热处理温度对硅酸钇纳米晶相组成及显微结构的影响

以硝酸钇、硅酸钠和氢氧化钠为起始原料,采用微波水热法制备了硅酸钇纳米晶。研究了后期热处理温度对硅酸钇纳米晶的相组成和显微结构的影响。利用X-射线衍射仪(XRD)、场发射扫描电子显微镜(FESEM)和透射电子显微镜(TEM)对粉体进行了表征。结果表明:经微波水热可直接合成硅酸钇粉体,但其结晶性能较差,后期热处理有助于提高其结晶性能。随着热处理温度的升高,粉体中Y2SiO5相的含量增加,微晶的微观结构从棉絮状结构逐渐向柱状结构转变,Y2SiO5纳米晶沿[378]取向生长。     

pH值对硅酸钇涂层结构影响的研究

采用一种新颖的水热电沉积方法直接在石墨表面制备了硅酸钇涂层,利用XRD,EDS和SEM等测试手段对涂层进行测试分析,重点研究了电沉积前驱溶液pH值对涂层显微结构的影响.结果表明:当前驱液的pH值为1.5～3.0及水热温度为150℃时,即可制备出硅酸钇涂层.随前驱液pH值增加,涂层开裂趋势减弱,结晶趋势增强,致密度有所提高.     

使用预制的硅酸乙酯粘结剂制造熔模精铸壳型

研制的预制硅酸乙酯粘结剂用于代替工业硅酸乙酯(ЭТС-32和ЭТС-40)制造熔模精铸用陶瓷壳型。试制的工业批量产品已在一系列企业中试用。研究和试用结果证明,使用预制粘结剂制造熔模精铸壳型有良好的前景,有必要尽快投入工业生产。该工作为苏联航空材料研究院科研成果在企业推广的实例。     

钇对Ti-23Al-25Nb合金压缩性能的影响

采用SEM和XRD分析热处理后合金试样的显微组织及相组成,用TEM分析原始组织中钇的存在方式.结果表明,钇在原始组织中以Y2O3形式存在;钇增加O相衍射峰,提高Ti-23Al-25Nb合金压缩性能,如抗压强度、压缩率等,钇的强化作用是由于Y2O3第二相粒子强化和钇细化晶粒的晶界强化共同作用的结果.     

化学气相渗透制备氧化硅基复合材料

 以正硅酸乙酯为氧化硅先驱体,以 Nextel4 80纤维三维编织体作为沉积载体,采用化学气相渗透的方法制备了 Nextel4 80 /氧化硅复合材料。研究了正硅酸乙酯温度和沉积温度对沉积速率和渗透效果的影响,分析了沉积过程中产生瓶颈效应和固相粉末的原因以及沉积产物的相和复合材料的显微结构。结果表明 :1沉积速率随正硅酸乙酯温度和沉积温度的升高而显著升高;2瓶颈效应是由于正硅酸乙酯浓度过高,导致沉积速率过快引起的;3固相粉末是因为沉积温度过高,正硅酸乙酯分子或分解的过渡产物在到达沉积区域前已经完全分解引起的;4正硅酸乙酯为先驱体的化学气相沉积产物为无定型氧化硅;5化学气相沉积获得的无定型氧化硅基体与纤维有较佳的热匹配。     

PIP法制备3DNextelTM720／Mullite复合材料

采用先驱体浸渗热解法制备了 3DNextelTM 72 0 Mullite复合材料 ,并对基体的组分控制、复合材料致密化以及热处理温度对复合材料强度的影响进行了研究。结果表明 ,采用正硅酸已酯和异丙醇铝作为先驱体可以在相对低温 (≤ 12 0 0℃ )通过循环浸渗热解制备孔隙率低于 2 0 %的复合材料。     

快速激光标记系统

东芝公司出售的高速钇铝柘榴石激光标记系统的最大平均输出功率为300W,是同类产品的输出功率的三倍,该公司称使用LAY726C和合成树脂材料(如塑料)时,标记速度则为一般系统的两倍。该系统能在未处理的钢材、铝或其他金属及陶     

控制航空发动机运转间隙的热喷涂封严涂层

介绍了控制航空发动机运转间隙的热喷涂封严涂层的研究和应用，即等离子喷涂聚苯酯／铝硅封严涂层，氧－乙炔焰喷涂六方氮化硼陶瓷封严涂层，以及等离子喷涂钇稳氧化锆陶瓷封严涂层。此外还针对现有的问题提出了今后应开展的研究工作。     

有机－无机杂化介孔二氧化硅的合成与表征

以正硅酸乙酯和含有亚脲基的桥联硅烷为前驱体,以十六烷基三甲基溴化铵为模板剂,在碱性条件下制备了具有"蠕虫状"双介孔孔道结构和高比表面积的杂化介孔二氧化硅材料,并采用XRD、FTIR、NMR、TEM、SEM等手段对制备的材料进行表征.研究发现,亚脲基均匀地嵌入到介孔孔壁中,随孔壁中亚脲基基团含量的增加,介孔二氧化硅的有序性下降,比表面积减小.     

