一个新的蠕变寿命估算公式的推出

本文从一些经典公式出发,推导出新的寿命公式。另外,通过引入蠕变损伤特征参量的概念还导出类似的另一个蠕变寿命估算公式。所推导出两个公式在16MnR材料中得到较为成功的应用。     

一种用于材料高温蠕变分析的统一粘塑性损伤本构模型

通过应变等效假设在本文提出的具有过应力特征的统一粘塑性本构模型［５］中引入了描述材料损伤的内变量。并且给出了一个基于组合功密度概念的新的损伤模型。同以往的唯象模型相比，该损伤模型具有较明确的细观物理意义，能反映应变率和应力状态对损伤演化发展的影响。     

CFRP层板的落重冲击分层损伤研究

采用落重冲击试验方法研究了航空上常用的铺层形式为［Ｏ２／９Ｏ２／４５２／－４５２］ｓ的先进复合材料（ＣＦＲＰ）低能冲击损伤问题。重点讨论了落重冲击后分层损伤形貌、冲击能量Ｗ与分层面积Ａ之间的关系以及基体韧性对ＣＦＲＰ抗冲击性能影响。     

固体火箭发动机寿命预估的一种考虑

利用弹性－粘弹性对应原理，分析长期贮存固体推进剂药柱由环境温度变化引起的热应力，计算药柱损伤，并对发动机寿命进行预估。理论分析和算法具有普遍性，可供工程设计参考。     

一个简易实用的疲劳损伤累积法则

1.法则的提出 利用材料的等幅疲劳试验数据进行承受变幅荷载的实际构件的疲劳设计,必须借助疲劳损伤累积理论。40年代以来,人们一直试图寻找一种较好的疲劳损伤累积理论。表1列举了其中的一些典型代表。     

单晶高温合金接近使用条件下的寿命估算与损伤分析

针对发动机热端部件承受的典型载荷谱，发展了一种通用的寿命预测方程和损伤分析方法。这个方法是在疲劳蠕变交互作用断裂特征图及其最大应力修正的寿命方程基础上建立的。根据ＤＤ３单晶合金的疲劳蠕变交互作用断裂特征图及其最大应力修正的寿命方程，验证了本方法是切实可行的。预测精度是符合要求的。     

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.     

无损检测的内涵演变及其在质量控制中的作用

就无损检测的内涵如何从探伤演变到评价及无损检测在质量控制中的应有作用作了叙述,希望对相关人员开拓思路、提高工作质量有所裨益.     

高能CO2激光腔镜高反介质薄膜的传输特性

为了获得适用于高能CO2激光器的高抗破坏阈值高反薄膜,以10.6μm高反膜ZnSe/YbF3,PbTe/BaF2膜系为例,数值模拟了激光在高反介质膜中的传输的场特性;给出了激光在多层介质膜中的场强分布、温度场分布及热应力分布。结果表明硅镜基体上的PbTe/BaF2膜系所需膜层厚度小、膜层数少,反射率可高达99.98%。     

彩色三维激光快速成型技术的研究

目前逆向工程采用线结构激光和一个彩色面阵CCD摄像机构成三维彩色扫描系统,彩色CCD摄像机分两次对被测物体成像,首先摄取物体的彩色图片,然后加用滤光片再摄取激光光平面上的三维信息.最后将两次获取的信息重叠,便可得到三维彩色信息.提出了激光光平面方程式三维测量方法,建立了相应的数学模型.研制成一套适用于彩色逆向工程流程,并进行了实验研究,给出了实验结果.