天舟一号空间冷凝实验装置地基冷凝实验

天舟一号（TZ-1）蒸发与冷凝实验装置地面科学匹配实验是优化空间实验参数与两相试验系统技术参数的重要环节.通过地面科学匹配冷凝实验,控制冷凝实验输入条件,观察条件变化给非稳态冷凝换热带来的影响,可为空间实验数据处理提供修正依据.实验内容主要包括:改变冷凝台和蒸气温度,获得换热系数随时间变化的规律,从而指导空间实验数据采集和液池加热;通过实验验证蒸气压力对液膜换热系数的影响.实验还证明了冷凝台温度、蒸气温度、抽气压力等对换热系数也都有很大影响.地面科学匹配实验对于完善实验装置、优化工况与实验参数以及提高实验可靠性具有指导意义.      

3D information from 2D images recorded in the European Modular Cultivation System on the ISS

The European Modular Cultivation System (EMCS) on the ISS allows long-term biological experiments, e.g. on plants. Video cameras provide near real-time 2D images from these experiments. A method to obtain 3D coordinates and stereoscopic images from these 2D images has been developed and is described in this paper. The procedure was developed to enhance the data output of the MULTIGEN-1 experiment in 2007. One of the main objectives of the experiment was to study growth movements of the Arabidopsis plants and the effect of gravity on these. 3D data were important during parts of the experiment and the paper presents the method developed to acquire 3D data, the accuracy of the data, limitations to the technique and ways to improve the accuracy. Sequences of 3D data obtained from the MULTIGEN-1 experiment are used to illustrate the potential of this newfound capability of the EMCS. In the experiment setup, a positional depth accuracy of about ±0.4 mm for relative object distances and an absolute depth accuracy of about ±1.4 mm for time dependent phenomena was reached. The ability to both view biological specimens in 3D as well as obtaining quantitative 3D data added greatly to the scientific output of the MULTIGEN-1 experiment. The uses of the technique to other researchers and their experiments are discussed.     

空间对接机构碰撞试验系统的开发研究

为研究空间对接机构在对接过程中的碰撞现象,研制了碰撞试验系统.探讨了试验系统方案;依据Hertz弹性接触理论,仿真计算了加速度频率特性,确定了加速度传感器的选择原则;利用该系统开展了低速碰撞试验.试验结果表明,该系统能够满足测量对接碰撞力的要求.      

The Scanning Sky Monitor (SSM) on ASTROSAT

The Scanning Sky Monitor is one of the experiments onboard the ASTROSAT, an Indian multiwavelength astronomy satellite mission. This experiment will detect and monitor X-ray transients in the energy band 2–10 keV. It is similar in design to the ASM on RXTE. It consists of position-sensitive proportional counters with one-dimensional mask. We describe the configuration of the experiment. We also discuss some of the results obtained using a detector which has already been fabricated and tested in our laboratory.     

Comparison of fragments created by low- and hyper-velocity impacts

This paper summarizes two new satellite impact experiments. The objective of the experiments was to investigate the outcome of low- and hyper-velocity impacts on two identical target satellites. The first experiment was performed at a low-velocity of 1.5 km/s using a 40-g aluminum alloy sphere. The second experiment was performed at a hyper-velocity of 4.4 km/s using a 4-g aluminum alloy sphere. The target satellites were 15 cm × 15 cm × 15 cm in size and 800 g in mass. The ratios of impact energy to target mass for the two experiments were approximately the same. The target satellites were completely fragmented in both experiments, although there were some differences in the characteristics of the fragments. The projectile of the low-velocity impact experiment was partially fragmented while the projectile of the hyper-velocity impact experiment was completely fragmented beyond recognition. To date, approximately 1500 fragments from each impact experiment have been collected for detailed analysis. Each piece has been weighed, measured, and analyzed based on the analytic method used in the NASA Standard Breakup Model (2000 revision). These fragments account for about 95% of the target mass for both impact experiments. Preliminary analysis results will be presented in this paper.     