微量Y对Al-Mg-Si系合金组织性能的影响

在熔炼过程中以铝钇中间合金形式加入稀土Y元素,研究了0～0.45%范围内不同Y加入量对Al-Mg-Si系铝合金铸态组织、导电性能及高温蠕变抗力的影响。结果表明:经过适量稀土Y微处理后的合金材料具有细小均匀的铸态组织,平均晶粒尺寸维持在50μm左右,材料的导电能力得到一定程度的改善,最佳电导率比原来增加4%,实验材料的热稳定性显著增强,高温下的硬度、抗拉强度分别比原来提高30%和25%。     

Cometary Refractory Grains: Interstellar and Nebular Sources

Comets are heterogeneous mixtures of interstellar and nebular materials. The degree of mixing of interstellar sources and nebular sources at different nuclear size scales holds the promise of revealing how cometary particles, cometesimals, and cometary nuclei accreted. We can ascribe cometary materials to interstellar and nebular sources and see how comets probe planet-forming process in our protoplanetary disk. Comets and cometary IDPs contain carbonaceous matter that appears to be either similar to poorly-graphitized (amorphous) carbon, a likely ISM source, or highly labile complex organics, with possible ISM or outer disk heritage. The oxygen fugacity of the solar nebula depends on the dynamical interplay between the inward migration of carbon-rich grains and of icy (water-rich) grains. Inside the water dissociation line, OH^? reacts with carbon to form CO or CO₂, consuming available oxygen and contributing to the canonical low oxygen fugacity. Alternatively, the influx of water vapor and/or oxygen rich dust grains from outer (cooler) disk regions can raise the oxygen fugacity. Low oxygen fugacity of the canonical solar nebula favors the condensation of Mg-rich crystalline silicates and Fe-metal, or the annealing of Fe-Mg amorphous silicates into Mg-rich crystals and Fe-metal via Fe-reduction. High oxygen fugacity nebular conditions favors the condensation of Fe-bearing to Fe-rich crystalline silicates. In the ISM, Fe-Mg amorphous silicates are prevalent, in stark contrast to Mg-rich crystalline silicates that are rare. Hence, cometary Mg-rich crystalline silicates formed in the hot, inner regions of the canonical solar nebula and they are the touchstone for models of the outward radial transport of nebular grains to the comet-forming zone. Stardust samples are dominated by Mg-rich crystalline silicates but also contain abundant Fe-bearing and Fe-rich crystalline silicates that are too large (?0.1 μm) to be annealed Fe-Mg amorphous silicates. By comparison with asteroids, the Stardust Fe-bearing and Fe-rich crystalline silicates suggests partial aqueous alteration in comet nuclei. However, aqueous alteration transforms Fe-rich olivine to phyllosilicates before Mg-rich olivine, and Stardust has Mg-rich and Fe-rich olivine and no phyllosilicates. Hence, we look to a nebular source for the moderately Fe-rich to nearly pure-Fe crystalline silicates. Primitive matrices have Mg-Fe silicates but no phyllosilicates, supporting the idea that Mg-Fe silicates but not phyllosilicates are products of water-rich shocks. Chondrule-formation is a late stage process in our protoplanetary disk. Stardust samples show comet 81P/Wild 2 formed at least as late to incorporate a few chondrules, requiring radial transport of chondrules out to perhaps >20 AU. By similar radial transport mechanisms, collisional fragments of aqueously altered asteroids, in particular achondrites that formed earlier than chondrules, might reach the comet-forming zones. However, Stardust samples do not have phyllosilicates and chondrules are rare. Hence, the nebular refractory grains in comet 81P/Wild 2, as well as other comets, appear to be pre-accretionary with respect to asteroid parent bodies. By discussing nebular pathways for the formation of Fe-rich crystalline silicates, and also phyllosilicates and carbonates, we put forth the view that comets contain both the interstellar ingredients for and the products of nebular transmutation.     

Ion Irradiation and the Origin of Cometary Materials

For about 20 years laboratory research has been carried out on the effects induced by energetic ions on materials (ices, silicates, carbons) of cometary relevance. Here I present some recent results and outline the relevance such laboratory investigations might have for understanding the origin of cometary materials. This revised version was published online in June 2006 with corrections to the Cover Date.     

