magnetosphere well below the cutoff for stripped ions. Ions which reach low altitude can be stripped by the residual atmosphere and become stably trapped. An experiment has been developed which will be able to detect the intensities of such stably trapped heavy ions as a function of magnetospheric position. In anticipation of the flight of this experiment, the fluxes and spectra of the trapped heavy ions have been calculated based upon the anomalous component observed in the IPM.     

“风云一号”(B)星对内辐射带质子的观测结果

本文介绍“风云一号”(B)星上的“宇宙线成份监测器”于1990年11月19至24日对内辐射带质子的观测结果。通过对这些结果的分析, 本文获得了4—23MeV能量范围内辐射带质子垂直强度在磁坐标内的分布特征。同时, 本文还给出了100°E子午面内质子垂直强度的分布。分析表明, 所得结果与辐射带理论一致。      

Depth dose measurements with the Liulin-5 experiment inside the spherical phantom of the MATROSHKA-R project onboard the International Space Station

The Liulin-5 experiment is a part of the international project MATROSHKA-R on the Russian segment of the ISS, which uses a tissue-equivalent spherical phantom equipped with a set of radiation detectors. The objective of the MATROSHKA-R project is to provide depth dose distribution of the radiation field inside the sphere in order to get more information on the distribution of dose in a human body. Liulin-5 is a charged particle telescope using three silicon detectors. It measures time resolved energy deposition spectra, linear energy transfer (LET) spectra, particle flux, and absorbed doses of electrons, protons and heavy ions, simultaneously at three depths along the radius of the phantom. Measurements during the minimum of the solar activity in cycle 23 show that the average absorbed daily doses at 40 mm depth in the phantom are between 180 μGy/day and 220 μGy/day. The absorbed doses at 165 mm depth in the phantom decrease by a factor of 1.6–1.8 compared to the doses at 40 mm depth due to the self-shielding of the phantom from trapped protons. The average dose equivalent at 40 mm depth is 590 ± 32 μSV/day and the galactic cosmic rays (GCR) contribute at least 70% of the total dose equivalent at that depth. Shown is that due to the South Atlantic Anomaly (SAA) trapped protons asymmetry and the direction of Liulin-5 lowest shielding zone the dose rates on ascending and descending nodes in SAA are different. The data obtained are compared to data from other radiation detectors on ISS.     

三种类型的质子耀斑

根据SMM卫星观测资料,分析了GRL,PE和GRL/PE三种类型质子耀斑在硬X射线辐射特征上的差异。结果表明,存在的差异与粒子加速区(或作用区)分别处于不同的日面高度有关。      

On the origin of trapped heavy ions at L = 1.4-1.6.

Aboard the NASA satellite Long Duration Exposure Facility (LDEF) heavy ions of nuclear charge Z = 8-26 were detected with energies between 15 and 50 MeV/nuc which are far below the cutoff energy required of fully stripped ions to reach the LDEF orbit. The arrival directions and the falling energy spectra of these particles are consistent with a trapped component incident in the South Atlantic Anomaly at L = 1.4-1.6. The trapped oxygen, neon and argon ions probably originate from the anomalous cosmic rays, whereas the origin of the other particles like magnesium, silicon and iron is not yet solved but may be associated with the October 89 solar energetic particle events.     

Radiation effects in space.

The radiation protection guidelines of the National Aeronautics and Space Administration (NASA) are under review by Scientific Committee 75 of the National Council Protection and Measurements. The re-evaluation of the current guidelines is necessary, first, because of the increase in information about radiation risks since 1970 when the original recommendations were made and second, the population at risk has changed. For example, women have joined the ranks of the astronauts. Two types of radiation, protons and heavy ions, are of particular concern in space. Unfortunately, there is less information about the effects on tissues and cancer by these radiations than by other radiations. The choice of Quality Factors (Q) for obtaining dose equivalents for these radiations, is an important aspect of the risk estimate for space travel. There are not sufficient data for the induction of late effects by either protons or by heavy ions. The current information suggests a RBE for the relative protons of about 1, whereas, a RBE of 20 for tumor induction by heavy ions, such as iron-56, appears appropriate. The recommendations for the dose equivalent career limits for skin and the lens of the eye have been reduced but the 30-day and annual limits have been raised.     

Recent developments in ion mass spectrometers in the energy range below 100 keV

The recognition that heavy ions often have similar or higher abundance than protons in space plasmas and the fact that ions with masses and/or charges larger than unity are ideally suited to test theories on origin, transport, acceleration, and loss of these plasmas led to the development of new and more sophisticated mass spectrometers during the last decade. The characteristics of several state-of-the-art instruments which have been flown or selected for missions will be discussed and aims for future developments will be given.     

Radiation issues for piloted Mars mission.

Man is now entering an era of colonizing the moon and exploration of Mars. The crewmembers of a piloted mission to Mars will be exposed to inner belt trapped protons, the outer trapped electrons, and the galactic cosmic radiation. In addition there is always the added risk of acute exposure to a solar particle event. Current radiation risk is estimated using the idea of absorbed dose and ICRP-26, LET-dependent quality factors. In a spacecraft with aluminum walls (2 g cm-2) at solar minimum the calculated dose equivalent is 0.73 Sv for a 406-day mission. Based on the current thinking this leads to an excess cancer mortality in a 35 year male of about 1%. About 75% of the dose equivalent is contributed by HZE particles and target fragments with average quality factors of 10.3 and 20, respectively. The entire concept of absorbed dose, quality factor, and dose equivalent as applied to such missions needs to be reexamined, in light of the fact that less than 50% of the nuclei in the body of the astronaut would have been traversed by a single GCR nuclei in the 406-day mission. Clearly, more biologically relevant information about the effects of heavy ions and target fragments is needed and fluence based risk estimation strategy developed for such long term stays in space.     

Single-event upset in geostationary transfer orbit during solar-activity maximum period measured by the Tsubasa satellite

This paper reports single-event upset (SEU) occurrence related to the space radiation environment in geostationary transfer orbit during solar-activity maximum period measured by the Tsubasa satellite. Most SEUs are measured in the inner radiation belt, indicating that they are mainly caused by trapped protons. Thus, the spatial distribution and the temporal variation of the SEU count correlate well with those of trapped protons. The peak SEU rate appears around L = 1.4. The transition point from SEUs caused by trapped protons to those caused by galactic cosmic rays is around L = 2.6. During the experiment period, increased SEU count was sometimes detected due to solar and geomagnetic events outside the inner radiation belt.