环三磷腈基聚酰亚胺耐高温基体树脂合成与表征及热性能

以六(4-氨基苯氧基)环三磷腈为前驱体,与马来酸酐反应后经过热处理得到两类新型耐高温基体树脂环三磷腈基六取代和三取代聚酰亚胺。采用傅里叶转换红外光谱、核磁共振和元素分析等方法进行了结构表征。TGA与DTG测试表明,两类聚合物的初始分解温度分别为409.36℃和396.95℃,空气中850℃时残焦量高达65.23%和73.78%,表现出十分优良的耐热性能,适合作为火箭、导弹的耐高温复合材料。     

芳氧基聚磷腈绝热包覆材料的性能表征

针对固体火箭发动机对绝热包覆材料性能要求,制备了芳氧基聚磷腈绝热包覆材料。利用热导率测定仪、动态热机械仪、SEM以及国军标规定的测试方法对芳氧基聚磷腈的热导率、线膨胀系数、烧蚀后碳层结构、密度、线烧蚀率以及与推进剂的相容性等进行了表征。结果表明,芳氧基聚磷腈的热导率为0.187 W/(m·K)、线膨胀系数为2.31×10-4、密度为1.196 g/cm3、线烧蚀率为0.109 mm/s,而且烧蚀后成碳率高、碳层坚硬,同时该材料与推进剂具有良好的相容性。芳氧基聚磷腈优异的物理性能及抗烧蚀性能,证明其可作为火箭发动机绝热包覆材料,并显示出良好的应用前景。     

芳氧基聚磷腈绝热包覆材料的性能表征

针对固体火箭发动机对绝热包覆材料性能要求,制备了芳氧基聚磷腈绝热包覆材料。利用热导率测定仪、动态热机械仪、SEM及国军标规定的测试方法对芳氧基聚磷腈的热导率、线膨胀系数、烧蚀后碳层结构、密度、线烧蚀率及与推进剂的相容性等进行了表征。结果表明,芳氧基聚磷腈的热导率为0.187 W/(m·K)、线膨胀系数为2.31×10-4℃-1、密度为1.196 g/cm3、线烧蚀率为0.109 mm/s,而且烧蚀后成碳率高、碳层坚硬,同时该材料与推进剂具有良好的相容性。芳氧基聚磷腈优异的物理性能及抗烧蚀性能,证明其可作为火箭发动机绝热包覆材料并显示出良好的应用前景。     

C/C-ZrC-Cu复合材料的微观结构与抗烧蚀性能

采用低温反应熔渗工艺,以Zr_2Cu合金为熔渗金属,在密度为(1.25±0.05) g/cm~3的毡基C/C复合材料中引入ZrC+Cu组分,以提高其抗氧化烧蚀性能。采用X射线衍射仪(XRD)、光学显微镜(OM)和扫描电子显微镜(SEM),分析C/C-ZrC-Cu复合材料的相组成与微观结构,在氧-乙炔环境下考核材料的抗烧蚀性能。结果表明,C/C-ZrC-Cu复合材料形成了三维网络状(热解碳+ZrC+Cu)混合基体结构,热解碳可以有效防护高温金属熔体对碳纤维造成的损伤,Zr C和Cu的引入有效改善了抗烧蚀性能,氧乙炔烧蚀120 s后,线烧蚀率从毡基C/C复合材料的9.0×10~(-3)mm/s降低为-1.0×10~(-3)mm/s,主要归因于材料表面形成了相对完整的ZrO_2保护层和Cu的发汗冷却作用,对应的氧化烧蚀机制主要为Zr C、C等氧化引起的热氧化烧蚀和Cu熔化、挥发等引起的热物理烧蚀。     

高耐热型填料改性EPDM绝热层性能研究

以三元乙丙橡胶(EPDM)为基体,中空聚酰亚胺纤维为耐热型纤维,分别从低密度高成炭、高耐热以及分子链催化成炭三方面出发,通过机械共混法制备了酚醛空心微球(HPM)、聚酰亚胺树脂(PIR)以及含不饱和双键环磷腈衍生物(CPD)复合的EPDM绝热层,并对这三种绝热层进行了硫化性能、力学性能、与金属界面粘接性能以及耐烧蚀性能...     

