耐热200℃韧性双马来酰亚胺树脂基复合材料的性能研究

由烯丙基化合物与双马来酰亚胺（ＢＭＩ）共聚而成的Ｘ４５０２树脂，具有优良的综合性能，由Ｘ４５０２树脂的丙酮溶液与Ｔ－３００碳纤维制备的预浸料具有良好的成型工艺性。Ｔ－３００／Ｘ４５０２复合材料具有突出的抗断裂性能（ＧＩＣ＝２１５Ｊ／ｍ＾２）和良好的湿／热稳定性，在２００℃下具有较高的强度保持率。     

无机粒子对石墨烯微片／环氧树脂复合材料导电性能的影响

以 KNG-CZ030石墨烯（graphene nanoplatelets,GNPs）为导电填料,环氧树脂（E-54）为聚合物基体,2-乙基-4甲基咪唑（2,4-EMI）为固化剂,采用溶液混合和超声分散的方法制备导电复合材料。通过添加无机粒子（NaCl, TiO2）,研究了无机粒子对石墨烯微片分散均匀性的影响以及对 GNPs ／E-54复合材料导电性能的影响。实验结果表明：加入 NaCl 和 TiO2提高了石墨烯微片在基体中的分散性,降低了复合材料室温体积电阻率,即提高了导电性能;NaCl ／GNPs ／E-54和 TiO2／GNPs ／E-54复合材料室温体积电阻率为106Ω·m 时,石墨烯质量分数分别为0．75％和0．73％,与未添加无机粒子的 GNPs ／E-54复合材料质量分数0．97％相比有所降低。     

激光—超声旋涡测量技术

综述了激光－超声旋涡测量技术的特点,详细介绍了目前国内外采用的两种实用测量技术（超声脉冲信号法和超声连续信号法）并给出了细长三角翼和函道风扇流场的应用测量结果。     

铸造A356.2（Sc，La）铝合金研究

采用铸造工艺制备了A356.2（Sc，La）铝合金，测试分析了稀土元素Sc和La对铝合金中共晶硅的细化作用及对合金力学性能的影响。结果表明，单独添加稀土元素La对A356.2（La）铝合金中的共晶硅有一定的细化作用，但对力学性能的改善作用不大。而含有两种稀土元素0.38%Sc+0.14%La的A356.2（Sc，La）铝合金中的共晶硅细化作用较好和力学性能更高，其共晶硅细化到2.3 μｍ，抗拉强度和伸长率分别达到181.6 MPa和4.0%。稀土Sc和La对共晶硅的细化作用主要是弥散强化和细晶强化共同作用的结果，这两种强化与铝合金中析出的Al₃Sc相和稀土La相有关。     

4A分子筛介孔球的制备及表征

以正己烷／十六烷基三甲基溴化铵（CTAB）／正辛醇混合微乳液为反应体系,以硅酸钠和铝酸钠为反应原料,采用微乳法首次合成4A分子筛介孔球。利用透射电子显微镜（TEM）和X射线粉末衍射（XRD）对所得产品的形貌、尺寸、结构进行了表征。结果表明,采用微乳法可以成功制得具有笼型结构的纳米4A分子筛介孔球,由约8nm的4A分子筛粒子沿表面活性剂所包裹的油水界面堆积而成,其直径大小约为40nm。     

C/C—SiC复合材料的制备与性能

采用化学气相渗透（CVI）法和液相浸渍有机物先驱体混合工艺制备了C／C－SiC复合材料，并对复合材料力学性能、抗烧蚀性能和抗氧化性能进行表征。结果表明：制备的C／C－SiC复合材料在基本保证C／C复合材料力学性能的基础上，抗氧化和抗烧蚀性能得以大幅度提高，提出了制备兼具C／C复合材料与陶瓷材料的技术途径。     

一种快速制备C/C材料方法的探索研究

介绍了一种新的Ｃ／Ｃ材料制备方法－－快速化学液气相渗透致密法。利用该技术,采用碳毡作预制体,以两种液态低分子有机物作碳源前驱体沉积时间在３ｈ内,沉积温度在９００℃￣１１００℃范围内可获得密度达１．７４ｇ／ｃｍ＾３的Ｃ／Ｃ材料。碳纤维表面最大沉积速率可达６４μｍ／ｈ,比传统的等温ＣＶＩ沉积速率（０．１μｍ／ｈ￣０．２５μｍ／ｈ）提高了２００倍以上,并初步分析了该技术快速致密多孔预制体的机理。     

面对21世纪的改进从“黄蜂”到“超黄蜂”(下)