The PAMELA Storage and Control Unit

The PAMELA experiment aims to measure with great precision the antimatter present in our Galaxy in the form of high energy particles; in the same time it will measure the galactic, solar and trapped components of cosmic rays. The experiment will be housed on board a Russian Resurs-DK1 satellite and launched in the year 2005 to fly a 350–600 km orbit with an inclination of 70.4°. All operations of the instrument – including data storage – are handled by the PAMELA Storage and Control Unit (PSCU), which is divided in a Central Processing Unit (CPU) and a Mass Memory (MM). The CPU of the experiment is based on a ERC-32 architecture (a SPARC v7 implementation) running a real time operating system (RTEMS). The main purpose of the CPU is to handle slow control, acquire and store data on a 2 GB MM. Communications between PAMELA and the satellite are performed via a 1553B bus. Data acquisition from the sub-detectors (Time-of-Flight counter, Magnetic Spectrometer, Electromagnetic Calorimeter, Anticoincidence shield, Neutron Detector, and Bottom scintillator S4) is performed via a 2 MB/s interface. Download from the PAMELA MM towards the satellite main storage unit is handled by a 16 MB/s bus. The daily amount of data transmitted to ground has been evaluated in not more 20 GB. In this work, we describe the CPU of the experiment and the general software scheme.     

表面钝化对超临界航空煤油静态结焦特性影响

通过静态装置,研究了不锈钢经表面磷化、酸洗钝化以及电解钝化后对超临界压力下航空煤油RP-3热氧化结焦的抑制效果,并对表面钝化层的耐久性做出评估.研究发现,不锈钢的钝化膜层有效地降低不锈钢表面催化活性,按结焦抑制效果排序为:电解钝化>酸洗钝化>磷化;化学稳定性好、耐蚀性强的钝化膜层会延长材料的使用寿命,按钝化膜耐蚀性排序为:电解钝化>酸洗钝化>磷化;综合结焦抑制效果及化学稳定性两个因素考虑,电解钝化为最佳表面钝化方案,但其在高温高腐蚀的煤油环境下长时间实验时易失去钝化效用.     

空间站微重力流体实验设备需求分析

对国际空间站和中国科学实验卫星及载人飞行器上开展的微重力流体实验情况进行论述和分析,重点分析了国际空间站（ISS）微重力流体科学实验设备情况.根据中国空间微重力流体物理科学发展需求,结合国际空间站微重力流体科学实验对设备的需求,提出了未来在中国空间站开展微重力流体实验时空间实验设备需要重点考虑和解决的问题,同时提出相关设计建议.      

Some additional results in the regular balloon monitoring of cosmic rays in the Earth’s atmosphere

The different types of the data recorded in the experiment of the regular balloon monitoring of cosmic rays (carried out since 1957 by Lebedev Physical Institute, Moscow, Russia, in several locations) are described. So called detailed information (the form of each pulse detected by the ground-based receiver) recorded during the last 12 years is discussed in more details. The use of these data both for getting and correcting the standard results of the experiment and for obtaining some additional information on the cosmic rays in the Earth’s atmosphere is considered.     

An experiment to study solar flare effects on radio-communication signals

The occurrence of radio signal fading events caused by ionospheric absorption plays an important role in the performance of radio-communication systems. It is necessary to know the magnitude and time-scale of such events in order to specify technical parameters of the communication system to be used. Generally, fading events are associated with solar flares, which are characterized by sudden increase in the solar X-ray flux that causes an increase in the ionization in the lower ionosphere. The abrupt increase of ionization causes the absorption of radio waves propagating in the Earth–ionosphere wave-guide and is reported as radio signal fading events. A simple experiment to monitor the behavior of lower ionosphere has been carried out at the Southern Space Observatory-SSO/INPE (29.43°S, 53.8°W), located in southern Brazil. The experiment is basically a computer controlled radio receiver that records the received signal strength of Amplitude Modulated (AM) radio signals in the HF (High Frequencies) range. We analyzed data of the 6 MHz beacon signal that has been transmitted by a broadcasting radio station located about 400 km from the observation site. In this work we present initial results of daily variation of the received signal strength and fading events associated with solar flares observed in the 6 MHz signal monitored by the experiment during 2001. X-ray solar flux data from the GOES-8 satellite were used to identify X-ray solar bursts associated with solar flares. Based on the one-year data collected by the experiment, a statistical summary of fading occurrences and their correlation with solar flares, as well as the distributions of time-scales and magnitudes of such events are presented.     

