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。     

空间辐射粒子引起单粒子翻转率预计

空间辐射粒子引起单粒子翻转（ＳＥＵ）率预计的基础是地面粒子加速器模拟试验数据、卫星轨道的粒子辐射环境模型和高能粒子与器件相互作用模型。引起ＳＥＵ的空间辐射粒子包括银河宇宙射线、太阳宇宙射线和地磁俘获粒子。高能粒子通过电离产生多余电子－空穴对引起ＳＥＵ。介绍了计算轨道中ＳＥＵ率的程序ＣＲＥＭＥ。以８０Ｃ３１微控制器为例,根据串列静电加速器地面模拟试验结果,进行了在轨ＳＥＵ率预计。     

卫星天线辐射方向图的计算

利用几何绕射理论分析了卫星星体和太阳翼对卫星天线辐射场的影响 ,建立了一套以数值分析和仿真技术为主的卫星天线辐射场的预估方法 ,克服了传统设计与测量技术难于解决的问题。给出了一些数值计算验证 ,并结合型号设计 ,进行了实验验证。验证结果表明文中所作的理论分析和在此基础上开发的仿真算法和软件是可靠有效的。     

载人深空探测任务的空间环境工程关键问题

对载人深空探测过程中将遭受的太阳宇宙射线、银河宇宙射线、微重力、尘与尘暴、深空微生物等环境进行分析。对不同深空环境给航天员带来的威胁进行了探讨。从物理屏蔽防护、辐射风险的监测和预警、辐射防护药物、航天员选拨等角度对采取的措施进行了阐述。从空间辐射对航天员的损伤机理、抗辐射和微重力药物开发、空间辐射屏蔽防护结构与材料、航天服自清洁、抗微生物侵蚀材料的研发等多个角度对需要进一步开展的工作进行了讨论。     

强γ射线参考辐射场散射影响研究

采用蒙特卡罗程序MCNP对强γ射线参考辐射场的散射特性进行了模拟,确立了辐射场实验空间内的剂量率和能谱分布。通过多种角度对屏蔽墙散射和在束散射体散射进行了细致的分析,为校准实验室钴源辐射场的实验应用和屏蔽设计提供参考。     

涡扇发动机地面起动过程性能模拟

用积分方法建立了混合排气加力涡扇发动机起动过程模拟模型并用该模型进行了仿真计算,模型基于气动热力学方程、各部件特性以及经验关系式,根据给出的发动机起动过程初始条件、燃烧室供油规律等进行计算.为说明所建立的起动性能模型的模拟效果,将程序计算结果与试验结果进行了比较,结果表明该起动仿真模型能较准确地模拟混排加力涡扇发动机的地面起动过程.还分析了计算过程中对起动过程有比较大影响的因素,包括计算时间步长,起动机脱开转速,燃烧室总压恢复系数的经验系数,大气温度、压力以及海拔高度等.了解这些因素对起动过程及模拟结果的影响,便于通过修正的途径将该计算方法用于发动机地面起动性能的准确模拟.      

航天员受银河宇宙线辐射的剂量计算

在近地空间(LEO)和深空探测中,航天员遭受的辐射风险主要来自于银河宇宙线(GCR)照射.银河宇宙线的辐射剂量是航天员辐射风险评价的基础.国际放射防护委员会(ICRP)于2013年提出了新的航天员空间辐射剂量估算方法,以更准确给出空间重离子辐射的剂量.基于此方法,开发了宇宙线粒子在物质中输运的蒙特卡罗程序,并在程序中实现用中国成年男性人体数字模型来仿真航天员.采用该程序计算了粒子(Z=1~92)各向同性照射航天员时器官的通量-器官剂量转换因数,并估算出航天员在近地轨道空间受银河宇宙线辐射的剂量.     