改进电子设备在美国海军为F／A-18作规划时，E／F型的改进只是个开端。海军在解决了原来机体的缺陷之后，现在急于要搞清F／A—18上电子设备的局限性。为了使成本不致太高，目前的E／F型利用了C／D型中90％的电子设备。到2005年左右，波音公司将把即将完成试验的下一代电子设备装上飞机。新的基本航空电子设备包括正在为C／D型和E／F型两种机型研制的改进项目，有高级寻的前视红外（ATFLIR）吊舱、安装在头盔上的信号系统（JHMCS）和多功能信息分配系统（MIDS）。除此之外，还计划为E／F型作一些单独的改进，从一体化防御性电…     

热处理对Bi超导带材微结构和J_C值的影响

采用粉末装管加工技术（Ｐｏｗｄｅｒ－ｉｎ－ｔｕｂｅｔｅｃｈｎｉｑｕｅ）制备出了ＢｉＰｂＳｒＣａＣｕＯ／Ａｇ复合超导带材。研究了热处理对带材微观结构和临界电流密度（Ｊ＿ｃ）的影响。试验表明,合理的热处理温度范围为８４０～８５０℃,冷却速率为５０～１００℃／ｈ。     

DGPS／RA引导飞机进近着陆研究

定位系统（ＧＰＳ）正在获得越来越广泛的应用．本文叙述了采用差分全球定位系统／高度表（ＤＧＰＳ／ＲＡ）组合技术引导飞机进近着陆的研究试验，并对国际上ＧＰＳ引导飞机进近着陆应用研究的现状和发展趋势作了分析。     

搅拌对熔铸—原位反应TiB2／Al和TiC／Al复合材料微观组织的影响

研究、开发了一种熔铸－ 原位反应颗粒增强铝基复合材料制备技术,探讨了搅拌工艺对３ｖｏｌ％ ＴｉＢ２ 和３ｖｏｌ％ ＴｉＣ颗粒增强铝基复合材料微观组织的影响。结果表明,采用圆盘状叶片的搅拌装置对获得颗粒均匀分布、组织致密的铝基复合材料十分有利。     

Ultraviolet and optical observations of HDE 245770/ A 0535+26 system during an X-ray flare

We present high and low dispersion UV spectra of HDE 245770, which is the optical counterpart of the recurrent transient X-ray pulsar A 0535+26,during a decay of an X-ray flare. UBV photometric measurements and medium dispersion optical spectra were simultaneously obtained.The energy distribution of the star in the 12 – 10 micron range is compared with the models of Kurucz and Poeckert and Marlborough.In this phase, HDE 245770 does not show evaluable variations with respect to the quiescent X-ray phase.     

A 0535 + 26/HDE 245770: A typical X-ray/Be system

Among the X-ray/Be systems, A 0535 + 26/HDE 245770 has been noted, since its discovery, for its peculiar features in several respects, in a wide energy range. For this reason and for a series of concomitant favorable causes, this system has been one of the most studied among the massive X-ray binary systems. The most remarkable incident was that its optical identification with an early-type-emission-line star (O9.7IIIe) has led to a deep studies on Be stars and their interactions with neutron stars, which have allowed to discover, without unbiguity, the presence of optical indicators of consequent X-ray flares, as well as that Be stars in X-ray/Be systems behave just as normal Be stars. Overmore, thanks to the multifrequency coordinated observations of this system, the X-ray emissions from binary companion of the Be stars are best explained by assuming the presence of a thick equatorial disk with low expansion velocity and a thin polar region with high expansion velocity. This picture reconciled the strong discrepancy in mass loss rate evaluations coming from IR and from UV measurements, assuming that the observed regions are enterely distinct from each other, one being a high-density, low-velocity region, and the other being a low-density, very hot, rapidly-expanding disk-like zone.Since, this picture seems to be the best up-to-date frame to cuckold all the experimental panorama available on X-ray/Be systems, we would like to paint in this paper the multifrequency behaviour of A 0535 + 26/HDE 245770, which is the best studied among such systems, in order to stimulate future coordinated experimental-theoretical works on this very interesting class of objects.     

On the optical variability of a be star,HDE 245770, — the optical counterpart of the transient X-ray pulsar A0535+26

Photoelectric WBVR observations of Be star HDE 245770=V 725 Tau, the optical counterpart of the transient X-ray pulsar A0535+26, having a pulse period of about 104 s, were conducted for more than 10 years. An irregular long-term optical variability of the star with amplitudes of the order of a few tenths of magnitude was found to be a usual phenomenon. In some cases rapid changes of the star's optical luminosity with a characteristic period of a few tens of minutes or a few hours, and an amplitude of several hundredths of magnitude in all the spectral bands used, which have practically coincided or correlated with the X-ray pulsar outbursts detected by X-ray satellites, were observed.Photoelectric recording of the optical flux from HDE 245770 were made in 1981–1982 with a time resolution of 1 second and 10 s, respectively, in theR spectral band (₀ 7000 Å) and in the narrowH -emission-line band (_1/2 75 Å) using a 48-cm reflector of High-Mountain Tien-Shan observatory of the Sternberg Astronomical Institute near Alma-Ata. An analysis of autocorrelation functions of the flux changes from object under study and a comparison with the star BD+26° 876 indicated the variability of luminosity of V 725 Tau in theR spectral band on a time scale of a few tens of second; this variability resembles shot noise with a characteristic time of stochastic bursts of about 15–20 s and their amplitudes of about a few tenths of a percent. InH -emission-line radiation autocorrelation functions and power spectra show quasiperiodic variability of luminosity of HDE 245770 with a characteristic period of about 100–150 s and an amplitude in the neighbour-hood of 0.5%. The latter result is not quite reliable because of not quite fine weather conditions during the observations; independent observations and check-up are required.     

