多孔氧化锆陶瓷光固化工艺及压缩性能研究

在传统陶瓷成型工艺中,制备具有复杂多孔结构的高性能陶瓷样件向来是一大难点,随着增材制造技术的引入,对于所成型样件结构的限制大大减少,但如何利用增材技术实现多孔样件的稳定制备是关键问题。针对光固化陶瓷增材成型这一制备工艺,进行了成型以及烧结过程工艺参数的研究与优化,结果表明,对于面投影式光固化陶瓷成型适用的曝光时间为5s、成型层厚为30μm、烧结温度为1480℃,利用该参数可成型具有规则多孔单元的氧化锆结构,其显微硬度及致密度分别为13.91GPa以及95%。利用工业CT模型重建,并与理论模型比对,发现多孔样件在宏观尺度上均匀;而利用压缩测试与有限元仿真对照,静态应力分布、弹性阶段动态压缩结果以及断口微观形貌均表明多孔样件在压缩性能上已达到其理论强度。通过光固化成型高性能多孔氧化锆样件,可为航空领域中轻量化设计提供新的选择。     

3D打印用硅基陶瓷前驱体研究进展北大核心CSCD

聚合物前驱体转化法可使用聚合物的成型加工工艺实现陶瓷材料的加工制备,在高性能陶瓷和复合材料制备方面显示出独特的优势。3D打印技术在陶瓷前驱体成型中的应用为制备复杂结构陶瓷制件提供了全新的可能。本文从3D打印硅基陶瓷前驱体树脂体系、打印技术及其应用等方面,系统总结了近年来3D打印制备SiCO、SiCN、SiC及含B、Zr等元素硅基陶瓷材料前驱体的研究进展,并进一步指出了3D打印陶瓷前驱体面临的挑战与研究方向。     

陶瓷零件增材制造技术及在航空航天领域的潜在应用

陶瓷零件因其强度高、密度低、耐高温及耐腐蚀等特点在航空航天领域具有广阔的应用前景。然而,陶瓷零件的传统制造方法存在周期长、成本高、依赖模具且难以制造复杂结构等问题,极大限制了陶瓷零件在航空航天领域的应用。增材制造技术是一种基于"离散-堆积"成型原理、由三维数据驱动直接制造零件的方法。与传统制造方法相比,增材制造技术具有设计自由度高、产品研发周期短、制造成本低等优势,可以无需模具快速制造复杂结构陶瓷零件。在简要阐述增材制造原理和特点的基础上,系统地分析了采用三维打印、激光选区烧结、激光选区熔化、熔融沉积造型、分层实体制造、光固化成型等技术制造陶瓷零件的研究现状及存在的问题。最后,对陶瓷零件增材制造技术在航空航天领域的潜在应用进行了分析与展望。     

增材制造——面向航空航天制造的变革性技术

增材制造技术在航空航天应用方面具有单件小批量的复杂结构快速制造优势,未来将向着设计、材料和成形一体化方向发展。分析了增材制造在航空航天领域应用发展的3个层面,以航空发动机涡轮叶片增材制造、高性能聚醚醚酮（PEEK）及其复合材料、连续纤维增强树脂复合材料及太空3D打印为主题,介绍了增材制造技术国内外以及西安交通大学的研究状况。涡轮叶片应用增材制造工艺可以有效提高效率降低成本,未来向高性能的高温合金和陶瓷基复合材料增材制造技术发展。高性能轻质聚合物PEEK及其复合材料增材制造在高力学性能结构件、吸波功能件的成形中得到应用,将改变现有的设计与材料,推动结构与功能一体化发展。连续纤维复合材料增材制造将带动无模具纤维复合材料成形的新发展,在太空3D打印将改变未来航空航天制造模式。增材制造技术将给航空航天制造技术带来变革性发展。     

