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81.
Ni-7.3%Si-2.2%B合金快淬组织与深过冷快凝机制 总被引:1,自引:0,他引:1
采用B_2O_3玻璃和纯循环过热净化相结合的方法去除液态金属中的异质晶核,使液态Ni-7.3%Si-2.2%B合金获得了330K的过冷度。对比分析了该合金在低温基板上的快淬薄片与大体积深过冷试样的微观组织。借助计算机和红外测温系统,快速采集了熔体的再辉过程。数据处理发现,在深过冷液态金属的整个再辉区间,温度的上升速率呈瞬态变化特征,再辉时间随初始过冷度的提高而减小。最后,由再辉曲线确定出深过冷液态金属再辉过程中的固相分数与时间以及凝固速度与瞬时过冷度的关系。 相似文献
82.
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
83.
用扫描隧道显微镜(STM)对粘胶基碳纤维(RCF)表面的微观结构进行了研究,首次获得了原子级的RCF图像,对其原子间距作了精确地量化,并且尝试着将所得到的图像与高定向降解石墨(HOPG)相比较,以期对RCF的微观结构有更深入的了解,在原子级尺度上,发现了原子排列并不规则的石墨状结构,二维视图量化结果表明:相邻原子间距为0.142nm,最近六圆环中心的距离是0.253nm。 相似文献
84.
本文构造了轴向大扰动,径向小扰动轴对称速势方程的AF-2分解格式,计算了IC型皮托管式进气道的跨音速内外流场,并对这种分解格式进行了线化的稳定性分析。分析表明:AF-2方法的稳定性优于SLOR方法,其收敛速度至少比SLOR方法快10倍。 相似文献
85.
介绍了与F/A-18E/F飞机发动机提高性能相适应的、设计Ma=2.0的固定几何的“CARET”进气道的设计,分析了新设计的E/F进气道性能和机体/进气道一体化的模型风洞试验结果。该进气道新概念设计对我国在研或预研的某些机种都有较好的参考与借鉴价值。 相似文献
86.
87.
武迪蒙%曾科%唐文睿%杨刚 《宇航材料工艺》2007,37(2):17-21
合成了三种AB型聚酰亚胺单体:4-(4-氨基苯氧基)邻苯二甲酸(单体4),4-(3-氨基苯氧基)邻苯二甲酸(单体7)和对(间)乙基4-(3-氨基苯氧基)邻苯二甲酸酯(单体8或9)。利用热失重分析(TGA)对比研究了这三种AB型聚酰亚胺单体的热行为。结果表明,单体4、单体7和单体8(9)在升温的过程中能发生热聚合生成聚酰亚胺。将单体4用于气相沉积聚合设备,得到了均匀透明的聚酰亚胺薄膜。对分子结构的修饰使单体8(9)较之单体7有更好的挥发性。 相似文献
88.
89.
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
90.
UKF方法及其在方位跟踪问题中的应用 总被引:13,自引:0,他引:13
采用UKF(Unscented Kalman Filter)方法处理了平面内地面站对目标的方位跟踪的估计问题。目标的位置和速度由选定的高斯分布采样点来近似,在每个更新过程中,采样点随着状态方程传播并随着非线性测量方程变换,由此不但得到目标位置和速度的均值及较高的计算精度,而且避免了对非线性方程的线性化过程。仿真结果表明,UKF方法比传统的扩展卡尔曼滤波(EKF)算法有更高的估计精度,并能有效地克服非线性严重时,方位跟踪问题中很容易出现的滤波发散问题。 相似文献