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21.
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
22.
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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利用NI 的PXI-6281高速数据采集卡来完成角速度波动信号的采集,借鉴信号失真度的概念,分析角速度反馈信号的基波和高次谐波大小,求取高次谐波与基波幅值比,作为角速度波动率. 相似文献
24.
主动段扰动引力是引起弹道导弹制导方法误差的主要因素。因此,要提高导弹的制导精度,就必须能够在弹上实时计算扰动引力。但现有方法在计算快速性和存储量之间无法得到有效协调。为此,把广义延拓逼近思想引入有限元逼近方法中,将插值单元周围节点的信息也包含到单元内一点扰动引力的计算当中,建立了一种新的数学模型。对所选发射空域,在发射坐标系中进行了直角坐标划分。计算结果表明,这种方法能够更加精确地逼近弹道导弹主动段的扰动引力,在600 km×250 km×6 km的主动段飞行区域内,只需要保存60个节点数据,就能使由逼近误差导致的落点偏差小于10 m,是一般有限元逼近方法精度的4倍以上。 相似文献
25.
电子商务中虚拟现实的应用 总被引:3,自引:0,他引:3
针对虚拟现实技术在电子商务等领域的广泛应用,阐述了虚拟现实的概念、几种实现方法的原理。给出了用杰图造型师软件实现面向景点的三维全景图和面向物体的三维全景图的方法和步骤;分析了连接www网的场景描述语言—VRML的语言结构,编辑方法和VRML的常用浏览器软件,这样用键盘或鼠标任意改变视角来观看在网页上展示的各种产品。总结了虚拟现实技术未来的应用领域和应用前景,以及受成本、硬件、带宽、模拟环境等因素的影响可以选择不同的技术形式。 相似文献
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27.
可拓模式识别算法是根据各个关联度的对比来识别最终的模式,其中经典域区间的确定有着重要的作用。传统的经典域确定方法是基于数理统计学的,不适用于小样本数据,数据不完全以及数据分布未知等复杂情况。引入Bootstrap算法,并和传统的方法对比,更精确地确定了经典域区间。 相似文献
28.
本文通过对该型教练机现有航空电子系统构型、驾驶员操作程序、接口控制文件深入研究,结合未来功能扩展需求,给出了合理的系统构型分析、功能分配、数据流规划、原相关系统软件改动分析,在此基础上还设计出了嵌入式训练系统技术方案.依据方案研制的嵌入式训练系统原理样机通过系统动态试验、航电系统地面综合试验和飞机地面通电试验,证明系统... 相似文献
29.
AOS(Advanced Orbiting System,高级在轨系统)已经逐渐被各国空间组织采用,随着空间任务的发展趋势更多样化和复杂化,对AOS的QoS(Quality of Service,服务质量)也提出了更高要求.针对AOS服务质量的提升需求,提出了一种虚拟信道优先级策略,使用大容量缓存结合数据压缩动态策略和遥测数据抽帧策略相结合的QoS保证方法,通过分析返向链路带宽与航天器遥测用户带宽的裕量,可以动态调整QoS保证,以适应不同应用环境下的航天器AOS的QoS保证需求.通过模拟不同的工况进行仿真试验,结果表明,该AOS服务质量保证方法适用于返向链路带宽裕量充足和不足的工况,比传统的全同步策略和同步异步结合策略拥有更广泛的适应范围. 相似文献
30.