环氧树脂耐电子辐照性能

研究了电子辐照对几种4,4’-二氨基二苯甲烷固化的环氧树脂造成的破坏效应.结果表明:在1.4 MeV电子辐照时,环氧树脂会变色、失重、开裂,同时力学性能下降.实验结果表明:双酚A二缩水甘油醚(DGEBA),N,N,N’,N’-四缩水甘油基-4,4’-二氨基二苯甲烷(TGDDM),对氨基苯酚三缩水甘油环氧树脂(TGPAP),DGEBA/TGDDM和DGEBA/TGPAP共混物均能承受106 Gy的吸收剂量.而DGEBA/TGPAP共混物,能承受107 Gy的吸收剂量.环氧树脂抗辐照性能的次序为DGEBA/TGPAP＞ DGEBA/TGDDM ＞TGPAP≈TGDDM＞DGEBA.环氧树脂经电子辐照后压缩模量增加,表明在辐照效应中交联机理占主导,DMA和DSC分析也证实了这一点.     

辐射交联热缩制品

本成果研制的产品是采用聚烯烃材料加入添加剂热塑成型 ,经高能电子辐照处理后 ,加工定型制成。辐射交联热缩套管具有热缩性能 ,当加热到一定温度时 ,可收缩到原来挤塑时的形状和尺寸 ,即产生“记忆效应”。加工方便 ,质量优异 ,成本低廉 ,节省能源 ,没有污染。产品热缩温度为 115℃～ 130℃ ;使用温度为 - 5 5℃～ 80℃ ;脆化温度为 - 70℃ ;耐电压强度 >15ｋＶ/ｍｍ·ｍｉｎ ;体积电阻率 >5 .4 2× 10 16Ω·ｃｍ ;抗张强度 (2 3℃ ) >15 .68ＭＰａ ;极限伸长率 (2 3℃ ) >4 0 0 % ;纵向收缩率 <10 %。辐射交联热缩制品可广泛应用于航天、…     

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。     

三维全五向编织复合材料的切边效应

对切割与未切割的三维全五向(3DF5D)编织复合材料进行了纵向拉伸力学性能研究。首先分别对2种编织角下3种不同情况(未切割、沿厚度方向切边和沿宽度方向切边)的试件进行了力学性能实验,实验结果表明,沿着厚度方向切边使材料的刚度和强度分别下降了约10%和25%;沿着宽度方向切边使材料刚度和强度分别下降了约3%和18%;进一步通过有限元数值模拟对上述实验过程进行了仿真计算,得到了单胞的损伤演化过程、破坏机理以及应力-应变曲线。最后对实验结果和计算结果进行了对比,结果显示二者吻合良好。研究结果表明,三维全五向编织复合材料的编织角越大,拉伸刚度和强度会越小;试件尺寸越大,厚度方向和宽度方向切边的影响越小,并趋于定值。     

两种典型铺层玻璃纤维复合材料的拉伸力学行为

利用电子万能实验机及分离式Hopkinson拉杆对玻璃纤维增强复合材料S4C9-1200/SY14的两种不同铺层角度层合板([0]16和[±45]4S)进行了应变率为10-3～103s-1下的单轴拉伸力学性能测试。从应力应变曲线和试样破坏断口分析了材料的应变率效应、纤维损伤和界面脱粘损伤。实验结果表明:[0]16层板破坏时表现出典型的不规则脆性破坏,纤维的损伤具有初始门槛值,而纤维的强化存在应变率门槛效应。[±45]4S层板主要破坏方式是纤维与基体的脱粘,损伤发展近似线性。应变率高于强化门槛时,[±45]4S层板表现出极强的应变率依赖性,极限强度能提高10%～50%。     

2D C/SiC 复合材料的静压痕力的损伤表征

为考察2D C/SiC 复合材料在外力作用下产生的不可见损伤对其力学性能的影响。通过静压痕实验引入损伤,采用红外热波成像和残余性能测试的方法,表征2D C/SiC 复合材料的损伤。结果表明:施加能量为0.75 J时,复合材料内部开始产生损伤, 施加能量为1.8 J(接触力1 700 N、压痕深1 mm)时,损伤模式发生转变;随着损伤程度的加重,残余压缩强度下降率约为残余拉伸强度下降率的2倍。     

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%。     

碳纤维束大小对2D C/SiC复合材料力学性能的影响

通过对2种丝束大小平纹机织的碳纤维布增强SiC(C/SiC)复合材料的力学性能实验,研究了纤维束丝束大小(1k和3k)对复合材料力学性能的影响。实验结果表明:纤维束大小不同,导致纤维束弯曲程度和复合材料孔隙率不同,从而使得C/SiC复合材料力学性能产生差异。     

