盐雾腐蚀对NiCoCrAlY涂层性能的影响

利用中性盐雾试验对物理气相沉积制备的NiCoCrAlY防护涂层进行常温腐蚀,研究了常温盐雾腐蚀对NiCoCrAlY涂层的微观形貌以及高温性能的影响.试验结果表明:经过盐雾腐蚀的涂层表面的均匀性和完整性均被破坏,涂层表面产生了大量的腐蚀坑;高温循环氧化以后,表面形成的Al₂O₃氧化膜变得粗糙、破碎且不连续,而且氧化膜容易剥落,降低了涂层的高温抗氧化能力,缩短了涂层的使用寿命.      

模拟服役环境中航空导管连接件耐蚀性能研究

采用自制的航空导管连接件腐蚀试验系统,研究了航空镀镉45^#钢导管连接件在模拟服役环境中的气密性、油压气密性以及应力腐蚀、表面腐蚀等性能.对该导管连接件在高温盐水溶液6%NaCl(90±5)℃浸泡与空气烘烤(60±5)℃循环200次条件下的表面腐蚀及应力腐蚀行为进行了评价;探讨了在模拟服役环境中,45^#钢发生腐蚀的机理.10^＃航空油不对镀镉45^＃钢造成腐蚀.镀镉45^#钢导管连接件在模拟服役环境中只是表面镀镉层发生腐蚀破坏,基体45^#钢只发生轻微腐蚀,表明45^＃钢导管连接件表面的镀镉磷化层可作为阳极性镀层而对基体金属进行保护.在最小屈服强度0.85的弯曲应力水平作用下,无应力腐蚀倾向.导管材料铝合金LF2-M与连接件45^#钢在6％NaCl水溶液中只有很小的电偶腐蚀电流,平均电偶电流密度为0.185μA/cm²,证明该类导管及导管连接件能安全地进行偶接.     

湿热环境下湿度对塑封器件贮存可靠性的影响

针对塑封电子器件在湿热环境下的贮存可靠性问题,通过湿热实验考察了湿热环境中的湿度因素对某型塑封器件贮存过程中的吸湿行为、封装表面状态以及电性能的影响.结果表明:环境湿度对塑封器件吸湿过程有显著影响,在同样的温度下相对湿度越高,器件的吸水速率越大,达到饱和时的饱和水汽含量也越大,而湿度对器件水汽吸收达到饱和时间的影响比较小,一般贮存300 h后水汽含量都达到饱和;塑封器件在湿热环境下贮存的主要失效模式是外引线腐蚀,且随着相对湿度增加腐蚀程度更加严重,分析认为器件封装过程中在外引线表面造成的断口、裂纹和针孔等缺陷处是腐蚀发生的敏感区;在贮存期内湿度对塑封器件的电性能影响不大.     

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.     

基于近邻传播聚类的航空电子部件LMK诊断模型

针对小样本条件下,航空电子部件功能模块故障诊断精度不高的问题,将局部多核学习（LMKL）算法的多分辨率解释与局部特征自适应表示能力和超限学习机（ELM）运算高效的特点相结合,提出一种新的局部聚类MK-ELM（LCMKELM）诊断模型。通过引入近邻传播（AP）聚类,在挖掘训练样本局部特征信息的同时,有效约减了局部算法的计算复杂性,避免了过学习问题的出现;通过分别分析输入空间与特征空间的聚类特征,构造了相应的2种选通函数M₁、M₂,以优化选通函数的模型参数取代优化局部权重,有效解决了核超限学习机（KELM）的对偶优化形式关于局部权重二次非凸的问题。将本文模型应用于某型机旋转变压器激励发生电路功能模块故障诊断,结果表明:相比于4种常用的多核诊断算法,模型在实现低漏警、低虚警的同时,采用M₁选通函数的诊断算法将诊断精度平均提升了3.80%,采用M₂选通函数的诊断算法将诊断精度平均提升了5.98%。同时,模型在实现与流行的LMKL算法相近的训练时间的同时,测试时间更短。      

