CCD温度对星敏感器星点定位精度的影响

CCD噪声是影响星敏感器星点定位精度的误差源之一,以DV437-BU2型CCD为例,对CCD的暗电流、暗电流散粒噪声、暗电流不均匀噪声等的温度特性进行了实验测量．研究了CCD温度对星敏感器星点定位精度的影响,结果表明：对于DV437-BU2型CCD芯片,当CCD工作温度高于300K时,降温可以显著提高星敏感器星点定位精度,当CCD工作温度低于300K时,降温对星点定位精度的影响不明显;当温度由330K降到300K时,星点定位精度由0．12个像素提高至0．078个像素．     

内冷却紧凑式固体除湿器实验研究

在叉流板翅式换热器结构基础上,研发制作了一种粘贴型内冷却紧凑式固体除湿器,并对这种新型除湿器的性能进行实验研究.除湿器使用硅胶作为吸湿剂,通过导热胶将硅胶颗粒粘贴在除湿器主边的气流通道壁面上.实验分为4组,分别在高湿度和低湿度环境工况下,测试本文研制的除湿器在有内冷却和无内冷却条件下的除湿运行效果以检验内冷却气流对除湿器性能的影响.实验表明,内冷却紧凑式固体除湿器工作性能优良,在除湿器有内冷却的条件下,工作周期内除湿器的平均除湿量显著提高.在高湿度条件下,硅胶在20min内的动态吸湿率可达12.4%,高于目前已知的常压下硅胶对水蒸汽的动态吸湿率.      

环路热管稳态建模及运行特性分析

建立了环路热管的稳态模型,并基于能量平衡、压力平衡、质量守恒以及几何约束进行求解,证实了许多相关文献介绍的环路热管稳态运行特性,例如,热沉温度、环境温度等对稳态蒸发温度的影响.对下述问题提出见解:蒸发器的漏热的分析;可变热导区和固定热导区的成因;固定热导区热导的变化;工质充装量和储液器容积的确定方法.结果表明,用来加热通过毛细芯的流体的蒸发器漏热分量在热载荷较大时不可忽略;反重力高度和环境对回流液体的加热是可变热导区的成因;大热载荷下,固定热导区热导随热载荷增大而减小,并可能达到临界热载荷,其解决方案在于工质充装量和储液器容积的匹配.      

循环湿热环境下碳纤维复合材料的界面性能

针对CCF300/5428复合材料在循环湿热环境下的吸湿-脱湿行为和层间剪切性能进行了研究,并结合扫描电镜观察了循环湿热处理的不同阶段纤维/基体界面结合状态.研究结果表明:经过反复吸湿后,水分的初始扩散速率和饱和吸湿率增加;脱湿后水对复合材料层间剪切性能的影响大部分可以消除;复合材料吸湿后室温环境下性能下降较少,但在高温高湿环境下,复合材料的性能会显著降低.     

开式固体除湿空调关键部件及系统分析

开式固体除湿空调系统是一种节能、无污染的新型空调系数，本文研究了开式固体除湿空调系统的关键部件－转轮式固体除湿器，给出了此类除湿器的一种数学模型。在此基础上，针对几种不同流程的系统型式，就除湿器效率对各系统性能的影响进行了研究。     

真空与磁场热处理改善FeCo合金的软磁性能

针对发电机中转子用FeCo合金(国产牌号1J22)进行了组织结构与磁性能的研究.通过对该合金进行真空处理以及磁场热处理,研究了组织结构对软磁性能的影响规律;研究了附加磁场强度以及热处理温度对磁场处理效果的影响,并结合该合金的磁致伸缩伸缩系数的变化规律,分析了磁场热处理效果的微观机制.当合金组织为轧制态时,磁场热处理效果不明显;在合金的再结晶温度以上进行磁场热处理时,获得了显著的磁场热处理效果,矫顽力下降至72A/m(0~9Oe)以下.     

