不同屏蔽材料对空间100 MeV质子防护效果分析

为了研究地球空间辐射环境中高能质子的屏蔽问题,使用基于蒙特卡罗方法的Geant4软件模拟了100 MeV质子入射相同面密度的Al、PE、水三种屏蔽材料,通过分析射线穿过屏蔽材料后在水模体中的深度剂量分布、屏蔽材料内的能量沉积、屏蔽材料产生的次级粒子能谱,对不同面密度下三种材料的质子屏蔽效果进行了对比分析。结果表明:Al、PE、水三种屏蔽材料中,使用PE屏蔽材料比Al屏蔽材料节省27.29%的重量即可实现对100 MeV质子的有效屏蔽,水屏蔽材料比Al材料节省22.46%的屏蔽材料重量;面密度为6.48 g/cm~2PE材料对100 MeV质子的屏蔽能力比同等面密度下Al材料增加59.23%;等效Al厚度为27 mm时,PE屏蔽比Al屏蔽能力增加达到最大值82.96%。     

真空100 keV质子辐照对石墨膜热性能的影响

研究了25 μm石墨膜在能量100 keV最大注量2.5×10¹⁵ p/cm²的真空质子辐照条件下的微观结构和热性能，采用拉曼光谱（Raman spectrum）、X射线衍射（XRD）、X射线光电子能谱（XPS）进行微观结构分析，采用激光闪射法（LFA）进行热性能分析。石墨膜晶面间距为0.335 83 nm，石墨化度为95.0%。结果发现，质子辐照会导致石墨膜表层产生缺陷，片层间距增大，石墨化度降低，氧含量升高；随着质子辐照注量的增加，Raman光谱中D和G峰的积分面积比表明缺陷密度不断增加。25 μm石墨膜经过能量为100 keV注量为2.5×10¹⁵ p/cm²质子辐照后，石墨膜热扩散系数无明显变化。     

空间重粒子入射屏蔽材料的蒙特卡罗模拟

针对空间辐射环境中银河宇宙射线重离子的屏蔽防护问题,使用基于蒙特卡罗方法的Geant4软件模拟330 MeV/n ~(12)C粒子入射铝、聚乙烯、水、液态氢4种屏蔽材料,分析了~(12)C粒子在4种屏蔽材料内的深度剂量分布;在Geant4中建立MIRD人体模型,分析了~(12)C粒子入射4种屏蔽材料后在人体睾丸器官内的吸收剂量;对每种次级粒子在器官内的吸收剂量进行比对,分析了~(12)C粒子入射PE材料产生的次级质子和次级中子能谱。结果表明:330 MeV/n ~(12)C粒子在液态氢中的入射深度为9.66 g/cm~2,在Al中的入射深度为液态氢中入射深度的2.63倍,~(12)C粒子入射5 g/cm~2Al屏蔽材料后在器官内的吸收剂量为2.98×10~(-14 ) Gy/Ion,在液态氢屏蔽后器官内的吸收剂量为2.29×10~(-14 ) Gy/Ion,与Al屏蔽相比吸收剂量降低23.2%。     

热控涂层电子辐照效应

研究防静电Kapton二次表面镜(ITO/Kapton/Al)、S781白漆两种典型热控涂层,在不同能量电子辐照后太阳吸收比退化情况,并利用X射线光电子能谱和扫描电子显微镜对样品表面的成分和形貌进行了分析。结果表明:相同电子注量下,不同能量电子对样品的太阳吸收比退化作用程度是有区别的。而样品光谱反射率、表面形貌、表面成分的损伤效应类似,说明不同能量电子辐照下,样品的退化机理是一致的。     

空间高能宇宙辐射探测设施HERD

空间高能宇宙辐射探测设施HERD主要科学目标为暗物质的搜寻、原初宇宙射线各成分能谱的精细测量以及伽玛射线巡天观测。HERD主要由一个五面灵敏的三维成像量能器和除底面之外全包络的硅径迹探测器构成。量能器包括约1万块硅酸钇镥(LYSO)晶体,实现入射粒子能量测量以及入射粒子种类的鉴别;硅径迹探测器由x-y方向正交排列的硅微条探测器组成,实现入射粒子方向、径迹的测量并测量入射粒子电荷。HERD的主要设计指标为:100Ge V以上能区的电子和伽玛射线探测能量分辨为1%,10 Ge V到1 Pe V能区的质子探测能量分辨为20%;200 Ge V时电子和弥散伽玛射线的有效几何因子大于3 m2sr,100 Te V时宇宙线核素的有效几何因子大于2 m2sr。量能器晶体创新性地采用波长位移光纤+ICCD读出方案,提高了在轨运行工程可行性。     

