陶瓷基分子吸附器的航天器污染控制性能试验研究

为验证陶瓷基分子吸附器利用多孔材料的吸附性能降低航天器一定区域内污染水平的能力,试验研究真空环境中13X分子筛材料的分子污染物吸/脱附特性,以及以13X分子筛为吸附剂的陶瓷基分子吸附器对航天器用电缆放气产物的吸附性能。试验结果表明:13X分子筛可以有效捕获污染物分子,陶瓷基分子吸附器的吸附能力在3.1×10-2～3.4×10-2 g/cm2之间。陶瓷基分子吸附器可以应用于航天器热真空试验和在轨运行时的污染控制,有利于延长航天器寿命、提高航天器可靠性。     

AZO改性Y2O3-ZnO-Al2O3热控涂层性能分析

为解决铝合金表面液相等离子体电解氧化（PEO）涂层（Y₂O₃-ZnO-Al₂O₃）导电性差而导致的静电效应,对其进行表面改性处理。采用原子层沉积（ALD）技术在铝合金表面PEO涂层原位沉积铝掺杂氧化锌（AZO）导电薄膜以提高PEO涂层的导电性。对AZO改性PEO涂层的相组成和表面微观结构进行分析;对不同沉积温度下所得复合涂层的电阻率、载流子浓度和迁移率,以及沉积前后的热控性能、耐腐蚀性进行测量分析。结果表明:AZO导电薄膜均质连续致密地沉积在PEO涂层表面;当沉积温度为150 ℃时,AZO@Y₂O₃-ZnO-Al₂O₃复合涂层的电阻率为1.15×10-4 Ω·cm,载流子浓度为1.8×1020 cm-3,太阳吸收比为0.409,发射率为0.892,且抗电化学腐蚀性能良好,能够满足航天器热控涂层在空间环境应用的技术要求。     

航天器密封管路的气态工质与示漏气体 漏率等效关系研究

利用多种气体分析仪,采取四级质谱定量分析技术,分别测定He、N₂、N_e、CF₄、Kr等气体在不同入口压力下通过不同的人造漏孔的漏率;经过对同工况下气体间漏率比对,研究气体间漏率等效关系。试验结果表明:气体在不同工况下处于不同的流动领域,且其漏率与入口压力存在着不同的数值关系,经分析试验结果得出适用于气体全流域的漏率经验公式;气体间漏率的等效关系在低漏率及高漏率端始终呈平滑的线性关系,而在中间的过渡区域呈四或五次多项式关系;但是CF₄与H_e的漏率等效性呈线性关系,显示出多原子分子与单、双原子分子在粒子输运过程中存在着差异。试验结果为示漏工质漏率指标的制定提供了基础数据。     

C/C-TaC复合材料制备技术研究

难熔金属碳化物的加入可有效提高C/C材料的抗烧蚀性能,并成为近年来国内外研究的热点。文章主要介绍了中南大学在难熔金属碳化物TaC改性C/C材料制备技术方面的研究工作,主要包括含有Ta₂O₅的树脂/沥青浸渍-高温处理原位反应生成TaC的工艺方法、用含有有机Ta的树脂浸渍-高温处理原位反应生成TaC的工艺方法、预制体编织过程中加入TaC制备C/C-TaC的工艺方法、基于化学气相渗透法制备TaC及SiC/TaC中间界面层改性C/C材料的工艺技术以及基于化学气相沉积法制备抗烧蚀TaC及SiC/TaC难熔金属碳化物涂层的工艺技术。     

空间流量调节阀的润滑

流量调节阀运动件较多,工作环境压力<10^-11Pa,流体润滑不适应该环境条件。阀芯与推进剂（N₂O₄和MON-1）接触,无成熟解决方案。本文提出的阀门运动件润滑方案,非接触介质运动件采用自润滑材料或固体润滑膜。阀芯润滑,提出了物理气象沉积类金刚石膜（DLC）、TiN-Au复合膜及单质纯金膜三种方案。通过试验研究,确定阀芯采用全新的润滑方式-离子镀金。     

TiO2光催化薄膜在空间污染防护 应用中的探索

文章采用溶胶凝胶法在JGS1石英玻璃上制备了TiO₂薄膜,并对其晶体结构与光催化性能之间的关系进行了研究,探讨了紫外光辐照下TiO₂薄膜对大分子链硅油光催化效果。结果表明:经500 ℃热处理后的TiO₂薄膜为锐钛矿结构,具有较高的光催化活性;在253 nm紫外光辐照下,TiO₂薄膜对大分子链硅油表现出较好的光催化降解效果。该研究将为空间环境下飞行器光学表面污染净化材料的开发提供有益参考。     