先进陶瓷黏结剂喷射增材制造技术发展与展望

在过去的20年中,陶瓷黏结剂喷射增材制造技术已经成为制造复杂陶瓷构件的一种革命性方法,特别是在航空航天、生物医疗、电子信息等多个关键领域展现出显著的应用潜力与价值。本文全面回顾了此技术的基础原理、材料选择、工艺流程、性能特征及制造缺陷,并针对未来的挑战和目标进行了深入展望。文中首先详细概述了该技术的成型原理,对其与其他增材制造工艺的优势和局限进行了对比分析;然后综合总结了国际研究进展,重点包括陶瓷粉末的性能与处理、黏结剂的配置与其在粉床中的动力学行为、工艺参数的调整与后续致密化工艺,并讨论了这些因素如何影响初坯和最终制件的密度、孔隙结构、组织特性及性能;最后,基于现有研究成果和应用局限,本文对粉末原材料、黏结剂的设计、工艺参数优化等方面提出了前瞻性的发展建议。本篇综述旨在为理解和应用陶瓷黏结剂喷射增材制造提供全面的科学研究和工程实践指导。     

航空发动机叶片用陶瓷型芯的光固化增材制造研究现状

随着对高推重比和高效率航空发动机日益增长的需求,发动机叶片正朝着复杂空心结构的方向发展,而这对高性能复杂结构的陶瓷型芯提出了更高的要求.与此同时,基于光固化原理的增材制造技术可以实现无模具条件下的高精度、快速以及综合性能优异的陶瓷型芯制备.然而,目前基于光固化增材制造的陶瓷型芯制备工艺依旧面临控制尺寸精度、优化脱脂烧结...     

金属材料增材制造技术在直升机中的应用发展研究

本文分析了金属材料增材制造技术的发展现状,包括金属材料增材制造工艺的分类及特点、原材料、主要设备供应商和研发方向、增材制造工件所需的主要后处理方法;回顾了增材制造技术在直升机中的应用现状,提出增材制造技术尚未用于制造直升机机体承力部件的主要原因（存在疲劳强度较低、成形精度较差、成本较高等问题）;展望金属增材制造在直升机结构拓扑优化设计、结构整体化设计、结构功能一体化设计及维护保障中的应用前景;提出增材制造技术在直升机应用的三个阶段。     

耐高温陶瓷基结构吸波复合材料研究进展

陶瓷基结构吸波复合材料具有耐高温、耐腐蚀、抗氧化等诸多优点,是解决武器装备热端隐身问题的关键材料,具有重要应用前景和战略意义。本文介绍了陶瓷吸波材料的微观-宏观多级设计方法,综述了掺杂改性碳化硅陶瓷、钡铁氧体陶瓷、聚合物转化陶瓷(PDCs)、3D打印多孔陶瓷及陶瓷蜂窝、连续纤维增强陶瓷基复合材料(CFCMC)等新型陶瓷基复合材料的最新研究进展,展望了结构吸波一体化的陶瓷基复合材料的发展趋势,提出微观-宏观多级结构设计的纤维增强陶瓷基复合材料将是未来高温隐身材料领域的重要发展方向。     

增材制造技术在液体火箭发动机领域的最新进展及产业化推进

介绍了航天领域液体火箭发动机的工作环境与制造特点，分析增材制造技术原理与在其制造领域存在的优势，综述分析了国内外航天增材制造技术应用最新情况；结合液体火箭发动机工程应用实例，对增材制造工程应用发展所经历的替代传统工艺、集成制造、轻量化制造和系统集成设计四个阶段的工程应用与效果进行了系统分析；并指出目前航天液体动力增材制造技术工程化应用推进过程存在的问题及解决方案，提出了增材制造产业化的发展建议。     

脉冲微孔喷射技术及其在增材制造方面的应用

介绍了用于制造单分散球形微米级粒子的脉冲微孔喷射技术.根据微滴制备原理,可将其分为适用于低熔点材料的压片式喷射装置及适用于高熔点材料的传动杆式喷射装置,分别阐述了两种方式的脉冲微孔喷射技术的喷射原理、相关特点以及该技术的发展和研究现状.目前,采用脉冲微孔喷射技术已成功制备出金属、半导体及生体材料单分散微粒子,具有粒径均一、圆球度高等优势.通过与其他微米级粒子制备技术,如均匀液滴喷射法、气动式按需喷射法及雾化法相比较,在诸多方面显示出脉冲微孔喷射法的独特优点.与此同时,分别讨论了脉冲微孔喷射技术在增材制造方面的潜在应用,可直接使用微米级粒子作为增材制造用粉体以及液滴沉积成型.鉴于脉冲微孔喷射技术的独特性,可以预见随着研究的不断深入,脉冲微孔喷射技术将在增材制造方面具有更加广阔的发展空间和应用前景.     

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.