环境温度对汽油缸内直喷汽车排放的影响

选取2辆典型汽油缸内直喷汽车(GDIV),在环境舱内进行了不同环境温度下,车辆冷启动和热启动后按照全球轻型车统一测试循环(WLTC)运行时的排气污染物试验,测量并分析了GDIV排气中的气态污染物和颗粒物,旨在为GDIV排放系统设计、控制策略制定以及评价汽车排放对环境影响的相关研究提供理论依据。研究结果表明:环境温度对GDIV试验车辆冷启动和热启动的颗粒物数量(PN)和颗粒物质量(PM)排放因子影响显著。环境温度低于14℃,冷启动工况下行驶时PN排放难以满足国Ⅵ排放标准限值,总碳氢化合物(THC)和CO的排放因子受温度的影响显著,热启动时影响不明显。无论是热启动还是冷启动工况,当温度从-7℃逐步上升到40℃时,试验车辆的CO₂排放因子呈现先减少后增加的变化规律,2辆车在热启动时的CO₂排放因子比冷启动时平均降低4%和7%。冷启动和热启动时,氮氧化物(NO_x)排放因子受温度的影响均没有明显的规律。      

γ-TiAl基自生复相材料的显微组织特征

研究了添加硼、硅、碳的 γ-TiAl基自生复相材料的显微组织特征.在压力4?GPa、温度1?273?K、反应合成时间60?min的条件下,通过粉末间的原位置换放热反应制备了样品.研究发现:Ti-Al-B三元合金含有TiAl相、Ti₃Al相和TiB₂相;Ti-Al-Si三元合金含有TiAl相、Ti₃Al相和Ti₅(Al,Si)₃相;Ti-Al-C三元合金含有TiAl相和Ti₃AlC相;Ti-Al-B-Si四元合金含有TiAl相、Ti₃Al相、TiB₂相和Ti₅(Al,Si)₃相;Ti-Al-B-C四元合金含有TiAl相、Ti₃AlC相和TiB₂相;Ti-Al-B-Si-C五元合金含有TiAl相、Ti₃AlC相、TiB₂相和Ti₅(Al,Si)₃相,其组织非常相似于预先设计的组织.在此基础上就不同相对性能的影响进行了分析.     

等离子体处理对非晶态合金镀层表面改性研究

通过微波等离子体处理方法对Ni-W、Ni-W-B非晶态合金镀层表面进行改性的研究,测量了表面改性对非晶态镀层耐蚀性、表面成分及结构的影响.结果表明,经过微波等离子体处理过的Ni-W、Ni-W-B非晶态合金镀层,提高了在H₂SO₄、HNO₃溶液中的耐蚀性以及在700℃环境下的抗氧化性能;微波等离子体处理过的非晶态合金镀层表面含W量和含O量相对提高了;镀层结构仍然是非晶态.     

激发跃迁速率对热力学非平衡氮气紫外辐射的影响

基于氮气的碰撞-辐射（CR）模型,计算了速度为6.2 km/s、初始压力为133 Pa的高超声速流动激波中N₂和N₂+分子电子能级的分布情况,分析了不同激发跃迁速率模型对电子能级分布及辐射光谱模拟的影响。针对流动中热力学非平衡区域和平衡区域,在300~440 nm的辐射光谱开展了逐线法的数值模拟,并与激波管实验测量光谱进行了对比。结果表明,目前的激发跃迁速率均存在偏差,综合Park模型的爱因斯坦系数和Johnston模型的碰撞激发速率可以得到与实验结果最为接近的辐射光谱。      

太阳E10.7指数的反演及预报方法

针对高层大气密度预报和轨道预报业务中对新型太阳紫外辐射指数E_10.7的需求,基于TIMED-SEE观测仪器提供的0.1～105 nm太阳辐射强度数据,开展了E_10.7指数反演和中期预报研究。 E_10.7指数是太阳光谱中波长为0.1～105 nm的辐射流量,单位与F_10.7指数相同（sfu,1 sfu=10–22 W·m–2·Hz–1）。 TIMED-SEE观测仪器提供的0.1～105 nm太阳辐射强度实测值具有高时间分辨率、延迟时间短和易获得的优势,利用最小二乘法拟合可反演出准实时的E_10.7指数,均方根误差为5.445 sfu。利用高阶自回归模型对E_10.7的中期预报效果尚佳,未来27天的预报值平均相对误差为7.83%。利用同样方法还开展了E_10.7指数81天中心滑动平均值未来27天预报试验,未来27天的预报值平均相对误差仅为3.63%。      