双储液器环路热管的设计与实验研究

设计了一套双储液器环路热管以解决其重力场中运行受方位限制的问题,介绍了通过储液器体积和工质充装量的匹配设计避免最难启动情形发生的方法,并进行了相关的实验研究。实验验证了双储液器环路热管重力场中运行不受方位限制的特性,并且发现,在可变热导区的一定的热载荷范围内,双储液器环路热管在不同姿态下稳态运行温度不相同,而其他热载荷区域内却基本一致。文章分别从储液器能量平衡和回流液体过冷量有效利用率的角度进行了分析和解释。     

史密森天文物理观测台研制的冷氢激射器及有关装置

低温冷却激射器为测量频率偏移和存储壁涂敷材料的弛豫特性创造了有利条件。这种涂敷材料是从常态变为气态物质而被冻结在存储壁上的。我们对FEP—120聚四氟乙烯在77K至48K之间的原始测试结果作了报道,并把这些测量结果和法国de Saintfuscien在372K至77K之间的测试数据进行了比较。对激射器的某些设计性能作了说明。低溫激射器的氢分离器,完全密封在真空环境中,其温度77k。本文还介绍了在真空中工作的分离器和其它一些装置。这些装置已在常温激射器中被采用并进行了测试。它们既适合于太空环境又适合于在地面使用。     

基于氧气A波段临近空间大气温度反演的贝叶斯与最小二乘法对比

基于氧气A波段的临边辐射模拟数据进行临近空间大气温度廓线的反演，分析比较了贝叶斯和最小二乘两种不同反演算法的特点.80km以下，信噪比为66～337时:基于贝叶斯理论反演的三条谱线761.59，762.2，764.05nm的反演误差平均值分别为5.52，3.94，4.73K；采用最小二乘法的反演误差平均值分别为10.57，7.04，8.80K.信噪比为6～34时:基于贝叶斯理论反演的三条谱线的反演误差平均值分别为18.27，12.18，18.27K；采用最小二乘法的反演误差平均值分别为103.18，68.79，85.98K.研究结果表明，基于贝叶斯理论的反演方法，利用先验信息对反演结果进行约束和修正，在有噪声的情况下获得了更合理的解，从而提高了反演精度和抗干扰能力.这为星载探测临近空间大气温度的算法研究和开发提供了参考，也为提高光谱仪器信噪比并进而提高温度反演精度提供了理论基础.      

减压直流等离子体射流电子温度的双静电探针测量

建立了一套双静电探针诊断系统,用于检测在气流量为4．2slm、弧电流为80A、真空室压力为165Pa的条件下纯氩直流非转移弧等离子体射流的电子温度及其分布。结果表明：发生器出口处射流中心的电子温度约为14500K,射流中电子温度随离开发生器出口的轴向或径向距离的增加而单调降低;径向电子温度梯度约为263K／mm,轴向电子温度梯度为69K／mm;射流中电子温度随弧电流增加而单调上升。     

The search for nitrogen compounds on the surface of Mars

Nitrogen is an essential element for life. Specifically, “fixed nitrogen” (i.e., NH₃, NH₄⁺, NO_x, or N that is chemically bound to either inorganic or organic molecules and is releasable by hydrolysis to NH₃ or NH₄⁺) is the form of nitrogen useful to living organisms. To date no direct analysis of Martian soil nitrogen content, or content of fixed nitrogen compounds has been done. Consequently, the planet's total inventory of nitrogen is unknown. What is known is that the N₂ content of the present-day Martian atmosphere is 0.2 mbar. It has been hypothesized that early in Mars' history (3 to 4 billion years ago) the Martian atmosphere contained much more N₂ than it does today. The values of N₂ proposed for this early Martian atmosphere, however, are not well constrained and range from 3 to 300 mbar of N₂. If the early atmosphere of Mars did contain much more N₂ than it does today the question to be answered is, Where did it go? The two main processes that could have removed it rapidly from the atmosphere include: 1) nonthermal escape of N-atoms to space; and 2) burial within the regolith as nitrates and nitrites. Nitrate will be stable in the highly oxidized surface soil of Mars, and will tend to accumulate in the soil. Such accumulations are observed in certain desert environments on Earth. Some NH₄⁺---N may also be fixed and stabilized in the soil by inclusion as a structural cation in the crystal lattices of certain phyllosilicates replacing K. Analysis of the Martian soil for traces of NO₃⁻ and NH₄⁺ during future missions will supply important information regarding the nitrogen abundance on Mars, its past climate as well as its potential for the evolution of life.     