CFRP/Al制孔分层临界轴向力研究

针对CFRP/Al在钻削加工中容易产生分层缺陷,而临界轴向力是表征叠层材料制孔损伤的基本参数,本文基于能量法建立了钻削Al/CFRP、CFRP/Al产生分层损伤的临界轴向力模型,并利用Abaqus软件对CFRP/Al钻削过程进行了数值模拟,得到了轴向力变化曲线。     

激光等离子体点源减阻技术中入射能量对气动阻力的影响

数值模拟了来流马赫数为5时的圆球绕流冷流场,以及来流与头部驻点附近注入激光能量而产生的等离子体相互耦合形成的流场的演化过程。计算结果表明:施加局部能量点源能够改变原有的弓形激波结构,使其变为斜激波,从而减小气动阻力;气动阻力随入射激光能量的增大而逐渐减小,当入射激光能量为1.1 J时,气动阻力减小的百分比高达40%。     

固体火箭发动机绝热层缺陷对药柱燃面影响的数值模拟

发动机绝热层人工脱粘层局部产生缺陷时,经柱燃面曲线偏离设计曲线,导致发动机２内弹道性能也偏离设计为了模拟这种缺陷对药柱燃面的影响,扩展了原通用坐标程序地计算范围,并又新增加了一些基本图形的算法。改进后的算法可适用于绝热层有或没有缺陷的药柱燃面计算。针对绝热层缺陷建立了三种燃烧模型,计算分析了缺陷类型、结构与位置尺寸对药柱燃面的影响,为分析绝热层有缺陷的发动机性能的基础。     

原子氧对Kapton／Al薄膜性能影响研究

模拟空间环境下原子氧辐照条件,通过采用固定的原子氧束流密度进行不同时间辐照试验,研究了温控涂层材料Kapton/Al薄膜的质量损失、光学性能、表面形貌和表面粗糙度的演化规律.试验结果表明,原子氧对材料的剥蚀量与原子氧的作用时间成正比例关系.材料辐照后太阳吸收率发生明显变化,而辐射率几乎不发生变化.辐照后试样表面的粗糙度,是影响太阳吸收率变化主要因素.随着辐照时间的增长,材料表面粗糙度增加,导致太阳吸收率增大.     

进口斜激波、膨胀波干扰下等直隔离段内的激波串特性

 超燃冲压发动机的隔离段在实际工作中会受到进气道唇罩激波及肩部膨胀扇的显著干扰,本文针对这一特定问题进行了专门研究。提出了唇罩入射激波及肩部膨胀扇的模拟方法,并利用德国Achen的风洞试验对其进行了检验,而后以此研究了入射激波及肩部膨胀扇干扰下隔离段内激波串的基本形态,并分析了出口反压和激波入射位置的影响。仿真结果表明：当激波串在隔离段内不断前移时,受唇罩入射激波及其反射激波的干扰,其高速核心区交替地偏向上下壁面;与无激波入射的情况相比,此时激波串的耐反压能力显著降低,且入射点位置越高,降低幅度越大,管道内的沿程静压分布规律与Waltrup经验公式偏离程度也越来越大。该文结果可为进气道/隔离段的一体化设计提供依据。     

ATS-6 Solar Cosmic Ray and Trapped Particle Experiment

The Solar Cosmic Ray and Trapped Particle Experiment was designed to study the entry, propagation, and loss of solar cosmic rays and the acceleration and loss of trapped electrons and protons in the magnetosphere. Two orthogonal proton and alpha partical telescopes measure protons from 300 keV to 250 MeV and alphas from 2 MeV to 200 MeV. Electron spectrometers measure electrons from 50 keV to 1 MeV and are used in conjunction with the 300-keV to 1.2-MeV proton channels to study the injection of electrons and protons into the magnetosphere during substorms. Two solar cosmic ray events were observed during the first four months of operation. The first of these began on July 3, 1974, and is probably one of the more complicated events in recent years. There were numerous flares and sudden commencements as well as intense fluxes of low energy plasma with a severly perturbed magnetosphere. The second solar cosmic ray event was smaller and was associated with an isolated east limb flare. The first increase was observed on September 11, 1974.     

