高职专业建设探索

作为一种新的教学类型，高等职业教育的专业建设对于培养适应市场需求的技术应用性人才犹为重要。本分析了现行专业建设中存在的问题，提出了如何结合高职教育特点改革高职专业建设的设想。     

高性能的标准单元库设计

从仿真和流片两个方面对标准单元库的验证方法进行了研究.在仿真方面,提出了采用静态时序分析工具和SPICE仿真工具对单元的估算值和仿真结果进行比较分析的方法来验证,同时还给出了具体的操作步骤实例.在流片验证中,提出了一种非常有效的电路结构.这种电路结构不但能够准确验证时序,还能极大地减少PAD数量;最重要的特点是:该电路能够完全避免PAD和非被测单元的引入带来的额外延迟,从而得到准确的被测单元延迟.     

叉流管－管型换热器二维温度场的数值分析

建立并导出叉流管－管型换热器传热过程的二维数学模型及相应的差分格式，对比实验数据和性能计算结果，表明数值方法是有效可行的。据此编制的计算机程序已成功地用于组合发动机空气预冷换热器工作过程的预测。     

混杂纤维复合材料吸湿行为研究

 本文采用80℃水浸的方法,研究了不同类型混杂复合材料层压板的吸湿行为,找到描述混杂复合材料吸湿规律方程。同时,从理论上对混杂复合材料的平衡吸湿量及湿扩散系数进行了分析,建立了数学表达式,理论与实验较好吻合。     

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。     

Simulation and Analysis of Crashworthiness of Fuel Tank for Helicopters

Crashworthiness requirement of fuel tanks is one of the important requirements in helicopter designs. The relations among the protection frame, textile layer and rubber layer of the fuel tank are introduced. Two appropriate FE models are established, one is for an uncovered helicopter fuel tank without protection frame, and the other is for fuel tank with protection frame. The dynamic responses of the two types of fuel tanks impinging on the ground with velocities of 17.3 m/s are numerically simulated for the purpose of analyzing energy-absorbing capabilities of the textile layer and protection frame. The feasibility of the current crashworthiness design of the fuel tank is examined though comparing the dynamic response behaviors of the two fuel tanks.     

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.     

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.     

产生标准失真源的方法

介绍了失真的测量原理和产生标准失真源的方法；介绍了失真度测量仪自动测试系统，并对测量装置的误差进行了分析。     

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.