氟代烷氧基聚磷腈弹性体的合成及性能研究

通过聚二氯磷腈(PDCP)与2,2,2-三氟乙醇钠、2,2,3,3,4,4,5,5-八氟戊醇钠(1∶1)和少量烯烃钠盐的亲核取代反应,制得可交联型的氟代烷氧基聚磷腈(e-PTOFP)。通过核磁共振(31P NMR,~1H NMR)测试,对其结构进行了表征。采用无转子硫化仪、氧指数实验(LOI)、垂直燃烧实验(UL-94)、烟密度测试仪和热失重(TGA)对氟代烷氧基聚磷腈弹性体的硫化性能、燃烧性能和热稳定性进行了分析。通过红外光谱(FTIR)对其热解残留物的结构进行了研究。结果表明,少量不饱和侧基的引入赋予了氟代烷氧基聚磷腈硫化性能,硫化后弹性体的氧指数为54.5,垂直燃烧等级为V-0,烟密度等级(SDR)为21.93,具有优异的阻燃性能、低烟性能和热稳性能,且其热降解的残留物主要是含P=O,N—H的磷氮化合物。可看出氟代烷氧基聚磷腈弹性体是潜在的综合性能优良的绝热层材料。     

耐烧蚀材料对无阻燃剂三元乙丙橡胶材料烧蚀性能的影响

为了提高固体火箭发动机绝热层材料耐烧蚀性能,采用三元乙丙橡胶、芳纶短纤纤维、硼酚醛树脂、过氧化二异丙苯为无阻燃剂绝热层材料的基本体系,研究了空心微珠、陶瓷微珠、玻璃鳞片、聚碳酸酯、苯并噁嗪树脂、甲基苯基硅树脂等耐烧蚀填料对三元乙丙橡胶烧蚀性能的影响。结果表明,无机填料(空心微珠、陶瓷微珠、玻璃鳞片各10份)、聚碳酸酯15份、苯并噁嗪树脂15份、甲基苯基硅树脂15份,线烧蚀率依次减少,分别为(0.203~0.222)mm/s、0.185mm/s、0.165mm/s、0.154mm/s,甲基苯基硅树脂是最理想的耐烧蚀填料,对无阻燃剂耐烧蚀三元乙丙橡胶研究具有一定的参考价值。     

航天飞行器防热涂层烧蚀行为及机理研究

为拓宽航天飞行器防热涂层裂解温域,提高涂层的耐烧蚀性能,文章通过热重–差示扫描量热分析仪(TG-DTG)分析了2种硅橡胶基体的热分解行为,并结合马弗炉烧蚀实验研究铁红、云母、白炭黑等3种功能组元对硅橡胶涂层静态烧蚀性能的影响,通过扫描电镜(SEM)以及红外光谱分析仪(FT-IR)分析烧蚀机理,最后通过马弗炉烧蚀实验及高温燃气流烧蚀实验对2种涂层的烧蚀性能进行考核。结果表明:甲基苯基硅橡胶在220～320℃温域的裂解主要以侧基交联为主;在320～480℃以由羟基引发的主链"回咬"机制为主;在480～630℃则通过链间折叠发生环降解反应。主链"回咬"和链间环降解反应均会导致树脂基体交联密度降低,力学性能下降,产生"粉化"。甲基乙烯基硅橡胶在其裂解温域370～780℃主要发生侧基交联反应,树脂基体交联密度上升,热稳定性提高。白炭黑对于2种硅橡胶基体的热稳定性提升最为显著;铁红、云母等均会在高温下与硅橡胶基体产生共融,减缓硅橡胶基体的高温裂解。     