Space Weather and the Ground-Level Solar Proton Events of the 23rd Solar Cycle

Solar proton events can adversely affect space and ground-based systems. Ground-level events are a subset of solar proton events that have a harder spectrum than average solar proton events and are detectable on Earth’s surface by cosmic radiation ionization chambers, muon detectors, and neutron monitors. This paper summarizes the space weather effects associated with ground-level solar proton events during the 23rd solar cycle. These effects include communication and navigation systems, spacecraft electronics and operations, space power systems, manned space missions, and commercial aircraft operations. The major effect of ground-level events that affect manned spacecraft operations is increased radiation exposure. The primary effect on commercial aircraft operations is the loss of high frequency communication and, at extreme polar latitudes, an increase in the radiation exposure above that experienced from the background galactic cosmic radiation. Calculations of the maximum potential aircraft polar route exposure for each ground-level event of the 23rd solar cycle are presented. The space weather effects in October and November 2003 are highlighted together with on-going efforts to utilize cosmic ray neutron monitors to predict high energy solar proton events, thus providing an alert so that system operators can possibly make adjustments to vulnerable spacecraft operations and polar aircraft routes.     

水工质微波加热推力器的击穿点火与离解损失估算

对水工质微波等离子推力器(MPT),用微波击穿气体放电产生等离子体的条件,数值估算了其点火的可行性;通过化学动力学计算证明了水工质MPT中离解损失的存在,并初步估算了理解损失的大小。结果表明,在1 kW的输入功率下水工质MPT的点火启动并不特别困难,从点火到稳定工作,能量吸收从场致电离、碰撞电离转变为热电离、碰撞电离和场致电离;水在MPT工作过程中会发生离解,离解损失在各类能量损失中所占的比重较大。     

The Polar Ionospheric X-ray Imaging Experiment (PIXIE)

The Polar Ionospheric X-ray Imaging Experiment (PIXIE) is an X-ray multiple-pinhole camera designed to image simultaneously an entire auroral region from high altitudes. It will be mounted on the despun platform of the POLAR spacecraft and will measure the spatial distribution and temporal variation of auroral X-ray emissions in the 2 to 60 keV energy range on the day side of the Earth as well as the night. PIXIE consists of two pinhole cameras integrated into one assembly, each equipped with an adjustable aperture plate that allows an optimum number of nonoverlapping images to be formed in the detector plane at each phase of the satellite's eccentric orbit. The aperture plates also allow the pinhole size to be adjusted so that the experimenter can trade off spatial resolution against instrument sensitivity. In the principal mode of operation, one aperture plate will be positioned for high spatial resolution and the other for high sensitivity. The detectors consist of four stacked multiwire position-sensitive proportional counters, two in each of two separate gas chambers. The front chamber operates in the 2–12 keV energy range and the rear chamber in the 10–60 keV range. All of the energy and position information for each telemetered X-ray event is available on the ground. This enables the experimenter to adjust the exposure timepostfacto so that energy spectra of each X-ray emitting region can be independently accumulated. From these data PIXIE will provide, for the first time, global images of precipitated energetic electron spectra, energy inputs, ionospheric electron densities, and upper atmospheric conductivities.     

Measurements of low energy electrons and ions during long-lived solar particle events

Following a solar flare in April 1979, a stream of ions and electrons appeared in interplanetary space for about 8 days. The ions follow a classic ESP pattern. Large fluxes of low energy (2–11 keV) electrons are also present throughout the event. Several distinct populations of these electrons can be identified in association with filaments of interplanetary magnetic field. The electron energy spectrum is remarkably well fit by a power law exponent -2.7 during most of the event.The pitch angle distribution of the low energy electrons are complex and undergo many changes. Weak pitch angle scattering and adiabatic effects play a role in shaping these distributions. The low energy electron fluxes increase following the strong interplanetary shock on 5 April 1979.An invited paper presented at STIP Workshop on Shock Waves in the Solar Corona and Interplanetary Space, 15–19 June, 1980, Smolenice, Czechoslovakia.Physics Department and Space Sciences Laboratory.Space Sciences Laboratory.     

