全文获取类型
收费全文 | 471篇 |
免费 | 108篇 |
国内免费 | 95篇 |
专业分类
航空 | 233篇 |
航天技术 | 153篇 |
综合类 | 58篇 |
航天 | 230篇 |
出版年
2024年 | 5篇 |
2023年 | 15篇 |
2022年 | 13篇 |
2021年 | 29篇 |
2020年 | 23篇 |
2019年 | 19篇 |
2018年 | 39篇 |
2017年 | 38篇 |
2016年 | 21篇 |
2015年 | 19篇 |
2014年 | 38篇 |
2013年 | 24篇 |
2012年 | 45篇 |
2011年 | 33篇 |
2010年 | 33篇 |
2009年 | 30篇 |
2008年 | 31篇 |
2007年 | 37篇 |
2006年 | 30篇 |
2005年 | 30篇 |
2004年 | 11篇 |
2003年 | 25篇 |
2002年 | 10篇 |
2001年 | 7篇 |
2000年 | 8篇 |
1999年 | 8篇 |
1998年 | 6篇 |
1997年 | 5篇 |
1996年 | 5篇 |
1995年 | 9篇 |
1994年 | 7篇 |
1993年 | 1篇 |
1992年 | 8篇 |
1991年 | 5篇 |
1990年 | 2篇 |
1989年 | 2篇 |
1988年 | 1篇 |
1987年 | 1篇 |
1984年 | 1篇 |
排序方式: 共有674条查询结果,搜索用时 15 毫秒
1.
提出了一种新的六端口自校准方法.本方法从六端口相对功率理论出发,导出了六端口系统常数的自校准方程,给出了求解系统常数初值的方法,并利用梯度法对方程组求解,仿真结果表明用一个匹配负载、四个失配负载就可以解出系统常数. 相似文献
2.
逆合成孔径雷达信号处理方法研究进展 总被引:3,自引:0,他引:3
朱兆达 《南京航空航天大学学报》1995,27(1):59-66
在简要评述国内外现有的逆合成孔径雷达(ISAR)信号处理的运动补偿和成象方法之后,介绍了南京航空航天大学ISAR课题组近年来在ISAR信号处理方法研究中取得的主要进展,包括基于多散射点定位观点的雷达成象观测模型,基于最大似然原理的同时运动补偿和成象方法,基于最大似然原理的多目标成象方法和基于时频分析的多目标成象方法,以及超分辩成象方法,文末指出了在ISAR信号处理方面有待进一步研究的问题。 相似文献
3.
最新的技术发展已为研制超分辨雷达创造了条件。它能够突破普通雷达基于匹配滤波原理的分辨能力,而实现超分辨。超分辨雷达的巨大计算量通常来自求解非线性最小二乘问题时的多维搜索。本文针对这一问题,研究了雷达信号处理中的两个典型例子:(1)利用阵列处理检测个数已知而方向未知的雷达目标;(2)对波音727飞机进行超分辨距离多普勒成像。说明Hop-field神经网络通过集体运算能够求解各种困难的最优化问题,因而在未来的超分辨雷达中有广阔的应用前景。 相似文献
4.
对不同视角雷达回波进行融合可以形成大的相干积累角,显著增强雷达空间监控能力。给出一种角分集(制)信号融合成像方法,对于角分集(制)回波方位向存在大的间隔,首先将每一距离单元方位向有效稀疏孔径数据排列组合成一Hankel矩阵,由参数化方法估计一维信号参数,再由估计得到的参数对空缺部分预测填补,对每个距离单元横向补全后,压缩得到二维图像。该方法克服了以往预测方法的不足,能有效用于方位向稀疏孔径预测外推,最终仿真与实际数据处理结果证实结论。 相似文献
5.
低轨卫星面阵凝视成像技术研究 总被引:2,自引:0,他引:2
文章介绍了面阵凝视成像的工作原理及特点,阐述了低轨卫星对地观测凝视成像面临的像移问题及其解决措施,对像移补偿装置与二维指向机构的结合做了初步探讨。 相似文献
6.
7.
提出一种适用于高星载聚束式合成孔径雷达(SAR)的改进Extended Chirp Scaling(ECS)算法。基于斜视距离等效模型,推导出改进的ECS算法,给出改进的方位Scaling因了以及算法的实现步骤。在斜视情况下改进的方法Scaling因子可以减小算法所需要的方位时间展宽,提高方位处理效率。为解决高分辨率星载聚束式SAR脉冲重复频率(PRF)过高等问题,在算法中结合了子孔径处理,并分析了采用子孔径处理的必要性及其实现方法。最后,通过计算机仿真,验证了算法的有效性。 相似文献
8.
通过对新型电子战装备的测试需求分析,提出一种基于微波注入网络的电子战装备测试系统.介绍了该测试系统的功能及工作原理;设计了基于微波注入网络的电子战装备测试系统的结构,并对各模块的功能进行了简单描述;最后对微波注入网络控制精度的关键技术进行了研究. 相似文献
9.
介绍了稀疏孔径成像系统的发展现状。重点介绍了系统的成像原理和种类,国外的研究进展以及系统实现的关键技术和应用前景。 相似文献
10.
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