芳纶纤维和丁腈橡胶体系绝热层新配方的研制

采用含卤-锑的阻燃剂,芳纶纤维代替石棉纤维,研制了耐烧蚀的丁腈橡胶绝热层新配方(D210配方)。试验研究了芳纶纤维用量、卤-锑阻燃剂用量及纤维排布方向对绝热层烧蚀性能的影响;研究了增塑剂用量对绝热层玻璃化温度的影响。结果表明,芳纶纤维用量为4份时,绝热层烧蚀性能最佳,线烧蚀率为0.051 mm/s,质量烧蚀率为0.069 g/s;在选定的阻燃剂用量范围内,阻燃剂对绝热层烧蚀性能影响不大;所选增塑剂用量为20份时,玻璃化温度Tg可达-40℃。试验还对绝热层力学性能、硬度、粘接性能、比热容、导热等性能进行了测试,表明新研制的耐烧蚀橡胶有可能成为替代传统的石棉纤维和丁腈橡胶体系的固体火箭发动机燃烧室内绝热层。     

PBT/增塑剂共混物相容性的介观动力学模拟

用分子动力学(MD)和介观动力学(MesoDyn)法模拟研究了粘合剂3,3-二叠氮甲基氧丁环-四氢呋喃共聚醚(PBT)与A3[双(2,2-二硝基丙醇缩甲醛(A2)与双(2,2-二硝基丙醇)缩乙醛(A1)质量比1∶1混合物]、端叠氮基聚叠氮缩水甘油醚(GAPA)等不同增塑剂组成的共混体系的溶度参数和共混物分子间的Flory-Huggins作用参数,预测了共混物的相容性和介观形貌。结果表明:室温下PBT/A3共混体系,增塑比为1.4时体系的相容性最好;对增塑比为1.2的PBT/A3/GAPA共混物,PBT/A3/GAPA配比为10/2/10体系的相容性最好。     

航天器舷窗玻璃超高速撞击损伤与M/OD撞击风险评估

用北京卫星环境工程研究所的18mm口径二级轻气炮(TLGG)和20 J激光驱动微小飞片装置(LDFF-20)对用作航天器舷窗玻璃的熔融石英玻璃的超高速撞击损伤特性进行了实验研究和分析.其中,TLGG发射的球形铝弹丸直径分别为1 mm和3 mm,速度2～6.5 km/s;LDFF-20发射的圆柱形飞片厚度7 μm,直径1 mm,速度1～8.3 km/s.撞击结果为:对12 mm厚的熔融石英玻璃,直径为3mm的弹丸甚至在2.8 km/s的低速下就将其穿透,而直径为1 mm的弹丸在6.5km/s的高速下没有穿透,这说明弹丸直径对撞击损伤特性有很强的影响;LDFF-20发射的微小飞片的撞击仅在玻璃表面产生很浅的凹坑,没有裂纹产生,但微小飞片的累积撞击损伤明显地降低了玻璃的透光性.实验初步获得了侵彻深度PC、侵彻直径D1与弹丸撞击速度Vp、弹丸质量Mp之间的经验关系.依据实验结果和目前的微流星体/空间碎片(M/OD)环境工程模型,建议对于高度为400 km、轨道倾角42°、寿命为3年的典型航天器,其舷窗玻璃的临界安全(非穿透)厚度至少为12mm.     

Hydrogen emission in meteors as a potential marker for the exogenous delivery of organics and water

We detected hydrogen Balmer-alpha (H(alpha)) emission in the spectra of bright meteors and investigated its potential use as a tracer for exogenous delivery of organic matter. We found that it is critical to observe the meteors with high enough spatial resolution to distinguish the 656.46 nm H(alpha) emission from the 657.46 nm intercombination line of neutral calcium, which was bright in the meteor afterglow. The H(alpha) line peak stayed in constant ratio to the atmospheric emissions of nitrogen during descent of the meteoroid. If all of the hydrogen originates in the Earth's atmosphere, the hydrogen atoms are expected to have been excited at T = 4400 K. In that case, we measured an H(2)O abundance in excess of 150 +/- 20 ppm at 80-90 km altitude (assuming local thermodynamic equilibrium in the air plasma). This compares with an expected <20 ppm from H(2)O in the gas phase. Alternatively, meteoric refractory organic matter (and water bound in meteoroid minerals) could have caused the observed H(alpha) emission, but only if the line is excited in a hot T approximately 10000 K plasma component that is unique to meteoric ablation vapor emissions such as Si(+). Assuming that the Si(+) lines of the Leonid spectrum would need the same hot excitation conditions, and a typical [H]/[C] = 1 in cometary refractory organics, we calculated an abundance ratio [C]/[Si] = 3.9 +/- 1.4 for the dust of comet 55P/Tempel-Tuttle. This range agreed with the value of [C]/[Si] = 4.4 measured for comet 1P/Halley dust. Unless there is 10 times more water vapor in the upper atmosphere than expected, we conclude that a significant fraction of the hydrogen atoms in the observed meteor plasma originated in the meteoroid.     