The Magnetic Electron Ion Spectrometer (MagEIS) Instruments Aboard the Radiation Belt Storm Probes (RBSP) Spacecraft

This paper describes the Magnetic Electron Ion Spectrometer (MagEIS) instruments aboard the RBSP spacecraft from an instrumentation and engineering point of view. There are four magnetic spectrometers aboard each of the two spacecraft, one low-energy unit (20–240 keV), two medium-energy units (80–1200 keV), and a high-energy unit (800–4800 keV). The high unit also contains a proton telescope (55 keV–20 MeV). The magnetic spectrometers focus electrons within a selected energy pass band upon a focal plane of several silicon detectors where pulse-height analysis is used to determine if the energy of the incident electron is appropriate for the electron momentum selected by the magnet. Thus each event is a two-parameter analysis, an approach leading to a greatly reduced background. The physics of these instruments are described in detail followed by the engineering implementation. The data outputs are described, and examples of the calibration results and early flight data presented.     

Charged-particle telescope experiment on Clementine

The charged-particle telescope (CPT) onboard the Clementine spacecraft measured the fluxes of energetic protons emitted in solar energetic particle events. Protons in the energy range from 10 to 80 MeV were of greatest interest for radiation effects such as total dose and single event upsets. Energetic electrons were also of interest for spacecraft charging and their contribution to total dose. The lower-energy CPT electron channels (25-500 keV) were mainly of geophysical interest. While orbiting the moon, the CPT observed the wake created by the moon when it blocked the flow of energetic particles in the magnetotail region. The CPT provided opportunities to observe energetic electron bursts during magnetic storms and magnetospheric substorms. CPT data are particularly useful in multispacecraft studies of interplanetary disturbances and their interaction with the magnetosphere. The proton channels on the CPT provided data on solar energetic protons and storm-time protons associated with the passage of an interplanetary shock at 0903 UT on Feb. 21, 1994. Results are compared with those from GOES-7, SAMPEX, and GEOTAIL.     

ATS-6 Synchronousi Orbit Trapped Radiation Studies with an Electron-Proton Spectrometer

The University of Minnesota Electron-Proton Spectrometer Experiment consists of two nearly identical detector assemblies. One of these assemblies was mounted in a position fixed on the satellite in the Environmental Measurements Experiments (EME) east direction and the other was rotated so that the spectrometer scanned a range of spatial directions covering 1800 from EME north to EME south through west. Each of the detector assemblies is a magnetic spectrometer containing four gold-silicon surface barrier detectors. This instrument provides a very clean separation between protons and electrons by the combination of pulse height analysis and magnetic deflection. Each detector assembly measures protons in three nominal energy ranges (30-50 keV), (50-160 keV), and (120-514 keV). Electrons also are measured in three energy intervals (30-50 keV), (150-214 keV), and (more than 500 keV). Data are transmitted from the experiment at rates as high as 8 measurements/s. Decreases in the flux of the energetic electrons and protons followed by very rapid increases are frequently observed on the nightside during periods of geomagnetic activity. Separation of temporal and spatial effects is possible using proton gradient information obtained when the detector systems are oppositely directed. Using this technique, the decreases have been interpreted as motion of the trapping region equatorward and Earthward of the satellite. The boundary motion associated with the particle recovery shows a marked local time dependence. Particle increases observed in the evening sector have been interpreted as motion from Earthward and equatorward of Applications Technology Satellite-6 (ATS-6).     

The Solar Electron and Proton Telescope for the STEREO Mission

The Solar Electron and Proton Telescope (SEPT), one of four instruments of the Solar Energetic Particle (SEP) suite for the IMPACT investigation, is designed to provide the three-dimensional distribution of energetic electrons and protons with good energy and time resolution. This knowledge is essential for characterizing the dynamic behaviour of CME associated and solar flare associated events. SEPT consists of two dual double-ended magnet/foil particle telescopes which cleanly separate and measure electrons in the energy range from 30–400 keV and protons from 60–7?000 keV. Anisotropy information on a non-spinning spacecraft is provided by the two separate telescopes: SEPT-E looking in the ecliptic plane along the Parker spiral magnetic field both towards and away from the Sun, and SEPT-NS looking vertical to the ecliptic plane towards North and South. The dual set-up refers to two adjacent sensor apertures for each of the four view directions: one for protons, one for electrons. The double-ended set-up refers to the detector stack with view cones in two opposite directions: one side (electron side) is covered by a thin foil, the other side (proton side) is surrounded by a magnet. The thin foil leaves the electron spectrum essentially unchanged but stops low energy protons. The magnet sweeps away electrons but lets ions pass. The total geometry factor for electrons and protons is 0.52 cm²?sr and 0.68 cm²?sr, respectively. This paper describes the design and calibration of SEPT as well as the scientific objectives that the instrument will address.