流量定位喷注器的静态与瞬态特性

本文分析了流量定位喷注器的工作原理及静态与瞬态特性,给出了实现等压降工作特性的基本准则.     

缘板及叶冠间的接触状况及其对叶片位移和应力的影响

1.计算方法及其实验验证 本文用分析法见文献[1],这里以WS9高压二级涡轮转子叶片(简称WS9叶片)为例来说明方法的特点。该转子轮盘上均匀安装110片叶片,组成具有循环对称接触结构的叶片环,有接触表面的循环对称结构。据此,可将图1所示的一片叶片取作基本段分析,但同时必须在该叶片一般有限元刚度方程中引入缘板及叶冠的循环对称接触表面(叶冠的A1侧面与A2侧面,以及缘板的B1侧面与B2侧面)处的循环对称接触     

一种新型的张力控制系统的研究

介绍一种以工控机为核心、交流数字伺服电机为执行元件、采用半径跟随臂实时反馈纱团半径值的新型张力控制系统，并具体介绍了张力控制系统的硬件、软件设计、数学模型的建立等。实际应用证明系统达到了要求的指标。     

复合材料板壳在过屈曲下最佳铺层设计的工程方法

 本文基于相同边界条件下铺层构成对失稳后的变形形态影响不大的基本假设,根据理论和实践经验得到的准最佳铺层失稳后的位移场为基础,给出了确定最佳铺层参数的工程方法。计算表明,其基本假设和解题思路是正确的。由于本方法最后归结为解一个一元三次方程,使计算大为简化,可降低设计成本和周期,在工程设计中具有实际意义。     

弯管模胎图形库管理系统的设计与实现

详细阐述了弯管模胎图形库的设计方案,并介绍了图形库的实现方式.最后通过实例阐明了系统在弯管模胎图形库管理中的具体应用.     

用能量法计算涡轮盘偏心孔边局部应力

为在弹塑性状态下计算孔边局部应力,本文基于能量法则,推导出计算孔边局部应力的方法。本文的方法简单实用,准确度较修正诺伯法计算结果要高,文中附有涡轮盘偏心孔的计算实例,并对计算结果进行了分析。     

粘性不可压缩流动三维复杂流场分块耦合求解

提出了一个粘性不可压缩流动三维复杂流场的分块耦合求解方法。可解决科学和工程计算中的各种稳态和瞬态粘性不可压缩流动计算问题。     

液氮纯度分析的偏差及修正

液氮纯度是液氮产品非常关键的一个技术指标.液氮纯度的在线跟踪测量是通过测量液氮中的氧含量来实现的.在多年来的液氮在线分析及液氮出库分析过程中,发现氧含量测量结果普遍偏低.本文通过理论分析及大量的实验数据,找到了数据产生偏差的原因,并给出了科学的修正办法,为以后液氮生产过程中更加有效地控制产品质量打下了基础.     

制备工艺对金刚石形核质量的影响

研究了制备工艺对微波等离子体ＣＶＤ金刚石成膜质量的影响。详细讨论了基片在等离子体中的位置、基片台结构、Ｎ２等离子体预处理及启动条件对金刚石成膜均匀性的影响。提出了能获得均匀金刚石膜的制备工艺程序。     

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.