高压空气大流量现场校准装置设计与实现

为满足新型吸气式发动机研制对于试验系统高压大流量超声速来流模拟条件下气体流量的准确测量和现场校准的迫切需求,设计了一套基于高压、大流量p.V.T.t法和比较法的流量现场校准装置(以下简称现场校准装置),通过原级p.V.T.t法与次级标准音速喷嘴相结合的方式,实现了压力3~23 MPa和流量1~60 kg/s条件下音速喷嘴流量系数的校准、溯源和试验系统空气流量准确测量,高压空气大流量现场校准装置扩展不确定度为0.84%。     

PEPA/AP膏体推进剂配方研究

开展了PEPA／AP型膏体推进剂配方研究。结果表明，PEPA／AP膏体推进剂的流变行为遵循Ostwalld幂定律，通过增稠剂种类和含量的改变可有效调节膏体推进剂的流变参数，增调剂NJ－4可使膏体推进剂具有良好的稳定性并保持稳定的流动性。燃烧调节剂FC－1能有效改善配方的点火和燃烧性能，拓宽了燃速范围（6．86MPa下，燃速15mm/s指高到15mm/s以上），显著降低了燃速压强指数（2．94－8．83MPa下，压强指数由0．71降至0．4）。     

短切炭纤维/酚醛树脂胶粘剂的配方研究

为确定最佳组分含量,采用正交实验法对“酚醛树脂(PF) 纳米S iO2粉 石墨粉 ZrO2粉 短切炭纤维”胶粘剂体系进行了配方研究,并探讨了组分含量对胶粘剂性能的影响。得到的最佳配方为“PF 2%纳米S iO2粉 1%石墨粉 1%ZrO2粉 4%短切炭纤维”,其对石墨材料的粘接强度达11.6 MPa,胶粘剂本体线烧蚀率为0.058 mm/s,质量烧蚀率为0.0732 g/s。胶粘剂可进一步用于粘接修复C/C复合材料喉衬构件的工艺缺陷。     

The putative mechanical strength of comet surface material applied to landing on a comet

The comet lander PHILAE (part of the ESA mission ROSETTA) is going to touch down on comet 67P/Churyumov–Gerasimenko in 2014. Landing dynamics depend on the mechanical strength of the surface material: in an extremely soft material, the lander (100 kg, 1 m/s touch-down velocity) may sink in too deep for successful operation while on a very hard surface the probability for bouncing and overturning increases. It is shown that direct knowledge on the strength of cometary surface material is very limited. In our view, even the Deep Impact experiment could not provide a reliable value of the mechanical strength of comet Tempel 1. We discuss the definition of “strength” and revise the ideas on cometary surface strength and theories that describe the low-velocity (≈1 m/s) impact of blunt bodies into dust-rich, fluffy cometary materials. Available direct and indirect measurements and data are critically reviewed. Lessons learnt from laboratory measurements to verify our equations of motion are presented as well. Conclusions for Philae are drawn: most likely, the soft landing will lead to a typical penetration of the lander's feet of up to 20 cm.     

Orbiting solar telescope on “Salyut-4” station

The orbiting solar telescope on Salyut-4 (F = 2,5 m, d = 250 mm) produces images of the Sun on the entrance slit of a stigmatic two-grating spectrograph (R₁ = 1 m, N₁ = 1200 lines/mm; R₂ = 0.5 m, N₂ = 2400 lines/mm, dispersion 16 Å/mm, spectral resolution 0,3 Å). The automatic system keeps the observed solar features on the slit of the spectrograph with an accuracy of 3–4 arc sec. The far UV-spectra (970–1400 Å) of solar flares, brightenings, flocculi and prominences were photographed and fresh coatings of mirrors were made during the flight.     