航天器用Parylene-C涂覆材料空间辐照适用性研究

派瑞林（Parylene）薄膜主要用于功率电刷的三防，确保电功率的稳定传输。本文对两种规格（17和27 μm）Parylene薄膜的厚度、热性能、绝缘性能、在铍青铜上的附着性能以及耐空间辐照性进行了研究。结果表明：通过真空气相沉积法制备的Parylene-C涂覆材料厚度误差可控在2 μm内；膜层在铍青铜上的附着力等级为1级，薄膜热分解温度为453 ℃，两种厚度薄膜击穿电压分别为3.65 kV（17 μm）和5.27 kV（27 μm）；经2.5×10¹⁵ p/cm²质子辐照后，膜层外观均完好，附着性能、热性能、绝缘性能仍满足工程使用需求；经2.5×10¹⁶ e/cm²电子辐照后，膜层出现严重开裂、起皮现象。对电子辐照前后膜层的热性能、红外结构等进行了进一步的研究，分析了电子辐照后膜层的失效机理并获得了Parylene-C涂覆材料膜层耐空间电子辐照上限为1×10¹⁴ e/cm²。     

不同钝化工艺SiO2薄膜的辐射缺陷

为研究不同钝化工艺栅介质用SiO₂薄膜的高能电子辐射缺陷特征，采用能量为1 MeV的高能电子在辐照注量为1×10¹⁵ e/cm²、5×10¹⁵ e/cm²和1×10¹⁶e/cm²下对三种不同钝化工艺（I，700 nm SiN + 500 nm PSG;II，1.2 μm SiN;III，700 nm PSG + 500 nm SiN）的SiO₂薄膜进行了辐照试验。拉曼光谱和X射线光电子能谱结果表明I和III钝化工艺SiO₂薄膜形成了非晶硅及双氧根离子，傅立叶红外光谱结果表明I钝化工艺SiO₂薄膜形成缺陷结构未知的A₁、A₂、B₁及B₂缺陷；II钝化工艺SiO₂薄膜形成A₁、B₁、及 缺陷；III钝化工艺SiO₂薄膜形成A₁、及B₂缺陷。     

WIND Observations of Suprathermal Electrons in the Interplanetary Medium

We review some of the new results for suprathermal electrons obtained with the 3-D Plasma and Energetic Particle Instrument on the WIND spacecraft, which provides high sensitivity electron and ion measurements from solar wind thermal plasma up to ≳MeV energies. These results include: (1) the observation of solar impulsive electron events extending down to ∼0.5 keV energy; (2) the observation of a turnover at ∼12 keV for electrons in a gradual large solar energetic particle (LSEP) event; (3) the detection of a quiet-time population (the ‘superhalo’) of electrons extending up to ∼100 keV energy; and (4) the probing of the magnetic topology and source region for magnetic clouds, using electrons. These unique WIND measurements are highly complementary to the particle composition measurements which will be made by ACE. This revised version was published online in June 2006 with corrections to the Cover Date.     

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.     

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.     

真空电子辐照对碳纤维/ 氰酸酯复合材料的影响

利用空间带电粒子模拟设备模拟真空电子辐照环境,研究真空电子辐照条件下碳纤维/氰酸酯复合材料层间剪切强度和质量损失率变化规律,并利用XPS和SEM对辐照前后复合材料表面性质和断口形貌进行分析和表征。结果表明:150 keV真空电子辐照作用对碳纤维/氰酸酯复合材料表面影响较大,随着真空电子辐照注量增加复合材料质量损失率先快速增加后趋于平缓,而层间剪切强度先增加后略有降低。     

ATS-6 Energetic Particle Radiation Measurement at Synchronous Altitude

The Aerospace Corporation energetic electron-proton spectrometer operating on Applications Technology Satellite-6 (ATS-6) detects energetic electrons in four channels between 140 keV and greater than 32 MeV, and measures energetic protons in five energy channels between 2.3 and 80 MeV and energetic alpha particles in three channels between 9.4 and 94 MeV. After more than a year of operation in orbit, the experiment continues to return excellent data on the behavior of energetic magnetospheric electrons as well as information regarding the fluxes of solar protons and alpha particles.     