H2O对空间站5A分子筛CO2去除性能影响

为进一步研究分子筛CO2去除系统应用于空间站的工作可靠性和鲁棒性,针对空间站4床分子筛(4-BMS)系统中可能出现的湿度失效保护问题展开了实验研究.测试了两种载人航天分子筛材料TC-5A与PSA-5A,研究了不同相对湿度对CO2吸附性能的影响;比较了相同湿度条件下,进口气体CO2浓度、粒径及吸附温度的变化对分子筛吸附CO2性能的影响,采用不同实验方法探究了H2O和CO2在两种分子筛材料中的竞争吸附关系.结果表明:PSA-5A吸附CO2性能优于TC-5A,但对H2O的吸附率略低于TC-5A.H2O的存在对分子筛吸附CO2影响非常大,空气中相对湿度达到60%时,分子筛基本失去了吸附CO2的能力.此外,温度升高会造成CO2的吸附量显著下降,但对H2O的吸附量影响相对较小,尤其是当相对湿度较高时.这对中国未来长期运行的空间站分子筛CO2去除系统工作有效性与工作鲁棒性的评价具有指导意义.     

光学原位法探针测量超低减排烟气

随着燃煤电厂超低减排的开展,烟气监测技术的要求也越来越严格。研制了应用差分光学吸收光谱(DOAS)和多波长消光的实时在线烟气监测探针,可同时对SO_2、烟尘等浓度进行监测。并在实验室进行了标定,SO_2浓度及烟尘反演误差均小于10%,不同浓度SO_2反演浓度曲线线性度好,线性相关系数为0.999 64。利用该系统对某燃煤电厂烟气中的SO_2和液滴颗粒物进行了现场监测。结果表明:该系统对SO_2、液滴颗粒的监测结果与锅炉运行工况、实际运行状况吻合。     

Atmospheric photochemistry above possible martian hot spots

Considering the possibility of outgassing from some localized sources on Mars, we have developed a one-dimensional photochemical model that includes methane (CH₄), sulfur dioxide (SO₂) and hydrogen sulfide (H₂S). Halogens were considered but were found to have no significant impact on the martian atmospheric chemistry. We find that the introduction of methane into the martian atmosphere results in the formation of mainly formaldehyde (CH₂O), methyl alcohol (CH₃OH) and ethane (C₂H₆), whereas the introduction of the sulfur species produces mainly sulfur monoxide (SO) and sulfuric acid (H₂SO₄). Depending upon the flux of the outgassed molecules from possible hot spots, some of these species and the resulting new molecules may be detectable locally, either by remote sensing (e.g., with the Planetary Fourier Spectrometer on Mars Express) or in situ measurements.     

Ablation and chemistry of meteoric materials in the atmosphere of Titan

We compute the input of meteoric materials expected on Titan, and integrate this dust model with an ablation model and a comprehensive chemical model, investigating the effects on the atmosphere and surface. We find that a water deposition of 10-100 times the expected interplanetary dust flux /7/, or a recent large impact, is required to produce the observed CO₂ abundance /2/. Ionisation due to meteoric activity is not likely to be higher than that due to other sources.     