Balloon observations of temporal and spatial fluctuations in stratospheric conductivity

The first campaign of the Polar Patrol Balloon (PPB) experiment (1st-PPB) was carried out at Syowa Station in Antarctica during 1990–1991 and 1992–1993. Based on the results of the 1st-PPB experiment, the next campaign (2nd-PPB) was carried out in the austral summer of 2002–2003. This paper will present stratospheric conductivity results from the 2nd-PPB experiment. In that experiment, three balloons were launched for the purpose of upper atmosphere physics observation (three balloons). Payloads of these three flights were identical with each other, and were launched as close together in time as allowed by weather conditions to constitute a cluster of balloons during their flights. Such a “Balloon Cluster” is suitable to observe temporal evolution and spatial distribution of phenomena in the ionospheric regions and boundaries that the balloons traversed during their circumpolar trajectory. More than 20 days of simultaneous fair weather 3-axis electric field and stratospheric conductivity data were obtained at geomagnetic latitudes ranging from sub-auroral to the polar cap. Balloon separation varied from ∼60 to >1000 km. This paper will present stratospheric conductivity observations with emphasis on the temporal and spatial variations that were observed.     

Selection and hydroponic growth of bread wheat cultivars for bioregenerative life support systems

As part of the ESA-funded MELiSSA program, the suitability, the growth and the development of four bread wheat cultivars were investigated in hydroponic culture with the aim to incorporate such a cultivation system in an Environmental Control and Life Support System (ECLSS). Wheat plants can fulfill three major functions in space: (a) fixation of CO₂ and production of O₂, (b) production of grains for human nutrition and (c) production of cleaned water after condensation of the water vapor released from the plants by transpiration. Four spring wheat cultivars (Aletsch, Fiorina, Greina and CH Rubli) were grown hydroponically and compared with respect to growth and grain maturation properties. The height of the plants, the culture duration from germination to harvest, the quantity of water used, the number of fertile and non-fertile tillers as well as the quantity and quality of the grains harvested were considered. Mature grains could be harvested after around 160 days depending on the varieties. It became evident that the nutrient supply is crucial in this context and strongly affects leaf senescence and grain maturation. After a first experiment, the culture conditions were improved for the second experiment (stepwise decrease of EC after flowering, pH adjusted twice a week, less plants per m²) leading to a more favorable harvest (higher grain yield and harvest index). Considerably less green tillers without mature grains were present at harvest time in experiment 2 than in experiment 1. The harvest index for dry matter (including roots) ranged from 0.13 to 0.35 in experiment 1 and from 0.23 to 0.41 in experiment 2 with modified culture conditions. The thousand-grain weight for the four varieties ranged from 30.4 to 36.7 g in experiment 1 and from 33.2 to 39.1 g in experiment 2, while market samples were in the range of 39.4–46.9 g. Calcium levels in grains of the hydroponically grown wheat were similar to those from field-grown wheat, while potassium, magnesium, phosphorus, iron, zinc, copper, manganese and nickel levels tended to be higher in the grains of experimental plants. It remains a challenge for future experiments to further adapt the nutrient supply in order to improve senescence of vegetative plant parts, harvest index and the composition of bread wheat grains.     

基于电子束蒸发沉积的曲面纳米薄膜均匀性研究

半球谐振子金属化是半球谐振陀螺研制过程中的重要环节，针对半球表面薄膜制备均匀性难以实现的问题，提出了一种将薄膜沉积实验和光学模拟相结合的方法。本文采用电子束蒸发技术在半球上沉积Au薄膜，利用台阶仪测量球面上不同位点的薄膜厚度，将平面上的膜厚等效为半球曲面上的膜厚，研究球面薄膜的均匀性，得出了在半球内外表面上薄膜的膜厚分布；同时对薄膜沉积均匀性进行光学模拟，将半球探测器上辐照度等效为实验中沉积所得到的薄膜厚度，计算得出的半球探测器上辐照度分布与实验测量结果一致性较好，可为半球谐振子纳米薄膜的均匀性制备提供理论基础。     

1+3/2级对转涡轮气动性能试验研究

无导叶对转涡轮是高性能发动机的关键技术之一。本文采用试验方法对1+ 3/2级对转涡轮进行了气动性能研究。本试验分为3个阶段,第1阶段为单独高压涡轮（HPT）试验,第2阶段为加大HPT和低压涡轮（LPT）间轴向间距联合试验,第3阶段为HPT和LPT间正常轴向间距联合试验。在正常轴向间距HPT和LPT试验中,LPT状态的确定通过利用单独HPT试验获得的效率与压比特性反推获得。试验表明,HPT喉道面积减小,而LPT喉道面积增大,这导致在总膨胀比一定情况下,HPT膨胀比增大,LPT膨胀比下降,同时LPT的存在对HPT特性影响不大。在总膨胀比分配中,HPT膨胀比变化很小,而LPT膨胀比变化范围较宽。涡轮级总效率由HPT决定,LPT轮一般相对较低,加大HPT和LPT间轴向间距对LPT性能影响很小。      

