原位生成Si2N2O与β-Si3N4晶种协同增韧Si3N4复相陶瓷研究

采用原位生成Si2N2O与添加β-Si3N4晶种的方法协同增韧,利用凝胶注模成型、无压烧结制备了Si3N4复相陶瓷材料,研究了协同增韧对材料力学性能和显微结构的影响.结果表明:通过添加5%(质量分数)的SiO2原位生成Si2N2O使材料的弯曲强度和断裂韧度有明显提高,分别达到359.8 MPa和4.67 MPa·m1/2,通过添加5%质量分数的β-Si3N4晶种,得到的Si3N4复相陶瓷材料中柱状β-Si3N4相生长完好、均匀分布,与板状Si2N2O结合良好.综合以上两种增韧机制使材料的力学性能进一步提高,弯曲强度为486.7 MPa,断裂韧度达到6.38 MPa·m1/2.     

三维网络碳化硅多孔陶瓷的制备

以中间相沥青添加55%(质量分数,下同)的Si粉混合物为原料,制备了含Si的炭泡沫模板。在高温反应烧结炉中,氩气气氛下1500℃保温1～6h,结合反应烧结工艺制备了碳化硅多孔陶瓷。利用扫描电子显微镜(SEM)和X射线衍射分析仪(XRD)对碳化硅多孔陶瓷的微观形貌、物相组成进行了观察,并对熔融Si与C的反应机理进行了探讨。结果表明:碳化硅多孔陶瓷的微观结构与炭泡沫模板的微观结构一致,烧结温度1500℃下,随着保温时间的延长,多孔陶瓷的弯曲强度先增大后减小,而孔隙率先减小后增大;在保温4h的条件下制备的碳化硅多孔陶瓷主要由β-SiC相组成,最大弯曲强度为26.2MPa,对应的孔隙率为45%。内部熔融的Si与外部熔融的Si同时与C反应生成SiC,最后两者结合在一起形成致密的SiC多孔陶瓷。     

微波烧结制备MoSi2 及SiC/ MoSi2 纳米复合陶瓷

采用微波烧结法制备了MoSi2和10vol%SiC/MoSi2纳米复合陶瓷。通过SiC预加热体的混合式加热法和合理的保温结构设计,实现了MoSi2低温阶段的快速升温,提高了温度均匀性。密度和力学性能测试结果表明,1 450℃保温60 min烧结工艺下,MoSi2试样的相对密度达到93.4%,断裂韧度4.5 MPa.m1/2,维氏硬度为10.53 GPa,弯曲强度为186 MPa。10vol%SiC/MoSi2试样尽管相对密度下降为90.3%,但各项力学性能均优于MoSi2试样。相比1 650℃热压烧结,微波烧结温度降低了200℃,MoSi2和SiC/MoSi2试样致密性有所下降,但力学性能有较大提高,尤其是MoSi2试样。断口扫描分析表明,微波烧结试样相对热压烧结试样基体晶粒更细,孔隙细小且分布均匀;SiC/MoSi2试样微波烧结的晶粒细化效果不如MoSi2明显。     

3Y-ZrO2／Al2O3细晶复相陶瓷涡轮盘的超塑挤压

以高纯氧化铝(Al2O3)和氧化锆(3Y-ZrO2)粉末为原料,在1450℃下通过真空热压烧结制备3Y-ZrO2/Al2O3细晶复相陶瓷致密块料,随后在1500~1650℃温度范围内进行涡轮盘模拟件的超塑挤压。结果显示,3Y-ZrO2/Al2O3陶瓷在1600℃具有最佳挤压性能,最大单位挤压力小于25MPa,最大压头速率达到0.14mm.min-1,成形件质量良好,无明显缺陷。与变形前相比,尽管材料晶粒明显粗化,但是致密度有很大提高,断口SEM显示主要以穿晶断裂方式为主,所以成形件的弯曲强度、断裂韧度和维氏硬度并没有出现大的变化,甚至盘片部位还有所提高,分别由变形前的573MPa,7.1MPa.m1/2和17.7GPa提高到617MPa,8.1 MPa.m1/2和18.8GPa。     

