高精度SINS/CCD/GPS组合导航系统研究与仿真

选取捷联惯导系统误差作为系统状态,利用捷联惯导系统(SINS)与电荷耦合器件(CCD)星敏感器各自的姿态矩阵输出构造量测,设计SINS/CCD组合导航算法;利用SINS与全球定位系统(GPS)各自的速度、位置输出构造量测,设计SINS/GPS组合导航算法。然后,利用联邦型卡尔曼滤波技术,将各子滤波器输出的系统状态局部最优估计值送入主滤波器,通过全局最优融合算法计算得到系统状态的全局最优估计值。仿真结果表明,基于SINS/CCD/GPS的组合导航系统具有很高的导航精度,达到了3.5m的定位精度和9″的航向精度,非常适用于飞行器的高精度导航定位。     

Φ5m立式风洞阻尼器的研制和应用

立式风洞开展自由失速/尾旋试验要求试验段气流速度具备快速调节能力,阻尼器是实现试验段气流速度快速调节能力的装置.叙述了阻尼器机械结构设计和它的功效,说明了控制系统设计及联调结果,介绍了试验段气流速度快速性调试方法及结论.系统应用表明,风洞试验段气流速度具备一定快速调节能力,具备开展自由失速/尾旋试验条件.     

耐高温复合材料的主动冷却实验和数值计算研究

高超声速吸气式发动机面临着严重的热防护问题,同时还存在着燃料和冷却剂不匹配的同题,必须使用耐高温材料与主动冷却相结合的冷却策略.针对一种使用陶瓷基耐高温复合材料的主动冷却模式开展了实验和数值研究,该多层材料主动冷却模式结合了主动冷却和耐高温复合材料的优点.基于这种主动冷却模式设计了一种多层材料组成主动冷却实验装置.利用燃气发生器提供的高热流环境对主动冷却实验装置开展了实验研究,并建立了一维非稳态复合结构的传热模型,模拟了不同材料组成的多层复合结构中的非稳态温度场.研究表明:基于C/SiC复合材料的多层材料主动冷却结构在高温高热流环境中的冷却能力较强,可以在使用较少冷却剂的条件下使发动机壳体内部的温度保持在可靠工作的范围内,说明使用基于耐高温复合材料的主动冷却模式是解决高超声速吸气式发动机热防护问题的新途径.     

C/C刹车材料用抗氧化涂层性能

研制了一种以磷酸、磷酸盐、硼化物等为原材料的磷酸盐涂料,在不同温度下烧结处理后,对其抗氧化性能及表面微观形貌进行研究.结果表明:650℃烧结的涂层氧化防护性能明显优于900℃烧结的;在700℃氧化30 h后,最小氧化失重率仅为1.76%,氧化后涂层仍然保持完整致密;经过900℃、3 min<=>室温、2min循环30次和l 100℃、3 min<=>室温、2 min循环10次的连续热震后,失重率为1.97%,涂层与C/C基体结合良好,涂层的热性能稳定.     

双出口气膜孔冷却效率数值模拟

为了优化气膜冷却结构,通过数值模拟研究了一种新型气膜孔(由两个圆柱孔组成的双出口孔)的气膜冷却特性.利用Fluent软件对Navier-Stokes方程进行求解,湍流模型采用两方程Realizablek-ε模型和增强壁面函数处理.圆柱孔射流的冷却效率计算结果和实验数据吻合较好.双出口孔射流冷却效率计算结果表明,双出口孔射流有效地增加了冷气的径向覆盖范围,在吹风比为0.5时,次孔射流起到了减弱主孔出口对旋涡的作用;在吹风比为1.0和2.0时,次孔射流使主孔出口处的对旋涡消失.最高冷却效率对应的吹风比为1.0.双出口孔射流在提高冷却效率的同时,其加工难度较扩张形孔明显降低.      

Implications of subzero metabolic activity on long-term microbial survival in terrestrial and extraterrestrial permafrost