一种大型固体火箭发动机界面脱粘缺陷的无损检测方法

针对列装部队服役产品现场开展固体火箭发动机燃烧室界面粘接质量无损检测的需求,研制了一种针对大型固体火箭发动机燃烧室推进剂/衬层/绝热层界面脱粘缺陷的无损检测系统。该系统基于机电阻抗频率响应函数方法,由多通道高速数据采集设备、压电主被动传感晶片、激励装置和软件评估系统组成,利用激励装置敲击固体发动机壳体待测结构表面,通过Lab VIEW数据采集程序测得响应信号,根据机电阻抗频响波形特征及波峰数量判断界面脱粘缺陷。当燃烧室绝热层/衬层/推进剂界面结构完好时,频响函数曲线仅有一个明显平滑的主波峰,当燃烧室绝热层/衬层/推进剂界面出现脱粘缺陷时,频响函数曲线的波峰数量增加,呈现明显的锯齿波形状。该方法便捷高效,非常适用于大型固体火箭发动机总装后整体产品燃烧室界面粘接质量的快速野外排查,也可进行长期的燃烧室界面状态健康监测。     

二茂铁功能化SBA-15的制备及其对AP／HTPB固体复合推进剂燃烧催化作用研究

二茂铁(Fc)及其衍生物是AP/HTPB固体复合推进剂的有效燃速催化剂,但在推进剂中的迁移始终是其应用的最大障碍。将二茂铁通过缩合反应接枝到介孔材料SBA-15的表面,制备了一种低迁移催化剂Fc-SBA-15。X射线衍射和N2吸附-脱附实验表明,Fc均匀致密地固定在了SBA-15的内外表面,Fc的负载没有对SBA-15的介孔结构造成破坏。改进的迁移性实验表明,制备的Fc-SBA-15复合材料是一种低迁移的催化剂。Fc-SBA-15对AP的热分解与AP/HTPB推进剂的燃烧具有较好的催化效果,添加2%的Fc-SBA-15使AP的高温热分解峰温度降低64℃,使AP/HTPB固体复合推进剂的燃速提高43%,压强指数下降30%。     

填料对推进剂用RTV-2硅橡胶包覆材料性能的影响

研究了气相法白炭黑、中空玻璃微球、绢云母等几类填料对包覆层用RTV-2硅橡胶力学性能、工艺性能及烧蚀性能的影响。结果表明,气相法白炭黑的补强效果最佳,绢云母和中空玻璃微球类填料对拉伸强度虽然有3~4倍的提高,但仍达不到白炭黑的补强效果,不能满足包覆层需求。胶料粘度随着填料加入量增大而升高,由于对粘度有严重影响,白炭黑必须进行表面处理后才能使用,而其余几类填料的影响则不是很大,可直接添加。这些填料都能在一定程度上提高材料耐烧蚀性,且差别不大。制备的RTV-2硅橡胶包覆层材料的质量烧蚀率和线性烧蚀率均小于0.050 g/s和0.050 mm/s,相对于某丁羟包覆层,分别减小了60%和80%以上,满足了某固体推进剂包覆层的技术要求。     

二氧化氮催化硝化甘油分解机理的数值计算

采用密度泛函理论（DFT）在B3LYP/6-31+G（d,p）水平上模拟计算了NO₂对硝化甘油（NG）催化分解的反应机理。通过与O—NO₂均裂、HNO₂分子内消去反应对比发现,NO₂分子对NG分解反应有显著的催化效应;NG的催化分解途径有α-H夺氢催化和β-H夺氢催化,计算得出2种途径的反应能垒分别为105.337 k J/mol和124.381 k J/mol,说明α-H夺氢催化更容易发生。     

燃烧室内燃烧模型对尾焰流场及其辐射的影响

基于压力隐式算子分裂(PISO)算法,通过求解Navier-Stokes方程,对燃烧室内一步反应和两步反应模型、无燃烧室三种情形下尾焰流场进行了数值仿真;采用结构和非结构网格并分别用TTM方法和Delaunay三角形方法来生成;利用高温气体高分辨率光谱参数数据库HITEMP对辐射传输方程进行求解,得到三种情形下尾焰中CO2和H2O的光谱辐射亮度分布。仿真结果表明:不同的燃烧模型影响尾焰流场及其辐射,无燃烧室时尾焰辐射较弱。     

Physical-chemical treatment of wastes: a way to close turnover of elements in LSS.