SPS烧结温度对ZrB_2-SiC复合陶瓷性能的影响

以放电等离子烧结法(spark plasma sintering,SPS)分别在1700℃和1900℃烧结制备Zr B2-20%Si C(ZS)复合陶瓷(分别简称为ZS1700和ZS1900),通过分析两种陶瓷的SEM、EDS、硬度、断裂韧度、高温弯曲强度、氧化增重和氧化截面等,研究烧结温度对ZS复合陶瓷微观结构、力学性能和抗氧化性能的影响。结果表明:烧结温度由1700℃提升至1900℃,ZS陶瓷晶粒长大,致密度由98%提高至99.8%,硬度由12.6 GPa提高至14.7 GPa;1600℃弯曲强度由101 MPa提高至286 MPa,1800℃弯曲强度由138 MPa提高至302 MPa,高温弯曲强度显著提高;与ZS1700相比,ZS1900在1500℃空气中的氧化深度小,基体中氧渗入量较少,抗氧化性能有一定提升。     

放电等离子烧结Al2O3-ZrO2纳米复相陶瓷及其力学性能

采用醇 水溶液加热法制备两相分散良好的纳米复合粉体,通过放电等离子超快速烧结制备Al2O3 ZrO2纳米复相陶瓷。研究了纳米第二相ZrO2对复相陶瓷致密化、烧结行为、力学性能以及微观结构的影响。从烧结激活能的观点解释了纳米第二相阻止基体Al2O3致密化的原因。放电等离子烧结得到了典型的晶间/晶内混合型纳米陶瓷,其弯曲强度高达1070MPa,断裂韧性达10.42MPa·m1/2。微观组织分析表明其中大量的内晶纳米颗粒阻止位错运动,使得基体氧化铝晶粒内形成复杂的位错组态,其主要特点为穿晶断裂和多重界面。     

高致密反应烧结SiC_f/SiC复合材料的微观结构与性能

SiC_f/SiC陶瓷基复合材料是航空发动机热结构部件的关键材料。基于国产KD-II碳化硅纤维,利用反应熔渗工艺制备了高致密的SiC_f/SiC复合材料,研究了其微观结构、常温/高温力学性能、热物理性能和高温长时氧化稳定性。反应熔渗制备的SiC_f/SiC显气孔率仅为1.6%,室温弯曲强度为(521±89)MPa,1200℃高温弯曲强度为(576±22)MPa,呈非脆性断裂特征,具有优异的高温力学稳定性。厚度方向常温热导率高达41.7W/(m·K),1300℃热导率为18.9W/(m·K)。SiC_f/SiC复合材料经1200℃氧化1000h仍保持非脆性断裂特征,弯曲强度为(360±54)MPa,仅下降19%,仍保持非脆性断裂特征。反应烧结制备的SiC_f/SiC复合材料具备优异的耐高温抗氧化性能,有望满足航空发动机热端部件对SiC_f/SiC陶瓷基复合材料的应用需求。     

2D-Cf/SiC复合材料及构件的无压成型工艺

采用无压成型工艺制备了2D-Cf/SiC及复杂构件。结果表明:复合材料弯曲强度达到328MPa,断裂韧度达到14.9MPa·m1/2,层间剪切强度达到35.9MPa,同时材料也具有很好的高温抗氧化性能。利用本工艺制备了某型号发动机的尾喷管,并成功通过了应用部门的试车考核。     

PIP工艺制备SiC晶须增强SiCf/SiC复合材料的性能

以不同界面层厚度的SiC纤维为增强相,采用先驱体浸渍裂解工艺(PIP)制备SiC_f(PyC)/SiC复合材料,并在复合材料基体中引入SiC晶须,对其性能进行研究。结果表明:热解碳(PyC)界面层厚度约为230 nm时,SiC纤维拔出明显,SiC_f/SiC复合材料拉伸强度、弯曲强度和断裂韧度分别达到192.3 MPa、446.9 MPa和11.4 MPa?m^1/2;在SiC_f/SiC复合材料基体中引入SiC晶须后,晶须的拔出、桥连及裂纹偏转等增韧机制增加了裂纹在基体中传递时的能量消耗,使复合材料的断裂韧度和弯曲强度分别提高了22.9%和9.1%。     