媒体SCAN

想参加星际旅行,却害怕宇宙射线对身体造成伤害吗?科学家提出了新构想——电浆泡泡,先将电浆形成电流,再利用此电流产生的磁场使宇宙射线偏折。若这个构想可行,未来宇航船笨重的宇宙射线保护壳将被轻薄的电浆泡泡所取代。在人类长期的太空旅行中,宇宙射线造成的健康问题是最重要的安全考量。可能的健康风险包括癌症、白内障、遗传疾病、中枢神经系统的损害等。太空中主要的辐射源包括银河宇宙射线、太阳粒子以及困在地球磁场中的质子、电子等。当生物长期曝晒于宇宙射线中时,射线的高能粒子可能造成D N A盐基键的断裂或其他无法修补的损毁…     

关于球形导体外部倾斜赫芝振子辐射场的探讨

本文给出球形导体倾斜赫芝振子辐射场的线极化与圆极化分量表达式,并进行计算,示出典型剖面内的各分量方向图。由此可进一步分析球形导体上线状天线的辐射特性。     

一种评估空间环境下半导体材料损伤的模拟方法

提出了一种模拟空间环境下半导体材料晶格损伤速率的方法, 计算了375km轨道高度不同纬度空间位置的飞行器模型中硅片产生晶格损伤的速率. 本方法考虑了宇宙射线的质子、正负电子、中子和γ射线成分, 建立了简单的多层飞行器结构模型, 并通过模拟给出了芯片上氕、氘、氚、氦、正负电子、正负π介子、γ射线及中子的损伤结果. 相比给出材料中的非电离能量损失, 更进一步给出了晶格损伤的产生速率, 为半导体器件的可靠性评估提供了进一步的参考数据.      

Cosmic ray reacceleration on the galactic wind termination shock

Reacceleration of cosmic rays produced by galactic sources on the galactic wind termination shock is considered. The problem of the cosmic ray spectrum continuity is investigated. Numeric results are presented and discussed. We found that a smooth spectral transition from the galactic cosmic rays to the cosmic rays reaccelerated at the galactic wind termination shock is difficult to produce, if the maximum energy of accelerated particles is the same throughout the surface of the termination shock. The possible solution of this problem is the non-spherical termination shock with different maximum energies at different places of the shock.     

Empirical model of cosmic ray spectrum in energy interval 1 MeV–100 GeV during 11-year solar cycle

The galactic cosmic rays (GCR) are the main ionization source at altitude of ∼3–35 km in the atmosphere. For high latitude anomalous cosmic ray (ACR) component has also a significant influence on the atmospheric ionization. We propose an empirical model for differential spectra D(E) of galactic and anomalous cosmic rays in energy interval 1 MeV–100 GeV during solar cycle. In the model data are used which cover three solar cycles: 20, 22 and 23. The LEAP87, IMAX92, CAPRICE94, AMS98 and BESS experimental spectra for protons and alpha particles are fitted to the proposed empirical model. The modulated GCR differential spectra are compared with force-field approximation to the one-dimensional transport equation and with solutions of two-dimensional cosmic ray transport equation. For experimental spectra, the calculation of the model parameters is performed by Levenberg–Marquardt algorithm, applied to the special case of least squares. Algorithm that combines the rapid local convergence of Newton–Raphson method with globally convergent method for non-linear systems of equations is applied for theoretically obtained differential spectra. The described programmes are realized in algorithmic language C++. The proposed model gives practical possibility for investigation of experimental data from measurements of galactic cosmic rays and their anomalous component.     

