2．5DC／SiC复合材料的热物理性能

分别采用热膨胀仪和激光脉冲导热仪测试2.5D C/SiC复合材料从室温到1400℃纵向、横向的热膨胀系数和厚度方向的热扩散系数.结果表明,2.5D C/SiC复合材料的热膨胀系数随温度的升高而缓慢升高,在350℃和700℃附近出现波动,且横向的热膨胀系数略高于纵向.热扩散系数随温度的升高逐渐降低,且下降速率随温度的升高而变缓.CVD SiC涂层后,材料热扩散系数提高1～2倍.     

新型Sip/4032Al复合材料热物理性能研究

采用挤压铸造方法,制备了高体积分数的Si_p/4032Al复合材料。显微组织观察表明,复合材料组织致密,颗粒分布均匀,材料中没观察到孔洞和缺陷;复合材料的线膨胀系数介于(8．1～12)×10~(-6)/K之间可调,并且随着增强体含量的增加而降低,退火后线膨胀系数略有降低,Kerner模型能够较好的预测复合材料的线膨胀系数;复合材料的热导率可达103 W/(m·K),随着增强体含量的增加略有下降,退火处理后热导率略有升高,热导率计算结果均大于测试值。     

Observational constraints on dark matter in the universe

Application of the cosmic virial theorem to galaxy redshift surveys suggests an open universe - if the dark material is distributed in the same way as galaxies. Here we investigate four redshift surveys. We present new results on the amplitudes of the two- and three-point galaxy correlation functions and we estimate the relative peculiar velocities in the deep redshift survey of Kirshner and co-workers (1983). Next, we review evidence which suggests that dark material is clustered on scales comparable to the optical radii of galaxies. In particular, we use spectroscopic and photometric observations to set constraints on the mass distribution in elliptical galaxies.     

球料比对羰基铁粉片型化演变和电磁性能的影响

以无水乙醇为隔离剂,通过湿法球磨制备了片型羰基铁粉,研究了球料比对片型化过程、电磁性能的影响。结果表明：增加球料比,羰基铁粉片型化更充分,晶粒尺寸减小;粒子的各向异性提高了片型羰基铁粉的微波电磁性能。以环氧树脂为基体树脂,填充体积分数30％的吸波剂制备了1．0mm 单层吸波涂层,在 X-Ku 波段反射率小于－7．5dB 的带宽大于10GHz,涂层最小面密度为2．96kg ／m2。     

固体冲压发动机燃气阀用C/SiC复合材料研究

采用“化学气相渗透法 先驱体浸渍裂解法”(CVI PIP)混合工艺制备了固体冲压发动机燃气阀用3D C/S iC复合材料,并对复合材料的显微结构和力学性能进行了研究。复合材料的密度为2.1 g/cm3,复合材料的室温剪切强度和轴向弯曲强度分别为55 MPa和643 MPa。在断裂过程中,复合材料表现出明显非灾难性的韧性断裂行为,试样断裂面存在大量的拔出纤维。复合材料具有优异的绝热性能,Z向热导率为14.5 W/(m.K),X-Y面内热导率为5.0 W/(m.K)。研制的3D C/S iC复合材料燃气阀成功通过冷气轴向抗冲击试验和发动机高温搭载试验考核。     

超声 C 扫描在 C/ SiC 复合材料与钛合金薄板钎焊质量中的应用

通过超声水浸脉冲法对C/SiC复合材料的声阻抗进行测定,结果表明,其声阻抗介于(4.0~4.7)×106kg/m2s之间;未焊合时界面反射系数约为1,焊接良好时界面反射系数介于0.71~0.74之间。为使未焊合时界面反射信号幅度比焊接良好时至少相差6 d B,C扫描检测时应监测二次以上界面反射信号幅度,并采用金相的方法对C扫描结果进行验证,二者一致性较好。     

Operant responding following exposure to HZE particles and its relationship to particle energy and linear energy transfer

On exploratory class missions astronauts will be exposed to a variety of heavy particles (HZE particles) which differ in terms of particle energy and particle linear energy transfer. The present experiments were designed to evaluate how these physical characteristics of different particles affect cognitive performance, specifically operant responding. Following exposure to ²⁸Si, ⁴⁸Ti, ¹²C and ¹⁶O particles at the NASA Space Radiation Laboratory rats were tested for their ability to respond appropriately to changes in reinforcement schedules using an operant task. The results showed that the effectiveness of different particles in disrupting cognitive performance, defined as the lowest dose that produced a performance decrement, varied as a function of the energy of the specific particle: for comparisons between different energies of the same particle (e.g., ⁵⁶Fe) the effectiveness of the particle was directly proportional to particle linear energy transfer, whereas for comparisons between different particles (e.g., ⁵⁶Fe and ¹⁶O) effectiveness was inversely proportional to particle linear energy transfer. The results are discussed in terms of the mechanisms that influence the effectiveness of different particles and energies and in terms of their implications for analyzing the possible risks to astronauts of decrements in cognitive performance following exposure to HZE particles on long-duration exploratory class missions.     

Cosmic radiation exposure of aircraft occupants on simulated high-latitude flights during solar proton events from 1 January 1986 through 1 January 2008

From 1 January 1986 through 1 January 2008, GOES satellites recorded 170 solar proton events. For 169 of these events, we estimated effective and equivalent dose rates and doses of galactic cosmic radiation (GCR) and solar cosmic radiation (SCR), received by aircraft occupants on simulated high-latitude flights. Dose rate and dose estimates that follow are for altitudes 30, 40, 50, and 60 kft, in that order.     

Study of correlations between waves and particle fluxes measured on board the DEMETER satellite

The topic of relativistic electron dynamics in the outer radiation belt has received considerable attention for many years. Nevertheless, the problem of understanding the physical phenomenon involved is far from being resolved. In this paper, we use DEMETER observations to examine the variations of the energetic electron fluxes and ELF/VLF wave intensities in the inner magnetosphere during the intense 8 November 2004 magnetic storm. Electron flux spectra and associated wave intensity spectra are analysed throughout the magnetic storm and common characteristics or differences to other storm events are retained. The overall objective of this study is to identify and derive parameters that are relevant for particle flux modelling; the time constant characterizing the persistent decay after particle enhancement was found to be one of these important model parameters.The analysis of the 8 November 2004 event reveals that for L-shell parameter higher than 4, an electron flux dropout is observed during the storm’s main phase for electrons in the energy range 0.1–1 MeV, as has been reported from other measurements. Characteristic wave spectra accompanying this phase are analysed. They show a typical enhancement in the frequency range 0.3–10 kHz at onset for all L-shell values under consideration (2 < L < 5). During the first stage of the recovery phase, the electron fluxes are increased to a level higher than the pre-storm level, whereas the level of wave intensity in the frequency range observed below 300 Hz is at its highest. In the second stage, the particle flux decrease goes hand in hand with a global wave activity decline, the relaxation time of the latter being smaller than the former’s one. In some other cases, long-lasting electron enhancement associated with constant wave activity has been observed during this latter stage. For the above mentioned storm, while at low L values the decay time constants are higher for low energy electrons than for high energy electrons, this order is reversed at high L values. At about L = 3.6 the time constant is independent of electron energy.