全文获取类型
收费全文 | 635篇 |
免费 | 182篇 |
国内免费 | 137篇 |
专业分类
航空 | 484篇 |
航天技术 | 227篇 |
综合类 | 48篇 |
航天 | 195篇 |
出版年
2024年 | 2篇 |
2023年 | 10篇 |
2022年 | 45篇 |
2021年 | 53篇 |
2020年 | 56篇 |
2019年 | 34篇 |
2018年 | 37篇 |
2017年 | 43篇 |
2016年 | 47篇 |
2015年 | 32篇 |
2014年 | 37篇 |
2013年 | 45篇 |
2012年 | 53篇 |
2011年 | 65篇 |
2010年 | 53篇 |
2009年 | 49篇 |
2008年 | 47篇 |
2007年 | 45篇 |
2006年 | 50篇 |
2005年 | 35篇 |
2004年 | 22篇 |
2003年 | 15篇 |
2002年 | 11篇 |
2001年 | 9篇 |
2000年 | 6篇 |
1999年 | 8篇 |
1998年 | 7篇 |
1997年 | 5篇 |
1996年 | 6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954条查询结果,搜索用时 15 毫秒
1.
《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2020,65(7):1701-1713
Equatorial plasma bubbles (EPBs) are common features of the equatorial and low-latitude ionosphere and are known to cause radio wave scintillation which leads to the degradation of communication and navigation systems. Although these structures have been studied for decades, a full understanding of their evolution and dynamics remains important for space weather mitigation purposes. In this study, we present cases of EPBs occurrences around April and July 2012 geomagnetic storm periods over the African equatorial sector. The EPBs were observed from the Communications/Navigation Outage Forecasting System (C/NOFS) and generally correlated well to the ionospheric irregularities observed from the Global Positioning System total electron content (GPS-TEC) measurements (rate of TEC change, ROT). This study revealed that the evolution of the EPBs during moderate storms is controlled by the strength of the daytime equatorial electrojet (EEJ) currents regardless of the strength of the equatorial ionization anomaly (EIA), the latter is observed during the July storm case in particular. These effects were more evident during the main and part of the early recovery phases of the geomagnetic storm days considered. However, the evening hours TEC gradients between regions of the magnetic equator and ionization crests also played roles in the existence of ionospheric irregularities. 相似文献
2.
Karl-Heinz Glassmeier Ingo Richter Andrea Diedrich Günter Musmann Uli Auster Uwe Motschmann Andre Balogh Chris Carr Emanuele Cupido Andrew Coates Martin Rother Konrad Schwingenschuh Karoly Szegö Bruce Tsurutani 《Space Science Reviews》2007,128(1-4):649-670
The fluxgate magnetometer experiment onboard the ROSETTA spacecraft aims to measure the magnetic field in the interaction
region of the solar wind plasma with comet 67P/Churyumov-Gerasimenko. It consists of a system of two ultra light (about 28
g each ) triaxial fluxgate magnetometer sensors, mounted on the 1.5 m long spacecraft boom. The measurement range of each
sensor is ±16384 nT with quantization steps of 31 pT. The magnetometer sensors are operated with a time resolution of up to
0.05 s, corresponding to a bandwidth of 0–10 Hz. This performance of the RPC-MAG sensors allows detailed analyses of magnetic
field variations in the cometary environment. RPC-MAG furthermore is designed to study possible remnant magnetic fields of
the nucleus, measurements which will be done in close cooperation with the ROSETTA lander magnetometer experiment ROMAP. 相似文献
3.
4.
介绍了液体火箭发动机推力室铣槽结构热应力的数值分析方法,通过建立液体火箭发动机推力室的流场燃烧和导热理论模型,运用有限体积法考虑液膜冷却计算出发动机工作时的燃气、燃烧室壳体和冷却工质的温度场,将得出的结果作为壳体热应力计算模型的边界条件进行热应力场有限元分析。内、外壁温度的计算数据与实验结果基本相符。 相似文献
5.
6.
建立了离子推力器束流分布的高斯模型,以200mm氙离子推力器为例,在不同工作环境下对推力器束流分布进行了数值模拟,并通过试验测量了推力器引出切面不同位置(轴向z=50mm,z=100mm)下的径向束电流密度和束离子密度分布。通过对数值模拟结果与试验测量结果的比较,误差为17%,认为数值模拟结果与试验测量结果吻合较好。表明离子推力器引出束流呈轴对称分布,在推力器出口附近,束离子密度很大,越往下游,密度越小且束流出现发散。 相似文献
7.
介绍了一种活塞位移型体积管常数的测定方法、数学模型及其测量标准不确定度分量,并给出了不确定度评定实例和验证结果。 相似文献
8.
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
9.
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