磁场辅助激光熔覆铝基金属玻璃覆层

为提高铝合金的表面性能,采用磁场辅助激光熔覆的方法在5083铝合金表面制备了Al-Ni-Y-Co-La五元金属玻璃熔覆层,并对其进行组织成分及性能分析。实验结果表明：熔覆层主要由非晶相、α-Al相以及Al₄NiY等金属间化合物组成,旋转磁场的搅拌作用使熔覆层非晶相含量由10.2%提高到30.7%,且能够有效抑制多道搭接和多层堆积过程中重熔区晶粒的生长,细化了熔覆层晶粒组织,降低了残余应力,提高了显微硬度及韧性,使其平均显微硬度从278 HV_0.1提高至335 HV_0.1,且波动较小,平均抗拉强度为303 MPa,为基体拉伸件的110.2%,平均伸长率为6.79%,为基体的33.1%。     

表面活性剂类型和用量对闭孔三聚氰胺泡沫的影响

研究吐温80和十二烷基苯磺酸钠(SDBS)两种类型表面活性剂及SDBS用量对闭孔三聚氰胺泡沫的影响。用三聚氰胺、甲醛合成三聚氰胺树脂,并制备泡沫样品进行测试。树脂表面张力测试结果显示相同用量下,相比于吐温80,SDBS使树脂表面张力更小,且随着SDBS用量增加,树脂张力呈现先减小后不变的趋势。SEM、力学性能测试分析结果显示,表面活性剂用量为3%时,相比于吐温80,SDBS制得泡沫孔径小且均匀。随着SDBS用量增加,泡沫孔径减小,均匀度先提高后降低,泡壁膜撕裂严重。受泡沫结构影响,SDBS用量为3%时,泡沫的压缩性能最好。     

表面活性剂对Ni-Co-PTFE复合电镀的影响

研究了表面活性剂对Ni-Co-PTFE复合电镀的影响情况，发现表面活性剂种类及其用量对该复合镀层中PTFE含量及镀层摩擦性能有显著的影响，其中以非离子表面活性剂与全氟阳离子表面活性剂组成的复合活性剂效果最好，其最佳用量为1g/L，获得的复合镀层微观表面结构致密，微粒分布均匀，摩擦系数最小，显微硬度HV0.1最大。     

搅拌摩擦焊搅拌头的研究进展

概述了国内外铝合金、镁合金、铜合金、钛合金及钢铁材料等多种合金搅拌摩擦焊用搅拌头的结构设计、材料、磨损失效和寿命等方面的研究进展,对比了各搅拌头的结构设计和材料性能优缺点,分析了搅拌头失效方式和寿命,展望了搅拌头的研究发展趋势。     

半固态金属材料EMS法制备过程中的微观组织相场法模拟

利用相场法模拟了电磁搅拌法(EMS法)制备半固态金属材料(Al-4Cu-Mg合金)过程中微观组织的演变,分析和讨论了宏微观因素,如扰动强度、各向异性强度、固液相中扩散系数比等对微观组织演变的影响。结果表明:界面层厚度的减小,使得固相颗粒的外形轮廓更接近于圆形;固相中扩散系数增加,可以减少微观偏论析的程度;扰动强度越大,初生相的微粒越细,其形态越趋向于球形。     

CygX-1/A candidate of the black hole

Among discrete galactic X-ray sources, Cyg X-1 has been noted for its peculiar features in several respects. It is one of the few sources with a hard power law spectrum extending beyond several hundred keV. Cyg X-1 also distinguishes itself by its profound time variability over a wide range of time scales. The most remarkable incident was that its optical identification with a spectroscopic binary HDE226868 has led to a presumption that it is a black hole. This possibility has induced continuous interests in the physical character of this source in conjunction with the nature of the black hole. The purpose of this paper is to summarize presently available pieces of knowledge on this source to help the design of future experimental and theoretical works, while the complexity of the source characteristics still has prevented us to construct a clear, coherent picture of this source in spite of the fact that numerous observational facts have been accumulated.