Solar gamma rays

The theory of gamma-ray production in solar flares is treated in detail. Both lines and continuum are produced. The strongest line predicted at 2.225 MeV with a width of less than 100 eV and detected at 2.24±0.02 MeV, is due to neutron capture by protons in the photosphere. Its intensity is dependent on the photospheric ³He abundance. The neutrons are produced in nuclear reactions of flare accelerated particles which also produce positrons and prompt nuclear deexcitation lines. The strongest prompt lines are at 4.43 MeV from ¹²C and at 6.2 from ¹⁶O and ¹⁵N. These lines result from both direct excitation and spallation. The widths of individual prompt lines are determined by nuclear kinematics. The width of the 4.43 MeV line is 100 keV and that of the 6.2 MeV feature is 300 keV. Both these lines have been observed from a solar flare. Other potentially observable lines are predicted at 0.845 and 1.24 MeV from ⁵⁶Fe, at 1.63 MeV principally from ¹⁴N and ²⁰Ne, at 1.78 MeV from ²⁸Si, at 5.3 MeV from ¹⁵O and ¹⁵N, and at 7.12 MeV from ¹⁶O. The widths of the iron lines are only a few keV, while those of the other lines are about 100 keV. The only other observed line is at 0.511 MeV from positron annihilation. The width of this line is determined by the temperature, and its temporal variation depends on the density of the ambient medium in the annihilation region. Positrons can also annihilate from the ³ S state of positronium to produce a 3-photon continuum below 0.511 MeV. In addition, the lines of ⁷Li and ⁷Be at 0.478 keV and 0.431 keV, which have kinematical widths of 30 keV, blend into a strong feature just below the 0.511 MeV line.From the comparison of the observed and calculated intensities of the line at 4.4 MeV to that of the 2.2 MeV line it is possible to obtain information on the spectrum of accelerated nuclei in flares. Moreover, from the absolute intensities of these lines the total number of accelerated nuclei at the Sun and their heating of the flare region can be estimated. We find that about 10³³ protons of energies greater than 30 MeV were produced in the 1972, August 4 flare.The gamma-ray continuum, produced by electron bremsstrahlung, allows the determination of the spectrum and number of accelerated electrons in the MeV region. From the comparison of the line and continuum intensities we find a proton-to-electron ratio of about 10 to 10² at the same energy for the 1972, August 4 flare. For the same flare the protons above 2.5 MeV which are responsible for the gamma-ray emission produce a few percent of the heat generated by the electrons which make the hard X-rays above 20 keV.NAS-NRC Resident Research Associate.Research supported by the National Science Foundation under Grant GP 31620.     

A three-dimensional plasma and energetic particle investigation for the wind spacecraft

This instrument is designed to make measurements of the full three-dimensional distribution of suprathermal electrons and ions from solar wind plasma to low energy cosmic rays, with high sensitivity, wide dynamic range, good energy and angular resolution, and high time resolution. The primary scientific goals are to explore the suprathermal particle population between the solar wind and low energy cosmic rays, to study particle accleration and transport and wave-particle interactions, and to monitor particle input to and output from the Earth's magnetosphere.Three arrays, each consisting of a pair of double-ended semi-conductor telescopes each with two or three closely sandwiched passivated ion implanted silicon detectors, measure electrons and ions above 20 keV. One side of each telescope is covered with a thin foil which absorbs ions below 400 keV, while on the other side the incoming <400 keV electrons are swept away by a magnet so electrons and ions are cleanly separated. Higher energy electrons (up to 1 MeV) and ions (up to 11 MeV) are identified by the two double-ended telescopes which have a third detector. The telescopes provide energy resolution of E/E0.3 and angular resolution of 22.5°×36°, and full 4 steradian coverage in one spin (3 s).Top-hat symmetrical spherical section electrostatic analyzers with microchannel plate detectors are used to measure ions and electrons from 3 eV to 30 keV. All these analyzers have either 180° or 360° fields of view in a plane, E/E0.2, and angular resolution varying from 5.6° (near the ecliptic) to 22.5°. Full 4 steradian coverage can be obtained in one-half or one spin. A large and a small geometric factor analyzer measure ions over the wide flux range from quiet-time suprathermal levels to intense solar wind fluxes. Similarly two analyzers are used to cover the wide range of electron fluxes. Moments of the electron and ion distributions are computed on board.In addition, a Fast Particle Correlator combines electron data from the high sensitivity electron analyzer with plasma wave data from the WAVE experiment (Bougeretet al., in this volume) to study wave-particle interactions on fast time scales. The large geometric factor electron analyzer has electrostatic deflectors to steer the field of view and follow the magnetic field to enhance the correlation measurements.     

Electron,Proton, and Alpha Monitor on the Advanced Composition Explorer spacecraft

The Electron, Proton, and Alpha Monitor (EPAM) is designed to make measurements of ions and electrons over a broad range of energy and intensity. Through five separate solid-state detector telescopes oriented so as to provide nearly full coverage of the unit-sphere, EPAM can uniquely distinguish ions (Ei≳50 keV) and electrons (Ee≳40 keV) providing the context for the measurements of the high sensitivity instruments on ACE. Using a ΔE×E telescope, the instrument can determine ion elemental abundances (E≳0.5 MeV nucl−1). The large angular coverage and high time resolution will serve to alert the other instruments on ACE of interesting anisotropic events. The experiment is controlled by a microprocessor-based data system, and the entire instrument has been reconfigured from the HI-SCALE instrument on the Ulysses spacecraft. Inflight calibration is achieved using a variety of radioactive sources mounted on the reclosable telescope covers. Besides the coarse (8 channel) ion and (4 channel) electron energy spectra, the instrument is also capable of providing energy spectra with 32 logarithmically spaced channels using a pulse-height-analyzer. The instrument, along with its mounting bracket and radiators weighs 11.8 kg and uses about 4.0 W of power. To demonstrate some of the capabilities of the instrument, some initial performance data are included from a solar energetic particle event in November 1997. This revised version was published online in June 2006 with corrections to the Cover Date.