烧结温度对氧化铝基陶瓷型壳显微组织及力学行为的影响

采用选择性激光烧结(selective laser sintering,SLS)快速制备高温合金叶片用氧化铝基陶瓷型壳初坯,并结合高温烧结(high-temperature sintering)进一步提高陶瓷型壳的力学性能。研究不同烧结温度(1450～1600℃)对氧化铝基陶瓷型壳的抗弯强度的影响,采用X射线衍射仪(XRD)、扫描电子显微镜(SEM)分析型壳的物相组成、断口微观形貌。结果表明:采用选择性激光烧结+高温烧结技术可快速高效地制备力学性能满足要求的陶瓷型壳,随着烧结温度从1450℃升高到1600℃,型壳的室温平均抗弯强度增大,并在1600℃时达到38.03 MPa;型壳的主要强化相为柱状莫来石相,且随烧结温度升高,型壳中莫来石相含量增加,石英相含量降低,方石英相含量先增加后有所降低;裂纹扩展形式从缓慢扩展转变为迅速扩展并引发瞬断,断口由撕裂状演变为平齐小断面,断裂方式由主要沿晶断裂向穿晶断裂转变,裂纹倾向于向晶内莫来石扩展。     

捷变频磁控管用高频直线振荡电机设计

捷变频磁控管的快速捷变特性取决于驱动电机的性能,要求电机功耗小、体积小、效率高,能实现高频稳幅直线振动.文章介绍了音圈直线电机、电磁开关式直线电机和电磁混合式直线电机等三种方案,通过对其工作原理和性能特点分析,确定了音圈直线电机驱动方案,进行了电磁场仿真分析和电磁参数设计,进行了样机试验测试.结果表明,设计的音圈直线电...     

桨叶实度及轴间距对摆线桨气动特性影响研究

悬停状态下,设计参数和摆线桨间距离对摆线桨的气动特性有较大影响。首先通过算例验证滑移网格计算方法应用于摆线桨悬停状态下气动力计算的准确性,然后研究摆线桨在不同半径、弦长和桨叶数时的气动参数特性,最后计算分析不同距离时,摆线桨间的气动干扰特性。结果表明:随着半径增大,桨叶气动力和单位面积上载荷均增大;弦长越大,气动力越大,桨叶单位面积上载荷反而越小;4叶片摆线桨产生的气动力比3叶片和6叶片大,而3叶片的桨叶载荷最大;合力偏转角分别随转速和实度的增大而减小;随着摆线桨间距离的增加,气动力损失系数和合力偏转角均减小。     

A new target tracking filter based on deep learning

At present, current filters can basically solve the filtering problem in target tracking, but there are still many problems such as too many filtering variants, too many filtering forms, loosely coupled with the target motion model, and so on. To solve the above problems, we carry out crossapplication research of artificial intelligence theory and methods in the field of tracking filters. We firstly analyze the computation graphs of typical a-β and Kalman. Through analysis, it is concluded that ...     

Investigations of entrainment characteristics and shear-layer vortices evolution in an axisymmetric rear variable area bypass injector

In this study,firstly,for the axisymmetric RVABI,the change-rule of adverse pressure gradient caused by radial velocity during the transition of internal flow mode in variable geometry is summarized,and a Bypass Ratio(BR) iterative algorithm based on the empirical correlation of non-equilibrium pressure is proposed.The algorithm can estimate the nonlinear relationship between area ratio and BR,with an error range falling below 6.5%.Then,we discuss the favorable effect of uniform mixing on the th...     