多舱段载人航天器CO2去除系统性能仿真分析

多舱段载人航天器通常由主控舱段利用舱间通风对组合体空气环境参数进行集中控制.利用Ecosimpro建立了一种多舱段载人航天器CO₂去除系统性能仿真分析模型,包括舱体模块、乘员模块、CO₂净化模块、舱间通风模块,并对三舱段载人航天器CO₂去除系统性能进行了计算分析.结果表明,当净化装置进风量为0.007 2 kg/s,非主控舱段驻留人数达到6人时,会造成非主控舱段CO₂分压超出700 Pa的指标上限.此时增大舱间通风量对降低非主控舱段CO₂分压的效果并不明显,有效的控制方式是增大净化装置进风量.当净化装置进风量增加至0.011 3 kg/s时,非主控舱段CO₂分压可降至700 Pa以下.该工作有助于加快载人航天器空气环境控制系统的设计和改进流程.     

混合球磨对YAl_2颗粒形貌及表面改性的影响

采用扫描电镜、能谱分析、透射电镜等分析方法研究了球磨对YAl₂及YAl₂/Mg颗粒的组织形貌、YAl₂颗粒在YAl₂/Mg颗粒中的分散性及YAl₂/Mg界面结合状况的影响.结果表明:YAl₂颗粒经球磨20 h后,其平均粒径约为1.5 μm,颗粒边缘尖角数量明显减少,呈圆滑的近球形.加入Mg颗粒进行混合球磨20 h后,YAl₂颗粒在混合颗粒中呈弥散分布,且表面包裹一层单质Mg,YAl₂/Mg的界面为直接结合型,未发现有界面反应.     

Hot atoms in cosmic chemistry

High energy chemical reactions and atom molecule interactions might be important for cosmic chemistry with respect to the accelerated species in solar wind, cosmic rays, colliding gas and dust clouds and secondary knock-on particles in solids. “Hot” atoms with energies ranging from a few eV to some MeV can be generated via nuclear reactions and consequent recoil processes. The chemical fate of the radioactive atoms can be followed by radiochemical methods (radio GC or HPLC). Hot atom chemistry may serve for laboratory simulation of the reactions of energetic species with gaseous or solid interstellar matter. Due to the effective measurement of 10⁸–10¹⁰ atoms only it covers a low to medium dose regime and may add to the studies of ion implantation which due to the optical methods applied are necessarily in the high dose regime.

Experimental results are given for the systems: C/H₂O (gas), C/H₂O (solid, 77 K), N/CH₄ (solid, 77K) and C/NH₃ (solid, 77 K). Nuclear reactions used for the generation of 2 to 3 MeV atoms are: ¹⁴N(p, ) ¹¹C, ¹⁶O(p, pn) ¹¹C and ¹²C(d,n) ¹³N with 8 to 45 MeV protons or deuterons from a cyclotron. Typical reactions products are: CO, CO₂, CH₄, CH₂O, CH₃OH, HCOOH, NH₃, CH₃NH₂, cyanamide, formamidine, guanidine etc. Products of hot reactions in solids are more complex than in corresponding gaseous systems, which underlines the importance of solid state reactions for the build-up of precursors for biomolecules in space. As one of the major mechanisms for product formation, the simultaneous or fast consecutive reactions of a hot carbon with two target molecules (reaction complex) is discussed.     

Photochemistry of planetary ionospheres

The basic photochemical processes in the upper atmospheres and ionospheres of the various bodies in our solar system (planets, moons and comets) are similar. However, there are many different factors (e.g. gas composition, energy input, gravity) which control/change the relative importance of these controlling processes. The photo-chemistry of the inner planets is reasonably well understood at this time, thus there is good agreement between model calculations and most of the observational data base. The extremely limited information that we have available on the ionospheres of the outer planets leads to significant uncertainties about some of the controlling processes. Some important questions (e.g. Is the charge exchange process H⁺ + H₂(v≥4) → H₂⁺ + H important? Is water vapor influx from the rings important?) remain unanswered at this time. In cometary atmospheres the freshly evaporated parent molecules are rapidly photodissociated and photoionized, therefore most of the chemical kinetics of cometary ionospheres involve these rapidly moving and highly reactive ions and radicals.     