Human thermohomeostasis onboard "Mir" and in simulated microgravity studies.

Significant changes of thermogomeostatic parameters was obtained by thermotopometric method using the techniques simulate of microgravity effects: bed rest, pressurized isolation, suit immersion (SI). However, each of ground models made rectal temperature (T) trend downward. The autothermometric study (24 and 12 sessions, 2-13th and 6-174th flight days) was carried out onboard "Mir" by two flight engineers who had preliminary tested at SI (1-2 days). Studies of German investigators onboard "Mir" confirmed: rectal T must be higher in space flight as compared to the normal environment (n=4). Comparative studies suggest that microgravity is a key factor for the human body surface T raise and abolishment of the external/internal T-gradient. T-homeostasis was not really changing during missions and could be regarded as acute effect of microgravity. After delineation of changes in body surface T--by Carnot's thermodynamic law--rectal T raise should have been anticipated. Facts pointing to the excess entropy of human body must not be passed over.     

Determination of epsomite-hexahydrite equilibria by the humidity-buffer technique at 0.1 MPa with implications for phase equilibria in the system MgSO4-H2O

Epsomite (MgSO(4).7H(2)O) and hexahydrite (MgSO(4).6H(2)O) are common minerals found in marine evaporite deposits, in saline lakes as precipitates, in weathering zones of coal and metallic deposits, in some soils and their efflorescences, and possibly on the surface of Europa as evaporite deposits. Thermodynamic properties of these two minerals reported in the literature are in poor agreement. In this study, epsomite-hexahydrite equilibria were determined along four humidity-buffer curves at 0.1 MPa and between 25 and 45 degrees C. Results obtained for the reaction epsomite = hexahydrite + H(2)O, as demonstrated by very tight reversals along each humidity buffer, can be represented by ln K(+/- 0.012) = 20.001 - 7182.07/T, where K is the equilibrium constant, and T is temperature in Kelvin. The derived standard Gibbs free energy of reaction is 10.13 +/- 0.07 kJ/mol, which is essentially the same value as that calculated from vapor pressure measurements reported in the literature. However, this value is at least 0.8 kJ/mol lower than those calculated from the data derived mostly from calorimetric measurements.     

Modes of uncontrolled rotational motion of the <Emphasis Type="Italic">Progress M-29M</Emphasis> spacecraft

We have reconstructed the uncontrolled rotational motion of the Progress M-29M transport cargo spacecraft in the single-axis solar orientation mode (the so-called sunward spin) and in the mode of the gravitational orientation of a rotating satellite. The modes were implemented on April 3–7, 2016 as a part of preparation for experiments with the DAKON convection sensor onboard the Progress spacecraft. The reconstruction was performed by integral statistical techniques using the measurements of the spacecraft’s angular velocity and electric current from its solar arrays. The measurement data obtained in a certain time interval have been jointly processed using the least-squares method by integrating the equations of the spacecraft’s motion relative to the center of mass. As a result of processing, the initial conditions of motion and parameters of the mathematical model have been estimated. The motion in the sunward spin mode is the rotation of the spacecraft with an angular velocity of 2.2 deg/s about the normal to the plane of solar arrays; the normal is oriented toward the Sun or forms a small angle with this direction. The duration of the mode is several orbit passes. The reconstruction has been performed over time intervals of up to 1 h. As a result, the actual rotational motion of the spacecraft relative to the Earth–Sun direction was obtained. In the gravitational orientation mode, the spacecraft was rotated about its longitudinal axis with an angular velocity of 0.1–0.2 deg/s; the longitudinal axis executed small oscillated relative to the local vertical. The reconstruction of motion relative to the orbital coordinate system was performed in time intervals of up to 7 h using only the angularvelocity measurements. The measurements of the electric current from solar arrays were used for verification.