The survival of microorganisms over extended time frames in frozen subsurface environments may be limited by chemical (i.e., via hydrolysis and oxidation) and ionizing radiation-induced damage to chromosomal DNA. In an effort to improve estimates for the survival of bacteria in icy terrestrial and extraterrestrial environments, we determined rates of macromolecular synthesis at temperatures down to -15°C in bacteria isolated from Siberian permafrost (Psychrobacter cryohalolentis K5 and P. arcticus 273-4) and the sensitivity of P. cryohalolentis to ionizing radiation. Based on experiments conducted over ≈400 days at -15°C, the rates of protein and DNA synthesis in P. cryohalolentis were <1 to 16 proteins cell(-1) d(-1) and 83 to 150 base pairs (bp) cell(-1) d(-1), respectively; P. arcticus synthesized DNA at rates of 20 to 1625?bp cell(-1) d(-1) at -15°C under the conditions tested. The dose of ionizing radiation at which 37% of the cells survive (D(37)) of frozen suspensions of P. cryohalolentis was 136?Gy, which was ～2-fold higher (71?Gy) than identical samples exposed as liquid suspensions. Laboratory measurements of [(3)H]thymidine incorporation demonstrate the physiological potential for DNA metabolism at -15°C and suggest a sufficient activity is possible to offset chromosomal damage incurred in near-subsurface terrestrial and martian permafrost. Thus, our data imply that the longevity of microorganisms actively metabolizing within permafrost environments is not constrained by chromosomal DNA damage resulting from ionizing radiation or entropic degradation over geological time.     

Martian CH(4): sources, flux, and detection

Recent observations have detected trace amounts of CH(4) heterogeneously distributed in the martian atmosphere, which indicated a subsurface CH(4) flux of ~2 x 10(5) to 2 x 10(9) cm(2) s(1). Four different origins for this CH(4) were considered: (1) volcanogenic; (2) sublimation of hydrate- rich ice; (3) diffusive transport through hydrate-saturated cryosphere; and (4) microbial CH(4) generation above the cryosphere. A diffusive flux model of the martian crust for He, H(2), and CH(4) was developed based upon measurements of deep fracture water samples from South Africa. This model distinguishes between abiogenic and microbial CH(4) sources based upon their isotopic composition, and couples microbial CH(4) production to H(2) generation by H(2)O radiolysis. For a He flux of approximately 10(5) cm(2) s(1) this model yields an abiogenic CH(4) flux and a microbial CH(4) flux of approximately 10(6) and approximately 10(9) cm(2) s(1), respectively. This flux will only reach the martian surface if CH(4) hydrate is saturated in the cryosphere; otherwise it will be captured within the cryosphere. The sublimation of a hydrate-rich cryosphere could generate the observed CH(4) flux, whereas microbial CH(4) production in a hypersaline environment above the hydrate stability zone only seems capable of supplying approximately 10(5) cm(2) s(1) of CH(4). The model predicts that He/H(2)/CH(4)/C(2)H(6) abundances and the C and H isotopic values of CH(4) and the C isotopic composition of C(2)H(6) could reveal the different sources. Cavity ring-down spectrometers represent the instrument type that would be most capable of performing the C and H measurements of CH(4) on near future rover missions and pinpointing the cause and source of the CH(4) emissions.     

基于FBM分形向量特征的图象匹配

由于自然景物图象的灰度与边缘特征不稳定，基于灰度与边缘的匹配算法对于这一类图象难以生效。本文通过分析ＦｒａｃｔａｌＢｒｏｗｎｉａｎＭｏｔｉｏｎ（ＦＢＭ）的Ｗｅｉｅｒｓｔｒａｓｓ－Ｍａｎｄｅｌｂｒｏｔ随机分形逼近函数的频谱，给出了分形向量特征的定义和快速判别图象的ＦＢＭ区域的方法。在ＦＢＭ区域内采用该特征进行匹配能克服复杂自然景物图象中灰度与边缘特征的不稳定性。实验表明采用ＦＢＭ分形向量特征的匹配方法能够获得比较传统匹配方法，例如平均绝对差算法以及特征匹配法更高的匹配定位精度和匹配概率     

Key science questions from the second conference on early Mars: geologic, hydrologic, and climatic evolution and the implications for life

In October 2004, more than 130 terrestrial and planetary scientists met in Jackson Hole, WY, to discuss early Mars. The first billion years of martian geologic history is of particular interest because it is a period during which the planet was most active, after which a less dynamic period ensued that extends to the present day. The early activity left a fascinating geological record, which we are only beginning to unravel through direct observation and modeling. In considering this time period, questions outnumber answers, and one of the purposes of the meeting was to gather some of the best experts in the field to consider the current state of knowledge, ascertain which questions remain to be addressed, and identify the most promising approaches to addressing those questions. The purpose of this report is to document that discussion. Throughout the planet's first billion years, planetary-scale processes-including differentiation, hydrodynamic escape, volcanism, large impacts, erosion, and sedimentation-rapidly modified the atmosphere and crust. How did these processes operate, and what were their rates and interdependencies? The early environment was also characterized by both abundant liquid water and plentiful sources of energy, two of the most important conditions considered necessary for the origin of life. Where and when did the most habitable environments occur? Did life actually occupy them, and if so, has life persisted on Mars to the present? Our understanding of early Mars is critical to understanding how the planet we see today came to be.