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复合材料板壳在过屈曲下最佳铺层设计的工程方法 总被引:1,自引:0,他引:1
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。 相似文献
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S. M. Krimigis D. G. Mitchell D. C. Hamilton S. Livi J. Dandouras S. Jaskulek T. P. Armstrong J. D. Boldt A. F. Cheng G. Gloeckler J. R. Hayes K. C. Hsieh W.-H. Ip E. P. Keath E. Kirsch N. Krupp L. J. Lanzerotti R. Lundgren B. H. Mauk R. W. McEntire E. C. Roelof C. E. Schlemm B. E. Tossman B. Wilken D. J. Williams 《Space Science Reviews》2004,114(1-4):233-329
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. 相似文献
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基于VXI总线和虚拟仪器技术,研制开发了用于外场的模拟式电子控制器检测软件,并对软件开发的过程和要求进行了分析,重点解决了程序设计中的需求分析和模块化设计问题。 相似文献
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研究了一种应用于机载火控系统的具有自学习功能的故障诊断系统.首先介绍了系统的总体结构;然后通过分析火控系统的结构建立了层次诊断模型,并通过示例对诊断系统中知识的表达方法、推理方法等问题做了详细的分析;最后详细描述了系统的自学习机制.应用具有自学习功能的故障诊断专家系统,可实现综合化机载火控系统的智能故障诊断. 相似文献
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GH4169合金疲劳裂纹扩展性能的试验研究 总被引:1,自引:0,他引:1
本研究中对GH4169高温合金的疲劳裂纹扩展性能进行了试验研究。主要进行了400℃~600℃范围内的疲劳裂纹扩展试验.其中对GH4169环形锻件进行了室温下的疲劳裂纹扩展试验。结果表明,在400℃-600℃范围内,温度对GH4169高温合金疲劳裂纹扩展性能的影响很小,随温度上升,裂纹扩展速率稍有加快;优质成分对GH4169高温合金的疲劳裂纹扩展性能几乎没有影响,在相同温度下,YZGH4169与GH4169的疲劳裂纹扩展速率几乎一样;材料品种对YSGH4169高温合金的疲劳裂纹扩展性能有一定影响,YSGH4169锻件比棒材的疲劳裂纹扩展性能要好一些。 相似文献
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关于确立CAD软件绘制标准化工程图地位的探讨 总被引:1,自引:0,他引:1
工程图样作为工程技术信息交流的必要手段,在工程设计与制造中起到举足轻重的作用,而繁琐的手工绘图又一直困扰着工程技术人员,计算机辅助绘图为解决这一问题提供了有利手段。但是工程图样既然作为交流文件,它的图形、标记以及表达形式都要严格执行《机械制图国家标准》。而目前CAD绘图软件中普遍缺少处理机械图样标准化功能的现象,必然要直接影响绘制工程图的质量和速度。本文的目的在于研究CAD软件的绘图功能与我国工程 相似文献
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Chung-Chieh Cheng 《Space Science Reviews》1972,13(1):3-123
The purpose of this work is to study the various -ray-production mechanisms in solar flares and to calculate the flux, the spectrum, and the decay curves of radiation. Using the continuity equation and taking into account the energy losses for solar-flare-accelerated particles, we obtain the time-dependent particle distribution and thus the time behavior of the resulting rays. The important processes for producing rays in solar flares are found to be nonthermal electron bremsstrahlung, decay of neutral mesons, positron annihilation, neutron capture, and decay of excited nuclei. The results are applied to several known solar flares. For a large flare such as the class 3+ on February 23, 1956, continuous rays with energies up to 100 MeV from electron bremsstrahlung and neutral meson decays are observable at the orbit of the Earth by existing -ray detectors. Line rays from positron annihilation (0.51 MeV), neutron capture (2.23 MeV), and deexcitation of excited nuclei O16 (6.14 and 7.12 MeV) and C12 (4.43 MeV) are particularly strong and well above the continuous -ray background due to electron bremsstrahlung. These lines can be detected at the Earth.NASA-NRC Resident Research Associate. 相似文献
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基于ArcGIS的燃气管网水力计算的设计与实现 总被引:1,自引:0,他引:1
为利用ArcGIS软件管理燃气管网数据,以特殊方式直接读取ArcMap的燃气管网图形数据,并完成整个管网的水力计算。算法不受管网的规模和结构的限制,以DLL的方式封装了数据的存取和计算功能,作为核心模块集成到基于ArcGIS Object的GIS平台。 相似文献