全文获取类型
收费全文 | 1284篇 |
免费 | 262篇 |
国内免费 | 299篇 |
专业分类
航空 | 691篇 |
航天技术 | 398篇 |
综合类 | 129篇 |
航天 | 627篇 |
出版年
2024年 | 13篇 |
2023年 | 37篇 |
2022年 | 40篇 |
2021年 | 43篇 |
2020年 | 45篇 |
2019年 | 27篇 |
2018年 | 80篇 |
2017年 | 51篇 |
2016年 | 66篇 |
2015年 | 58篇 |
2014年 | 101篇 |
2013年 | 68篇 |
2012年 | 128篇 |
2011年 | 126篇 |
2010年 | 97篇 |
2009年 | 95篇 |
2008年 | 95篇 |
2007年 | 71篇 |
2006年 | 96篇 |
2005年 | 81篇 |
2004年 | 55篇 |
2003年 | 43篇 |
2002年 | 33篇 |
2001年 | 39篇 |
2000年 | 39篇 |
1999年 | 34篇 |
1998年 | 30篇 |
1997年 | 25篇 |
1996年 | 20篇 |
1995年 | 22篇 |
1994年 | 17篇 |
1993年 | 10篇 |
1992年 | 20篇 |
1991年 | 8篇 |
1990年 | 7篇 |
1989年 | 9篇 |
1988年 | 7篇 |
1987年 | 2篇 |
1986年 | 6篇 |
1984年 | 1篇 |
排序方式: 共有1845条查询结果,搜索用时 31 毫秒
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.
反射面天线的双站雷达截面 总被引:1,自引:0,他引:1
本文导出了任意旋转反射器天线在任意双站角的散射场和雷达截面(RCS),其中反射场由几何光学法(GO)求得,绕射场则利用基于物理绕射理论(PTD)与等效线电流辐射积分公式导出的等效电磁流法求得。分别计算了轴向入射和偏轴向入射时在任意散射方向上水平极化与垂直极化两种情况下的双站RCS,并给出了这些结果的立体图形式。方法简化为单站情况时的计算结果与实验值大致相符。 相似文献
23.
24.
25.
自适应DBF与空间谱估计 总被引:2,自引:0,他引:2
讨论了自适应数字波束形成(DBF)技术和超分辨空间谱估计技术,并提出了一种基于信号协方差矩阵特征分解的时-空二维信号高分辨谱估计算法。以上技术应用于相控阵雷达系统,可以精确获得多个运动目标的方位信息和多普勒信息。文章最后给出了计算机模拟结果。 相似文献
26.
利用MF雷达对耀斑期间电离层D区电子密度的观测研究 总被引:1,自引:0,他引:1
利用MF雷达观测资料对X级别耀斑爆发期间在66-80km高度之间的电子密度进行了研究,观测到了耀斑爆发期间电子密度的突然增加,在较低高度上的电子密度的时间变化趋势与耀斑的软X射线辐射通量相关.电子密度的变化强度依赖于具体的耀斑参数,有些耀斑引起的电子密度增加高达400cm^-3,有些仅为100cm^-3左右.但耀斑期间在这一高度区间增加的总电子含量增量仅占耀斑辐射引起的整个电离层总电子含量增量的千分之一左右.最后,利用恢复阶段电子密度的时间变化过程估算了1997年11月4日耀斑期间部分高度上的有效复合系数. 相似文献
27.
A. Guharay P.P. Batista R.A. Buriti 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2021,67(10):3125-3133
An evident signature of a least studied quasi-90-day oscillation is found in the winds and tides in the MLT from an equatorial station, São João do Cariri (7.4°S, 36.5°W). The oscillation is found to appear mainly in certain intervals with small but appreciable seasonal (fourth harmonic of annual oscillation) contribution. The maximum amplitude of the oscillation is found to be around 10 m/s in the zonal wind. The enhancement peak of the oscillation exhibits downward movement indicating a plausible role of upward moving waves/tides in carrying its imprint from below to the MLT. Similar oscillation feature in the tropospheric zonal wind and ozone may imply its lower atmospheric origin as a component of the intraseasonal oscillation (ISO) that moves upward by modulating the tides. Subsequently, the propagating tides (mainly semidiurnal) are enhanced by the ozone in the stratosphere through absorption of solar UV radiation and finally manifest the oscillation in the MLT. Consistency of the present findings with the past investigations are observed in some aspects of the oscillation, whereas existing mismatches in others are believed to be due to geophysical variability depending on space and time among various locations on the globe. 相似文献
28.
29.
雷达导引头是反舰导弹的重要组成部分,对其综合能力的评估是一个多因素综合评判问题。文章分析了影响雷达导引头综合能力的主要因素,建立了雷达导引头综合能力评估指标体系和基于联系度的雷达导引头综合能力评估模型,并提出了联系度的比较规则。最后,评估得出了国外几种典型的雷达导引头综合能力的优劣排序。 相似文献
30.