"Man-plants-physical-chemical unit" system designed for space stations or terrestrial ecohabitats to close steady-state mineral, water and gas exchange is proposed. The physical-chemical unit is to mineralize all inedible plant wastes and physiological human wastes (feces, urine, gray water) by electromagnetically activated hydrogen peroxide in an oxidation reactor. The final product is a mineralized solution containing all elements balanced for plants' requirements. The solution has been successfully used in experiments to grow wheat, beans and radish. The solution was reusable: the evaporated moisture was replenished by the phytotron condensate. Sodium salination of plants was precluded by evaporating reactor-mineralized urine to sodium saturation concentration to crystallize out NaCl which can be used as food for the crew. The remaining mineralized product was brought back for nutrition of plants. The gas composition of the reactor comprises O2, N2, CO2, NH3, H2. At the reactor's output hydrogen and oxygen were catalyzed into water, NH3 was converted in a water trap into NH4 and used for nutrition of plants. A special accessory at the reactor's output may produce hydrogen peroxide from intrasystem water and gas which makes possible to close gas loops between LSS components.     

氧化亚氮双组元发动机热力性能计算分析

对绿色推进剂N2O,H2,CH3OH,C2H5OH,CH4,C2H6,C2H4,C2H2,C3H8及C3H6的物性进行了全面比较,并采用吉布斯最小自由能法对9种氧化亚氮双组元推进剂组合的热力性能展开全面计算及分析。N2O/H2组合由于其最低的燃气平均摩尔质量而具有最高的比冲;N2O/C2H2组合由于C2H2很高的标准生成焓其燃烧温度可高达3823 K;碳氢燃料在余氧系数α<0.4富燃工况下燃气中含有固碳颗粒,且摩尔含量随着α的降低而急剧升高,喷管出口处可高达35%～40%;N2O/C3H8和N2O/C3H6组合拥有很好的空间应用物性和较高的热力性能,在压比pc:pe=70 atm:1 atm工况下平衡流比冲分别为2 639 m/s和2 656 m/s,具有很好的应用前景。     

LIFE: Life Investigation For Enceladus A Sample Return Mission Concept in Search for Evidence of Life

Abstract Life Investigation For Enceladus (LIFE) presents a low-cost sample return mission to Enceladus, a body with high astrobiological potential. There is ample evidence that liquid water exists under ice coverage in the form of active geysers in the "tiger stripes" area of the southern Enceladus hemisphere. This active plume consists of gas and ice particles and enables the sampling of fresh materials from the interior that may originate from a liquid water source. The particles consist mostly of water ice and are 1-10?μ in diameter. The plume composition shows H(2)O, CO(2), CH(4), NH(3), Ar, and evidence that more complex organic species might be present. Since life on Earth exists whenever liquid water, organics, and energy coexist, understanding the chemical components of the emanating ice particles could indicate whether life is potentially present on Enceladus. The icy worlds of the outer planets are testing grounds for some of the theories for the origin of life on Earth. The LIFE mission concept is envisioned in two parts: first, to orbit Saturn (in order to achieve lower sampling speeds, approaching 2 km/s, and thus enable a softer sample collection impact than Stardust, and to make possible multiple flybys of Enceladus); second, to sample Enceladus' plume, the E ring of Saturn, and the Titan upper atmosphere. With new findings from these samples, NASA could provide detailed chemical and isotopic and, potentially, biological compositional context of the plume. Since the duration of the Enceladus plume is unpredictable, it is imperative that these samples are captured at the earliest flight opportunity. If LIFE is launched before 2019, it could take advantage of a Jupiter gravity assist, which would thus reduce mission lifetimes and launch vehicle costs. The LIFE concept offers science returns comparable to those of a Flagship mission but at the measurably lower sample return costs of a Discovery-class mission. Key Words: Astrobiology-Habitability-Enceladus-Biosignatures. Astrobiology 12, 730-742.     

Simulation of rocket plume and lunar dust using DSMC method

When lunar modules land on the Moon, dust impingement on the lunar module components and deposition on the thermal and optical surfaces would cause many serious problems. The emphasis of this research is on simulating the interaction of rocket plume and lunar dust using the direct simulation Monte Carlo (DSMC) method. The method is extended to model the movement and collision stages of rarefied plume gas and dust particles, including three collisional mechanisms: molecule–molecule, molecule–particle and particle–particle collisions. The reflection of gas molecules on the particle surface is computed by an indirect approach based on the coordinate transformation. Neighboring-cell contact detection scheme is applied to check for contacts between all possible particle pairs. The simulation results show that the acceleration of dust particle is mostly determined by the parameters of plume field. In the computational regions with larger gas density and velocity the particles can be accelerated to larger velocity and convected to higher temperature.     