Cometary atmosphere (gas and dust)

There is important progress now in the identifications and measurements of primary (parent) molecules in the inner coma of Comet Halley. H₂O, CO₂ and CO are definitely in the list, CH and some complicate organic molecules are suspected. Gas production rate for water vapor is Q_H2O 10³⁰ s⁻¹. The bulk of data doesn't contradict to the Whipple model of nucleus (with clathrate modification). Pronounced spatial structure of gaseous flow in the coma was observed, but in general measured properties of neutral gas in the coma of Comet Halley are not very different from predicted. Situation for dust is different. In situ dust measurements show that size spectrum and optical properties of particles in coma are substantively declining from predicted on the base of groundbased photometry. However there are discrepancies between Vega and Giotto dust counter data. Dust in the inner coma didn't prevent the succesful imaging of nucleus by TV on Vega 1 and 2.     

Intensity profiles of the multiple scattering light near the cometary nucleus

The multiple scattering of solar radiation in the cometary atmosphere is treated with the method of successive scattering. Referring to in situ measurements of comet Halley about the size and spatial distributions of dust, the optical thickness τ₁ of dust has been estimated, i.e. τ₁=0.03 at wavelength λ=0.62μm in a quiet time, but τ₁=0.3 when the outbursts/jets occur. In the derivation of τ₁, optical properties of dust including a mixing ratio of absorbing to silicate grains, are determined based on the polarimetry of P/Halley at λ=0.62μm observed during the phase angles over Nov. 1985 to May 1986 at the Dodaira Station of Tokyo Astronomical Observatory.

It is found that a temporary enhancement of τ₁ leads an increase of the upward reflected intensity when the surface albedo A of the nucleus is less than 0.04, but the reverse is true when A>0.04. On the other hand, the intensity of the downward radiation at the surface of the nucleus always decreases as an increase of τ₁.     

Physical properties of cometary dust: Relation of DIDSY data to grain properties

The Dust Impact Detection System (DIDSY) for the Giotto Halley Mission consists of two types of sensors for the detection of cometary dust particles: two impact plasma sensors and five piezo-electric momentum sensors. One sensor of each type is covered by a penetration film. A 1 μm thick aluminum film covers an impact plasma sensor. One momentum sensor is mounted onto the rear shield behind the 1 mm front shield made from aluminum. The parameters measured are the total charge released upon impact and the amplitude of the acoustic signal generated by the impact. Both quantities depend on the mass and speed of the impacting particles. At the impact speed of 68 km/sec the mass of cometary dust particles can be determined in the mass range from 10⁻¹⁷ g to 10⁻³ g. From the difference in the countrates measured by the sensors with and without penetration film the average bulk density of dust particles of masses 10⁻¹⁴ g and 10⁻⁶ g can be determined. With appropriate calibration an accuracy of a factor of 2 for both the mass and density determination can be obtained.     

Near infrared observations of comet Halley from Vega 2

Spatial distribution of the continuum radiation in the range of 0.95–1.9 μm presumes total dust production rate of the comet of 10ρ tonne s⁻¹ (ρ is the dust material density) and its angular distribution proportional cos . Observations of the water vapor band at 1.38 μ m reveal strong jets, their time shift from the dust jet measured in situ is consistent with gas velocity of 0.82±0.1 km s⁻¹ and dust velocity of 0.55±0.08 km s⁻¹. The OH vibrational-rotational bands observed are excided directly via photolysis of water vapor. Water vapor production rate deduced from the H₂O band and OH band intensities is 8×10²⁹ s⁻¹. Intensity of the CN(0,0) band result in the CN column density of 9×10¹² cm⁻², i.e. larger by a factor of 3 than given by the violet band.     

腐蚀条件下机翼主梁的疲劳寿命修正系数

针对歼击机主要疲劳关键件——机翼主梁,采用模拟试件进行加速试验环境谱下相当于地面停放不同年限的预腐蚀及谱载下疲劳试验,获得地面停放腐蚀影响系数C随地面停放年限T的变化曲线;由构成空中局部环境谱的各单一介质对谱载下寿命的影响试验,按百分比加权组合的方法获得空中腐蚀疲劳影响系数K.综合考虑C-T曲线与K,计算出不同无腐蚀条件下寿命和飞机年飞行小时数的组合所对应的腐蚀条件下机翼主梁疲劳寿命修正系数.为修正无腐蚀条件下寿命,从而评定腐蚀条件下机翼主梁寿命奠定了基础.