Si对TiAl合金高温抗氧化性能的影响

利用X射线衍射、扫描电镜、能谱仪等手段研究了TiAl-Si(原子数分数为0~20%)合金在1 173 K大气中24 h的恒温氧化.结果表明:Si元素可以有效地提高TiAl合金的高温抗氧化性能;随着Si含量的增加,氧化膜厚度依次减薄,TiO₂的含量逐渐减少,Al₂O3的含量逐渐增加,添加到10%左右时就有连续致密的Al₂O₃保护膜形成;Si在0~20%的添加过程中并没发现Si的氧化物生成.分析表明:Si对抗氧化性能的贡献可归结于Si与Ti有很好的亲和力,可以有效地降低Ti离子的活度、阻碍Ti离子的向外扩散, 相对来说增强了Al离子的活度,促进连续致密的Al₂O₃保护膜生成.      

On the possible detection of solid O2 and O3 interstellar grains with ISO

In various models of interstellar grain chemistry, solid O₂ is formed by accretion as well as by surface reactions on grains. In dense molecular cloud models, at a later stage of the evolution, the O₂ molecule may become a substantial grain mantle constituent. Since IR dipole vibrational transitions for the homonuclear diatomic molecule O₂ are forbidden, the abundance of this potentially important grain mantle component can not be determined. However, embedded in a dirty ice matrix, the fundamental vibration of O₂ at 1550 cm⁻¹ becomes observable at 10 K, due to interactions with surrounding molecules, which break the symmetry of molecular oxygen. This process might be applicable for the dust mantle environment of interstellar grains. We have studied the role of solid O₂ and O₃ in astrophysically relevant ice mixtures and discuss the possible detection of solid O₂ and its major photolysis product O₃ in interstellar grains, in dense molecular clouds. Both molecules represent a specific target to be observed by the ISO satellite in the near future.     

进气道结构对固体冲压发动机补燃室燃烧及内壁流场的影响

为研究进气道结构对固体冲压发动机补燃室燃烧及内壁烧蚀的影响,采用标准k-ε湍流模型,单步涡耗散燃烧模型与KING硼粒子点火燃烧模型,开展了双下侧90°进气结构和双侧180°进气结构固体冲压发动机补燃室内燃气燃烧数值模拟,对比分析了补燃室燃气燃烧流场特征和内壁烧蚀环境特征。结果表明:双侧180°进气结构在补燃室中形成大漩涡,有利于燃气与空气的掺混燃烧,至补燃室出口位置,总燃烧效率超过90%,且该结构有效减少了粒子对内壁的冲刷侵蚀;在双下侧90°进气结构补燃室中,凝聚相粒子和燃气贴近补燃室一侧运动,导致氧气浓度和温度分布不均,不利于燃气的掺混燃烧,总燃烧效率为74%,在远离补燃室进气道一侧形成高温热烧蚀、高浓度粒子侵蚀、高速射流冲刷和热应力集中的综合破坏;双侧180°进气结构的固体冲压发动机补燃室总体性能优于双下侧90°进气结构的冲压发动机补燃室。      

S3 and S4 absorption cross sections in the range of 340 to 600 nm and evaluation of the S3 abundance in the lower atmosphere of Venus

S₃ absorption cross section equals 6×10⁻¹⁷ cm² at 400 nm, 6 × 10⁻¹⁹ cm² at 500 nm (less by a factor of 4 than that given by Sanko), 4×10⁻²⁰ cm² at 600 nm. That of S₄ equals 1.5 × 10⁻¹⁷ cm² at 450 nm, 8 × 10⁻¹⁷ cm² at 500 nm, and 4.7 × 10⁻¹⁷ cm² at 600 nm. Preliminary evaluation of the S₃ mixing ratio in the lower atmosphere of Venus is (8±3)×10⁻¹¹ at 5 to 25km according to the Venera 14 measurements and several times lower at the locations of the Veneras-11 and -13.