PVC糊树脂对交联PVC泡沫塑料的影响

通过水煮发泡制备交联聚氯乙烯泡沫塑料,讨论了聚氯乙烯(PVC)糊树脂对泡沫制备过程中经制糊、模压和发泡工艺得到的产物的影响,研究了PVC糊树脂对制备的交联PVC泡沫压缩性能的影响.结果表明:制备交联聚氯乙烯泡沫塑料适宜的糊黏度是4～9 Pa·s;PVC糊树脂的K值较大或水萃取液pH值呈碱性可有效防止模压过程中PVC的降解;PVC糊树脂的水萃取液pH值呈碱性可催化发泡反应,有利于得到低密度泡沫且缩短发泡时间;随着其K值增加,制备的泡沫压缩强度增大,但是K值过大时,制备的泡沫泡孔较大,压缩强度反而降低,适宜的K值为70～80.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

Multiframe weak target track-before-detect based on pseudo-spectrum in mixed coordinates

Traditional multiframe Track-Before-Detect(TBD) may incur adverse integration loss resulting from model mismatch in sensor coordinates. Its suboptimal integration strategy may cause target envelope degradation. To address these issues, a pseudo-spectrum-based multiframe TBD in mixed coordinates is proposed firstly. The data search for energy integration is conducted based on an accurate model in the x-y plane while target energy is integrated based on pseudo-spectrum in sensor coordinates. The a...     

Deep Impact: Working Properties for the Target Nucleus – Comet 9P/Tempel 1

In 1998, Comet 9P/Tempel 1 was chosen as the target of the Deep Impact mission (A’Hearn, M. F., Belton, M. J. S., and Delamere, A., Space Sci. Rev., 2005) even though very little was known about its physical properties. Efforts were immediately begun to improve this situation by the Deep Impact Science Team leading to the founding of a worldwide observing campaign (Meech et al., Space Sci. Rev., 2005a). This campaign has already produced a great deal of information on the global properties of the comet’s nucleus (summarized in Table I) that is vital to the planning and the assessment of the chances of success at the impact and encounter. Since the mission was begun the successful encounters of the Deep Space 1 spacecraft at Comet 19P/Borrelly and the Stardust spacecraft at Comet 81P/Wild 2 have occurred yielding new information on the state of the nuclei of these two comets. This information, together with earlier results on the nucleus of comet 1P/Halley from the European Space Agency’s Giotto, the Soviet Vega mission, and various ground-based observational and theoretical studies, is used as a basis for conjectures on the morphological, geological, mechanical, and compositional properties of the surface and subsurface that Deep Impact may find at 9P/Tempel 1. We adopt the following working values (circa December 2004) for the nucleus parameters of prime importance to Deep Impact as follows: mean effective radius = 3.25± 0.2 km, shape – irregular triaxial ellipsoid with a/b = 3.2± 0.4 and overall dimensions of ∼14.4 × 4.4 × 4.4 km, principal axis rotation with period = 41.85± 0.1 hr, pole directions (RA, Dec, J2000) = 46± 10, 73± 10 deg (Pole 1) or 287± 14, 16.5± 10 deg (Pole 2) (the two poles are photometrically, but not geometrically, equivalent), Kron-Cousins (V-R) color = 0.56± 0.02, V-band geometric albedo = 0.04± 0.01, R-band geometric albedo = 0.05± 0.01, R-band H(1,1,0) = 14.441± 0.067, and mass ∼7×10¹³ kg assuming a bulk density of 500 kg m⁻³. As these are working values, {i.e.}, based on preliminary analyses, it is expected that adjustments to their values may be made before encounter as improved estimates become available through further analysis of the large database being made available by the Deep Impact observing campaign. Given the parameters listed above the impact will occur in an environment where the local gravity is estimated at 0.027–0.04 cm s⁻² and the escape velocity between 1.4 and 2 m s⁻¹. For both of the rotation poles found here, the Deep Impact spacecraft on approach to encounter will find the rotation axis close to the plane of the sky (aspect angles 82.2 and 69.7 deg. for pole 1 and 2, respectively). However, until the rotation period estimate is substantially improved, it will remain uncertain whether the impactor will collide with the broadside or the ends of the nucleus.     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.