The catalytic potential of cosmic dust: implications for prebiotic chemistry in the solar nebula and other protoplanetary systems

The synthesis of important prebiotic molecules is fundamentally reliant on basic starting ingredients: water, organic species [e.g., methane (CH(4))], and reduced nitrogen compounds [e.g., ammonia (NH(3)), methyl cyanide (CH(3)CN) etc.]. However, modern studies conclude that the primordial Earth's atmosphere was too rich in CO, CO(2), and water to permit efficient synthesis of such reduced molecules as envisioned by the classic Miller-Urey experiment. Other proposed sources of terrestrial nitrogen reduction, like those within submarine vent systems, also seem to be inadequate sources of chemically reduced C-H-O-N compounds. Here, we demonstrate that nebular dust analogs have impressive catalytic properties for synthesizing prebiotic molecules. Using a catalyst analogous to nebular iron silicate condensate, at temperatures ranging from 500K to 900K, we catalyzed both the Fischer-Tropsch conversion of CO and H(2) to methane and water, and the corresponding Haber-Bosch synthesis of ammonia from N(2) and H(2). Remarkably, when CO, N(2), and H(2) were allowed to react simultaneously, these syntheses also yielded nitrogen-containing organics such as methyl amine (CH(3)NH(2)), acetonitrile (CH(3)CN), and N-methyl methylene imine (H(3)CNCH(2)). A fundamental consequence of this work for astrobiology is the potential for a natural chemical pathway to produce complex chemical building blocks of life throughout our own Solar System and beyond.     

稀释气体流量对低压化学气相沉积硼掺碳涂层的影响

以BCl3-C3H6-H2为气相反应体系,采用低压化学气相沉积制备硼掺碳涂层.研究了Ar气稀释流量对硼掺碳涂层沉积速度、形貌、组成和键合状态的影响.结果表明,不同稀释气体流量作用下,硼掺碳的沉积速度没有明显变化,产物形貌由致密向层状转变,硼元素含量稍有减少而碳元素含量稍有增加.沉积产物中B元素的键合方式以B-sub-C和BC2O为主.结合化学反应和气体扩散,探讨了稀释气体的作用机制,表明PyC形成反应的主导作用导致稀释气体流量对沉积速度作用不明显,而BCl3和C3H6在Ar气中扩散系数的差异导致产物形貌和组成发生变化.     

兰姆波频散方程的分析及数值迭代算法

根据兰姆波运动规律的时间简谐波因子与频散曲线的物理特性,用数值迭代法在实数域内求解频散方程.给出了铝板中兰姆波相速度和群速度的解.研究表明:该法可较易获得频散曲线,无需方程分段求解,具一定的参考价值.     

Detectability of planetary characteristics in disk-averaged spectra. I: The Earth model

Over the next 2 decades, NASA and ESA are planning a series of space-based observatories to detect and characterize extrasolar planets. This first generation of observatories will not be able to spatially resolve the terrestrial planets detected. Instead, these planets will be characterized by disk-averaged spectroscopy. To assess the detectability of planetary characteristics in disk-averaged spectra, we have developed a spatially and spectrally resolved model of the Earth. This model uses atmospheric and surface properties from existing observations and modeling studies as input, and generates spatially resolved high-resolution synthetic spectra using the Spectral Mapping Atmospheric Radiative Transfer model. Synthetic spectra were generated for a variety of conditions, including cloud coverage, illumination fraction, and viewing angle geometry, over a wavelength range extending from the ultraviolet to the farinfrared. Here we describe the model and validate it against disk-averaged visible to infrared observations of the Earth taken by the Mars Global Surveyor Thermal Emission Spectrometer, the ESA Mars Express Omega instrument, and ground-based observations of earthshine reflected from the unilluminated portion of the Moon. The comparison between the data and model indicates that several atmospheric species can be identified in disk-averaged Earth spectra, and potentially detected depending on the wavelength range and resolving power of the instrument. At visible wavelengths (0.4-0.9 microm) O3, H2O, O2, and oxygen dimer [(O2)2] are clearly apparent. In the mid-infrared (5-20 microm) CO2, O3, and H2O are present. CH4, N2O, CO2, O3, and H2O are visible in the near-infrared (1-5 microm). A comprehensive three-dimensional model of the Earth is needed to produce a good fit with the observations.     

固体火箭发动机尾焰流场特性研究

针对某固体火箭发动机,对二维轴对称尾焰流场进行数值模拟,并考虑复燃化学反应和Al2O3颗粒运动的影响。计算得到了尾焰射流的温度场和组分分布图,将计算结果和地面实验结果进行对比,对尾焰流场主要特点进行分析。结果表明复燃化学反应主要发生在燃气空气混合区域,化学反应使复燃区域温度升高约250 K。该计算方法能反映出尾焰复燃流场的主要特点,可为固体火箭发动机尾焰红外特性的计算提供流场基本数据。