Crystalline Silicates

One of the big surprises of the Infrared Space Observatory (ISO) has been discovery of crystalline silicates outside our own Solar system. It was generally assumed before that all cosmic silicates in space were of amorphous structure. Thanks to ISO we know now that crystalline silicates are ubiquitous in the Galaxy (except for the diffuse ISM) and sometimes even in very large quantities (> 50% of the small dust particles). The evolution of the crystalline silicates is still not completely clarified, but the combination of theoretical modeling and observations have already shed light on their life-cycle. The absence of crystalline silicates in the diffuse ISM provides us with information about the dust amorphization rate in the ISM.     

离子注入改善电接触微动磨损研究

以AgCu10合金为对象, 研究和探讨了离子注入提高电接触材料的抗氧化和抗磨损性能并改善电接触微动磨损的技术. 试验结果表明,离子注入后的AgCu10合金大大减少了磨损颗粒的产生,降低了磨损过程中产生的金属转移, 减轻了磨损颗粒的氧化污染, 从而提高合金表面耐磨损和抗腐蚀性能, 改善电接触微动磨损性能.     

钇对Ti-Ti5Si3共晶合金微观组织和力学性能的影响

研究了稀土元素钇（Y）对Ti-Ti5Si3共晶合金的微合金化作用。微观组织分析表明,添加微量Y,可以改变原始钛硅合金的共晶团形态和组织形貌。适量Y的加入（原子比0．025％）,不仅使共晶团中粗大的Ti5Si3相颗粒明显细化和钝化,而且合金的微观组织也更加均匀。合金的室温压缩塑性和强度也得到了有效提高。稀土元素Y对钛硅合金的作用,很可能是因为Y原子替代了Ti5Si3相中的部分Si原子,形成硅化物Ti5（Si,Y）3所致。     

Presolar Grains in Meteorites and Their Compositions

Small amounts of pre-solar “stardust” grains have survived in the matrices of primitive meteorites and interplanetary dust particles. These grains—formed directly in the outflows of or from the ejecta of stars—include thermally and chemically refractory carbon materials such as diamond, graphite and silicon carbide; as well as refractory oxides and nitrides. Pre-solar silicates, which have only recently been identified, are the most abundant type except for possibly diamond. The detailed study with modern analytical tools, of isotopic signatures in particular, provides highly accurate and detailed information with regard to stellar nucleosynthesis and grain formation in stellar atmospheres. Important stellar sources are Red Giant (RG) and Asymptotic Giant Branch (AGB) stars, with supernova contributions apparently small. The survival of those grains puts constraints on conditions they were exposed to in the interstellar medium and in the early solar system.     

The Silicate Material in Comets

Silicates in comets appear to be a mix of high-temperature crystalline enstatite and forsterite plus glassy or amorphous grains that formed at lower temperatures. The mineral identifications from the 10 and 20 μm cometary spectra are consistent with the composition of anhydrous chondritic aggregate IDPs. The origin of the cometary silicates remains puzzling. While the evidence from the IDPs points to a pre-solar origin of both crystalline and glassy components, the signatures of crystalline silicates appear in the spectra of young stellar objects only at a late evolutionary stage, when comets are the likely source of the dust. This revised version was published online in June 2006 with corrections to the Cover Date.     

稀土Y对低膨胀高温合金显微组织和界面的影响

运用分析电子显微术、高分辨电子显微术、化学相分析和 X-射线衍射等方法分析研究了Fe-Ni-Co-Nb-Ti-Si低膨胀高温合金的相组成和相结构 ,以及稀土对合金的组织和性能的影响规律。结果显示 ,微量的稀土主要存在于合金的片状相中 ,并使其晶体结构发生变化。加入适量的稀土 Y后 ,合金片状相变得更加细密、均匀。和不含稀土的低膨胀高温合金相比 ,含 Y的低膨胀高温合金中片状相与基体的晶格错配由 0 .7%下降到 0 .0 7% ,表明界面应力明显下降     

The origin of tektites

The tektites called Muong Nong type by V. Barnes apparently represent the parent material from which other types are derived. In these tektites are found clues (coesite, angular voids) which indicate that they have not been substantially remelted since the event which detached them from the planet or satellite on which they were formed.From the nickel-iron spherules and the coesite it is deduced that the tektites were detached by meteorite impact. From the absence of cosmogenic isotopes and the distribution over the earth it is deduced that the source was either the earth or the moon. Calculations of rates of diffusion in silicates indicate that tektites could not have been produced from terrestrial sedimentary rocks; it has long been remarked that they are different from terrestrial igneous rocks. A lunar origin is therefore considered likely, in agreement with aerodynamic evidence. Contrary indications from the geochemical likeness of tektites to terrestrial materials, especially at the Ries Kessel and the Bosumtwi crater are noted, but these indications are considered to be outweighed by the difficulties of giving a physical account of a terrestrial origin.Interpreted as lunar materials, the tektites suggest that large portions of the lunar surface are covered with ash-flow tuff of a peculiar type, remarkably free of water and other volatiles. They also give evidence concerning the origin of the moon.