空间站材料科学加工试验炉的选择

对国际空间站上各国准备选用的材料科学试验加工炉进行了介绍. 主要呈现以下特点: 高度集成化的材料制备、测试、分析和处理等综合实验能力; 更高的精度、稳定性以及更长的使用寿命; 模块化、标准化和组合式; 应用遥科学实验技术. 从1998 年开始, 为适应未来中国空间站试验的需求, 发展了几类遥科学的空间加工炉及在长时间无人条件下由机器人照料的任意次更换样品的遥操作原型炉. 提出在中国载人航天工程第三步, 即空间站阶段的前期关键技术预研中, 设计和研发功能专业化, 结构模块化和接口标准化的典型功能实验单元, 通过技术集成可以在短时间内高效可靠地完成空间实验设备的配置、集成化和空间应用.      

空间科学实验通用地面检测系统研制

分析了地面检测设备在空间有效载荷研制过程中的作用,提出一种用于对多种空间微重力科学实验设备（载荷）进行地面测试的通用地面检测设备设计方法.通过载荷特性分析,对载荷中的控制对象进行分类.针对不同控制对象使用不同的操作进行控制.将载荷实验过程分解为一系列固定时刻执行的操作,通过配置静态配置表、动作配置表和动态配置表,实现对载荷实验过程的控制.地面检测设备由计算机、电源和RS422通信接口构成.针对不同载荷,使用规格一致的电缆和通信接口,保证地面监测设备的通用性.地面检测设备配合多功能炉、骨髓培养箱、辐射基因箱、煤燃烧箱、蒸发对流箱、导线特性箱及胶体材料箱7台载荷开展研制工作,在各载荷试验参数确定、空间试验流程确定、设备性能测试、环境模拟实验、电磁兼容实验、地面匹配实验以及载荷设备验收等过程中发挥了重要作用.      

APS星敏感器太阳照射影响分析及试验验证

针对APS星敏感器在轨过程中太阳照射问题进行了研究,分析了太阳照射对星敏感器功能和性能的影响,设计了太阳照射相关的试验及验证方案,最后给出了相关试验过程和试验验证结果,明确了分析及试验结论.通过分析和试验结果表明:紫外辐照试验对光学系统透过率无明显影响,且影响在APS星敏感器灵敏度余量范围内;在轨太阳照射对APS星敏感器探测器及整机的功能和性能无影响.相关分析和试验数据可作为星敏感器后续改进设计的依据和参考.     

Solar X-ray Monitor (XSM) on-board Chandrayaan-2 orbiter

The remote X-ray fluorescence spectroscopy is a powerful technique to investigate the elemental abundances in the atmosphere-less planetary bodies. The experiment involves measuring spectra of fluorescent X-rays from lunar surface using a low energy X-ray detector onboard an orbiting satellite. Since the flux of fluorescent X-ray lines critically depend on the flux and spectrum of the incident solar X-rays, it is essential to have simultaneous and accurate measurement of X-ray from both Moon and Sun. In the context of Moon, this technique has been employed since early days of space exploration to determine elemental composition of lunar surface. However, so far it has not been possible to exploit it to its full potential due to various reasons. Therefore it is planned to continue the remote X-ray fluorescence spectroscopy experiment on-board Chandrayaan-2 which includes both lunar X-ray observations and solar X-ray observations as two separate payloads. The lunar X-ray observations will be carried out by Chandra Large Area Soft x-ray Spectrometer (CLASS) experiment; whereas the solar X-ray observations will be carried out by a separate payload, Solar X-ray Monitor (XSM). Here we present the overall design of the XSM instrument, the present development status as well as preliminary results of the laboratory model testing. XSM instrument will have two packages namely – XSM sensor package and XSM electronics package. XSM will accurately measure spectrum of Solar X-rays in the energy range of 1–15 keV with energy resolution ∼200 eV @ 5.9 keV. This will be achieved by using state-of-the-art Silicon Drift Detector (SDD), which has a unique capability of maintaining high energy resolution at very high incident count rate expected from Solar X-rays. XSM onboard Chandrayaan-2 will be the first experiment to use such detector for Solar X-ray monitoring.