Ion production and ionization effect in the atmosphere during the Bastille day GLE 59 due to high energy SEPs

The influence of high energy particles, specifically cosmic rays, on atmospheric physics and chemistry is highly discussed. In most of the proposed models the role of ionization in the atmosphere due to cosmic rays is not negligible. Moreover, effect(s) on minor constituents and aerosols are recently observed, specifically over the polar regions during strong solar particle events. According to the recent findings for such effects it is necessary an essential increase of ion production, specifically during the winter period. The galactic cosmic rays are the main source of ionization in the Earth’s stratosphere and troposphere. Occasionally, the atmospheric ionization is significantly enhanced during strong solar energetic particles events, specifically over the polar caps. During the solar cycle 23 several strong ground level enhancements were observed. One of the strongest was the Bastille day event occurred on 14 July 2000. Using a full Monte Carlo 3-D model, we compute the atmospheric ionization, considering explicitly the contribution of cosmic rays with galactic and solar origin, focusing on high energy particles. The model is based on atmospheric cascade simulation with the PLANETOCOSMICS code. The ion production rate is computed as a function of the altitude above the sea level. The ion production rate is computed on a step ranging from 10 to 30?min throughout the event, considering explicitly the spectral and angular characteristics of the high energy part of solar protons as well as their time evolution. The corresponding event averaged ionization effect relative to the average due to galactic cosmic rays is computed in lower stratosphere and upper troposphere at various altitudes, namely 20?km, 15?km, 12?km and 8?km above the sea level in a sub-polar and polar regions. The 24^h and the weekly ionization effects are also computed in the troposphere and low stratosphere. Several applications are discussed.     

Radiation risk during long-term spaceflight.

Cosmonauts' exposure to cosmic rays during long-term spaceflight can cause unfavorable effects in health and risk for the crew members' lives. All unfavorable effects induced by exposure should be taken into consideration for the risk estimation. They should include both the acute deterministic effects and delayed effects called stochastic. On the ground the limitation of unfavorable consequences of acute exposure is achieved by means of establishing dose limits. But in space applications this approach can't be acceptable. Establishing a fixed dose limit is adequate to introducing indefinite reserve coefficient and therefore ineffective usage of spacecraft resource. The method of radiation risk calculation caused by acute and delayed effects of cosmonauts' exposure is discussed and substantiated in the report. Peculiarities of the impact of permanent radiation sources (galactic cosmic rays and trapped radiation) and the variable one (solar cosmic rays) are taken into consideration.     

Computation of radiation environment during ground level enhancements 65, 69 and 70 at equatorial region and flight altitudes

The radiation environment in the troposphere of the Earth is governed by cosmic rays of galactic and solar origin. During major solar energetic particles events the radiation environment changes dramatically. As a results the risk of biological effects due to exposure to ionizing radiation of aircrew increases. Here we present a numerical model for computation of absorbed dose in air due to cosmic rays of galactic and solar origin. It is applied for computation of radiation environment at flight altitude in the equatorial region during several major ground level enhancements, namely GLE65 on 28 October 2003, GLE69 on 20 January 2005 and GLE70 on 13 December 2006. The model is based on a full Monte Carlo simulation of cosmic ray induced atmospheric cascade. The cascade simulation is carried out with CORSIKA 6.990 code with corresponding hadron generators FLUKA 2011 and QGSJET II. The contribution of different cascade components, namely electromagnetic, hadron and muon is explicitly obtained. The spectra of arriving solar energetic particles are calculated from ground level measurements with neutron monitors and satellite data from GOES. The obtained results are discussed.     

Study of the 27-day variations of the galactic cosmic ray intensity and anisotropy

We demonstrate that the general features of the radial and azimuthal components of the anisotropy of galactic cosmic rays can be studied by the harmonic analysis method using data from an individual neutron monitor with cut off rigidity <5 GV. In particular, we study the characteristics of the 27-day (solar rotation period) variations of the galactic cosmic ray intensity and anisotropy, solar wind velocity, interplanetary magnetic field strength and sunspot number. The amplitudes of the 27-day variations of the galactic cosmic ray anisotropy are greater, and the phases more clearly established, in A > 0 polarity periods than in A < 0 polarity periods at times of minimum solar activity. The phases of the 27-day variations of the galactic cosmic rays intensity and anisotropy are opposite with respect to the similar changes of the solar wind velocity in A > 0 polarity periods. No significant dependence of the amplitude of the 27-day variation of the galactic cosmic ray anisotropy on the tilt angle of the heliospheric neutral sheet is found. Daily epicyclegrams obtained by Chree’s method show that the 27-day variations of the galactic cosmic ray anisotropy during A > 0 polarity periods follow elliptical paths with the major axes oriented approximately along the interplanetary magnetic field. The paths are more irregular during A < 0 polarity periods.     

