全文获取类型
收费全文 | 434篇 |
免费 | 75篇 |
国内免费 | 107篇 |
学科分类
航空航天 | 616篇 |
出版年
2024年 | 1篇 |
2023年 | 5篇 |
2022年 | 13篇 |
2021年 | 24篇 |
2020年 | 25篇 |
2019年 | 15篇 |
2018年 | 25篇 |
2017年 | 20篇 |
2016年 | 29篇 |
2015年 | 22篇 |
2014年 | 23篇 |
2013年 | 31篇 |
2012年 | 36篇 |
2011年 | 40篇 |
2010年 | 38篇 |
2009年 | 35篇 |
2008年 | 38篇 |
2007年 | 35篇 |
2006年 | 41篇 |
2005年 | 23篇 |
2004年 | 17篇 |
2003年 | 12篇 |
2002年 | 10篇 |
2001年 | 6篇 |
2000年 | 4篇 |
1999年 | 8篇 |
1998年 | 6篇 |
1997年 | 2篇 |
1996年 | 5篇 |
1995年 | 11篇 |
1994年 | 1篇 |
1993年 | 3篇 |
1992年 | 1篇 |
1991年 | 3篇 |
1990年 | 3篇 |
1989年 | 2篇 |
1988年 | 1篇 |
1984年 | 2篇 |
排序方式: 共有616条查询结果,搜索用时 218 毫秒
51.
把高压太阳电池阵放入低地球轨道中就会发生电弧放电,造成航天器表面退化、电磁干扰、PN结破坏和其它负作用.文章在阐述电弧放电机理的基础上,介绍了在试验室模拟等离子体环境中进行的两次放电试验.其中一个试验使用的是太阳电池阵物理等效模拟试件,另一个则是真实的太阳电池阵样品.试验得出了两种样品在等离子体环境中的放电位置、放电阈值电压,并发现环境与太阳电池电压及放电率等相关参数的关系.比较两个试验可以看出,在相似的环境下,模拟试件的放电阈值比较大.文章最后对试验现象的发生原因进行了初步的分析.研究LEO等离子体环境与HVSA之间的相互作用,并采取相应的防护措施,是大型空间活动必须解决的关键技术之一. 相似文献
52.
等离子体表面技术的研究与应用 总被引:5,自引:0,他引:5
概述了离子注入、离子束沉积、等离子喷涂、离子镀、等离子体增强化学气相沉积、等离子体化学热处理和双层辉光离子渗金属等等离子体表面技术的基本原理和最新进展,并给出了部分典型实例。 相似文献
53.
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
54.
55.
空间飞行体与等离子体在压缩区内的非稳态相互作用研究 总被引:1,自引:1,他引:1
研究了空间飞行体在运动过程中,其前端压缩区内飞行体与等离子体的、非稳态相互作用问题,得到了在强天线辐射源高频场作用下的控制方程.通过计算表明,飞行体上的天线可作为调制不稳定性的激发源,在等离子体中激发起很强的电磁孤波. 相似文献
56.
空间等离子体导致高电压太阳阵的电流收集 总被引:3,自引:0,他引:3
给出一种能方便计算空间等离子体引起高电压太阳阵(HVSA)电流收集的理论统计模式,通过对物理过程分析认为空间等离子体致HVSA的功率损耗对HVASA的设计是不应忽视的。 相似文献
57.
58.
59.
利用调制脉冲产生的余辉等离子体的参数测量表明:等离子体空间电位和电子温度的衰变是重要的,它在余辉等离子体的密度衰变过程研究中必须予以考虑.对容器中余辉等离子体密度径向分布的测量结果与理论预言是一致的. 相似文献
60.
光纤表面等离子体波传感器在理论上具有较高的研究价值 ,并且因为结构简单、灵敏度高等特点在工程上得到广泛应用。使用光纤表面等离子体波来测试折射率 ,方法简单、灵敏。本文介绍了利用光纤表面等离子体波传感器使用这种方法对环氧树脂复合材料进行固化监测。文中对不同折射率的溶液进行了折射率测试的研究 ,并设计了一种用于折射率测量的性能稳定、操作方便的光纤传感探头及整套的测试系统 ,用以对固化过程中环氧树脂在不同阶段的折射率变化进行实测。测试结果表明 ,该系统工作稳定、可靠 ,测试结果符合实际情况 相似文献