首页 | 本学科首页   官方微博 | 高级检索  
文章检索
  按 检索   检索词:      
出版年份:   被引次数:   他引次数: 提示:输入*表示无穷大
  收费全文   104篇
  免费   9篇
  国内免费   16篇
航空   85篇
航天技术   33篇
综合类   5篇
航天   6篇
  2022年   1篇
  2021年   2篇
  2020年   3篇
  2019年   1篇
  2018年   3篇
  2017年   1篇
  2016年   1篇
  2015年   2篇
  2014年   5篇
  2013年   4篇
  2012年   3篇
  2011年   1篇
  2010年   8篇
  2009年   11篇
  2008年   7篇
  2007年   17篇
  2006年   6篇
  2005年   11篇
  2004年   8篇
  2003年   5篇
  2002年   5篇
  2000年   1篇
  1999年   5篇
  1998年   5篇
  1997年   1篇
  1996年   1篇
  1994年   3篇
  1993年   2篇
  1992年   1篇
  1991年   1篇
  1990年   1篇
  1989年   2篇
  1988年   1篇
排序方式: 共有129条查询结果,搜索用时 31 毫秒
1.
Gradual solar energetic particle (SEP) events are evidently accelerated by coronal/interplanetary shocks driven by coronal mass ejections. This talk addresses the different factors which determine the composition of the accelerated ions. The first factor is the set of available seed populations including the solar wind core and suprathermal tail, remnant impulsive events from preceding solar flares, and remnant gradual events. The second factor is the fractionation of the seed ions by the injection process, that is, what fraction of the ions are extracted by the shock to participate in diffusive shock acceleration. Injection is a controversial topic since it depends on the detailed electromagnetic structure of the shock transition and the transport of ions in these structured fields, both of which are not well understood or determined theoretically. The third factor is fractionation during the acceleration process, due to the dependence of ion transport in the turbulent electromagnetic fields adjacent to the shock on the mass/charge ratio. Of crucial importance in the last two factors is the magnetic obliquity of the shock. The form of the proton-excited hydromagnetic wave spectrum is also important. Finally, more subtle effects on ion composition arise from the superposition of ion contributions over the time history of the shock along the observer’s magnetic flux tube, and the sequence of flux tubes sampled by the observer.  相似文献   
2.
混粉电火花加工表面的研究   总被引:1,自引:0,他引:1  
分析了混粉电火花加工工件表面的组成成分,探讨了混粉电火花加工获得低的表面粗糙度的机理。  相似文献   
3.
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   
4.
模拟月壤研制的初步设想   总被引:10,自引:2,他引:10  
模拟月壤是月球样品的地球化学复制品,作者总结世界上已有的5种模拟月壤JSC-1,MLS.1,MLS-2,MKS-1和FJS-1的研制过程、方法与基本理化性质,认为系列化模拟月壤研制对中国首次月球探测有重要意义,在此基础上,作者提出系列化模拟月壤研制的基本思路.  相似文献   
5.
韩利凯 《航空计算技术》2002,32(3):114-116,121
就一种用 80 31单片机控制的计算机组成原理实验仪的设计及实现进行了详细论述。  相似文献   
6.
中纬电离层暴时形态的理论模式研究   总被引:1,自引:0,他引:1  
结合观测结果对中纬电离层暴时形态进行理论模式研究.分析了两次电离层暴变事件中影响其基本形态的原子-分子含量比、上部输运通量和中性风等因素的行为,发现在这两次具有不同特点的事件中,中性风较为平稳,而原子-分子含量比和耦合输运通量的相对作用则各不相同.   相似文献   
7.
Optical emission and linear laser absorption spectroscopy techniques were used in investigation of plasma with copper and silver admixture. The method of selection of spectral lines and spectroscopic data with the aim of diagnostics of multicomponent air plasma with two metal vapors admixture was developed. Energy level populations behavior on the Boltzmann plot were used for Cu I and Ag I spectroscopic data selection. In this way the selection of spectroscopic data for some of Cu I and Ag I lines was realized. Stark broadening parameters of Cu I and Ag I were examined. Experimentally obtained temperature and electron density radial distributions were used in the calculation of plasma composition in the assumption of local thermodynamic equilibrium. Linear laser absorption spectroscopy was used to examine the state of plasma.  相似文献   
8.
In the past, clues on the potential radiogenic activity of the lunar interior have been obtained from the isotopic composition of noble gases like Argon. Excess Argon (40) relative to Argon (36), as compared to the solar wind composition, is generally ascribed to the radiogenic activity of the lunar interior. Almost all the previous estimates were based on, ‘on-the-spot’ measurements from the landing sites. Relative concentration of the isotopes of 40Ar and 36Ar along a meridian by the Chandra’s Altitudinal Composition Explorer (CHACE) experiment, on the Moon Impact Probe (MIP) of India’s first mission to Moon, has independently yielded clues on the possible spatial heterogeneity in the radiogenic activity of the lunar interior in addition to providing indicative ‘antiquity’ of the lunar surface along the ground track over the near side of the moon. These results are shown to broadly corroborate the independent topography measurements by the Lunar Laser Ranging Instrument (LLRI) in the main orbiter Chandrayaan-1. The unique combination of these experiments provided high spatial resolution data while indicating the possible close linkages between the lunar interior and the lunar ambience.  相似文献   
9.
针对航空发动机作业并行交叉的特点,提出一种“自底向上”的柔性建模方法,着重描述异类对象作业工序对资源的占用与冲突。引入基于资源库所的共享合成运算,解决了Petri网结构重用性差而无法动态建模的问题,合成模型具有守衡、有界和无死锁的结构性质。模型的状态方程在极大-加法代数意义下具有线性的形式,结合遗传算法实现基于周期的静态调度优化。  相似文献   
10.
李国民  刘军  沙江波 《航空学报》2010,31(8):1688-1694
 为了寻求Nb合金的强度和塑性的平衡,设计了以Nb基固溶体Nbss为主导相的Nb-xSi-6Hf-4Zr-2B-yTi(x=4,8;y=10,30;原子分数)合金,研究了Si和Ti对合金组织和室温力学性能的影响。结果表明,合金由Nbss、Nb3Si和Nb5Si3等3相组成。4Si-(10,30)Ti合金铸态组织是Nb枝晶和分布在枝晶间的硅化物(Nb3Si和Nb5Si3),8Si-(10,30)Ti合金Nb枝晶间分布的是Nb/硅化物(Nb5Si3)的共晶和Nb3Si,随着Si和Ti含量的增加,硅化物体积分数增加。1 600 ℃退火50 h可使部分Nb3Si共析分解,改变合金的组织形貌和各相的体积分数。随着Si和Ti含量的增加,合金的硬度和强度增加,但塑性和韧性降低。Nb枝晶的失效方式为解理断裂,而硅化物为脆性断裂。  相似文献   
设为首页 | 免责声明 | 关于勤云 | 加入收藏

Copyright©北京勤云科技发展有限公司  京ICP备09084417号