Cosmic-ray composition and its relation to shock acceleration by supernova remnants

An overview is given on the present status of the understanding of the origin of galactic cosmic rays. Recent measurements of charged cosmic rays and photons are reviewed. Their impact on the contemporary knowledge about the sources and acceleration mechanisms of cosmic rays and their propagation through the Galaxy is discussed. Possible reasons for the knee in the energy spectrum and scenarios for the end of the galactic cosmic-ray component are described.     

Organ shielding and doses in Low-Earth orbit calculated for spherical and anthropomorphic phantoms

Humans in space are exposed to elevated levels of radiation compared to ground. Different sources contribute to the total exposure with galactic cosmic rays being the most important component. The application of numerical and anthropomorphic phantoms in simulations allows the estimation of dose rates from galactic cosmic rays in individual organs and whole body quantities such as the effective dose. The male and female reference phantoms defined by the International Commission on Radiological Protection and the hermaphrodite numerical RANDO phantom are voxel implementations of anthropomorphic phantoms and contain all organs relevant for radiation risk assessment. These anthropomorphic phantoms together with a spherical water phantom were used in this work to translate the mean shielding of organs in the different anthropomorphic voxel phantoms into positions in the spherical phantom. This relation allows using a water sphere as surrogate for the anthropomorphic phantoms in both simulations and measurements. Moreover, using spherical phantoms in the calculation of radiation exposure offers great advantages over anthropomorphic phantoms in terms of computational time.     

Assessment and requirements of nuclear reaction databases for GCR transport in the atmosphere and structures

The transport properties of galactic cosmic rays (GCR) in the atmosphere, material structures, and human body (self-shielding) are of interest in risk assessment for supersonic and subsonic aircraft and for space travel in low-Earth orbit and on interplanetary missions. Nuclear reactions, such as knockout and fragmentation, present large modifications of particle type and energies of the galactic cosmic rays in penetrating materials. We make an assessment of the current nuclear reaction models and improvements in these model for developing required transport code data bases. A new fragmentation data base (QMSFRG) based on microscopic models is compared to the NUCFRG2 model and implications for shield assessment made using the HZETRN radiation transport code. For deep penetration problems, the build-up of light particles, such as nucleons, light clusters and mesons from nuclear reactions in conjunction with the absorption of the heavy ions, leads to the dominance of the charge Z = 0, 1, and 2 hadrons in the exposures at large penetration depths. Light particles are produced through nuclear or cluster knockout and in evaporation events with characteristically distinct spectra which play unique roles in the build-up of secondary radiation's in shielding. We describe models of light particle production in nucleon and heavy ion induced reactions and make an assessment of the importance of light particle multiplicity and spectral parameters in these exposures.     

Radial distribution of galactic cosmic rays at solar maximum

In this paper we analyze the spatial distribution of galactic cosmic rays during periods of maximum solar activity of the cycles 21, 22 and 23. We have used a two dimensional model to solve the cosmic ray transport equation. This model includes all relevant physical processes: diffusion, convection, drift and shock effects on cosmic ray propagation inside the heliosphere. We focused on the study of the radial distribution of galactic cosmic rays, and compare our results with the spacecraft observations for two energies (175 MeV H and 265 MeV/n He). Although the radial intensities of galactic cosmic rays can be explained qualitatively with all three local interstellar spectra (LISs) used in this work, we applied a reduced chi-squared analysis to investigate the best LIS that could fit the data.