全文获取类型
收费全文 | 373篇 |
免费 | 19篇 |
国内免费 | 60篇 |
专业分类
航空 | 159篇 |
航天技术 | 244篇 |
综合类 | 31篇 |
航天 | 18篇 |
出版年
2024年 | 1篇 |
2023年 | 11篇 |
2022年 | 4篇 |
2021年 | 14篇 |
2020年 | 15篇 |
2019年 | 16篇 |
2018年 | 28篇 |
2017年 | 6篇 |
2016年 | 5篇 |
2015年 | 7篇 |
2014年 | 16篇 |
2013年 | 17篇 |
2012年 | 20篇 |
2011年 | 24篇 |
2010年 | 15篇 |
2009年 | 34篇 |
2008年 | 29篇 |
2007年 | 14篇 |
2006年 | 17篇 |
2005年 | 17篇 |
2004年 | 9篇 |
2003年 | 25篇 |
2002年 | 7篇 |
2001年 | 10篇 |
2000年 | 7篇 |
1999年 | 9篇 |
1998年 | 13篇 |
1997年 | 14篇 |
1996年 | 10篇 |
1995年 | 8篇 |
1994年 | 14篇 |
1993年 | 5篇 |
1992年 | 3篇 |
1991年 | 1篇 |
1990年 | 3篇 |
1988年 | 1篇 |
1986年 | 2篇 |
1984年 | 1篇 |
排序方式: 共有452条查询结果,搜索用时 46 毫秒
191.
G.N. Kichigin 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
The paper discusses the possibility of particle acceleration up to high energies in relativistic waves generated by various explosive processes in the interstellar medium. We propose to use the surfatron mechanism of acceleration (surfing) of charged particles trapped in the front of relativistic waves as a generator of high-energy cosmic rays (CRs). Conditions under which surfing in the waves under consideration can be made are studied thoroughly. Ultra-high-energy CRs (up to 1020 eV) are shown to be obtained due to the surfing in relativistic plane and spherical waves. Surfing is supposed to take place in nonlinear Langmuir waves excited by powerful electromagnetic radiation or relativistic beams of charged particles, as well as in strong shock waves generated by relativistic jets or spherical formations that expand fast (fireballs). 相似文献
192.
E.I. Astafyeva E.L. Afraimovich S.V. Voeykov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(9):1459-1462
By using data from GPS receivers we detected huge-amplitude solitary large-scale traveling acoustic-gravity waves (LS AGW) which manifested themselves as perturbations of total electron content (TEC) of duration of about 40 min. Originated in the auroral area after significant alterations of geomagnetic field intensity during geomagnetic storms on 29–30 October 2003, LS disturbances propagated with a velocity about 1000–1200 m/s and caused generation of secondary small-scale (SS) waves with time period of 2–10 min. Such SS structure followed the solitary intensive AGW at a distance more than 4000 km. However, we observed such phenomenon only within the territory with high values of “vertical” TEC and steep gradients of TEC. Apparently, these conditions are necessary for generation of SS waves due to propagation of LS AGW. 相似文献
193.
I.R. Petrova V.V. Bochkarev R.R. Latipov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
We present results of the spectral analysis of data series of Doppler frequency shifted signals reflected from the ionosphere, using experimental data received at Kazan University, Russia. Spectra of variations with periods from 1 min to 60 days have been calculated and analyzed for different scales of periods. The power spectral density for spring and winter differs by a factor of 3–4. Local maxima of variation amplitude are detected, which are statistically significant. The periods of these amplitude increases range from 6 to 12 min for winter, and from 24 to 48 min for autumn. Properties of spectra for variations with the periods of 1–72 h have been analyzed. The maximum of variation intensity for all seasons and frequencies corresponds to the period of 24 h. Spectra of variations with periods from 3 to 60 days have been calculated. The maxima periods of power spectral density have been detected by the MUSIC method for the high spectral resolution. The detected periods correspond to planetary wave periods. Analysis of spectra for days with different level of geomagnetic activity shows that the intensity of variations for days with a high level of geomagnetic activity is higher. 相似文献
194.
Soft X-ray (SXR) waves, EIT waves, and Hα Moreton waves are all associated with coronal mass ejections (CMEs). The knowledge of the characteristics about these waves is crucial for the understanding of CMEs, and hence for the space weather researches. MHD numerical simulation is performed, with the consideration of the quiet Sun atmosphere, to investigate the CME/flare processes. On the basis of the numerical results, SXR, EUV, and Hα images of the eruption are synthesized, where SXR waves, EIT waves, and Hα Moreton waves are identified. It confirms that the EIT waves, which border the expanding dimmming region, are produced by the successive opening (or stretching) of the closed magnetic field lines. Hα Moreton waves are found to propagate outward synchronously with the SXR waves, lagging behind the latter spatially by ~27 Mm in the simulated scenario. However, the EIT wave velocity is only a third of the Moreton wave velocity. The synthesized results also suggest that Hα± 0.45Å would be the best off-band for the detection of Hα Moreton waves. 相似文献
195.
The surface wave induced magnetic reconnection (SWIMR) model based on Alfven Resonance theory will be discussed briefly both
for collisional and collisionless plasmas. It is shown that the spatial scales and time delays associated with Flux Transfer
Events and Pulsed Ionospheric Flows, as observed by satellites and SuperDARN radars and the magnetic bubbles, observed at
the high latitude boundary of the magnetopause, can be explained by the SWIMR model.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
196.
One of the most ubiquitous indicators of the state and topology of the magnetosphere are ultra-low frequency (ULF) waves.
These may be continuously and inexpensively monitored from the ground using networks of magnetometers. The most robust measurable
quantity provided by magnetometer networks is signal phase and this paper emphasizes the usefulness of this parameter in a
variety of ULF wave diagnostic processes ranging from equatorial to high latitudes.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
197.
198.
Magneto-gravity Waves Trapped in the Lower Solar Corona 总被引:1,自引:0,他引:1
Yu-Qing Lou 《Space Science Reviews》1999,87(1-2):261-264
The possibility of trapped magneto-gravity waves in the lower solar corona with an open magnetic field is discussed. Intensity
variations and/or Doppler shifts of relevant UV, EUV and x-ray spectral lines in the chromosphere, transition region and lower
corona may reveal the existence of such low-frequency modes (with periods longer than ∼ 1.5 hour). The spectrum may be either
discrete or continuous depending on the reflection property of the narrow transition region. These modes can be utilized to
probe the dynamics of the upper chromosphere, transition region and lower corona; they may also play an important role in
coronal heating.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
199.
介绍了一种斜边占π/5的等腰梯形脉宽调制波,从理论上证明了采用这种PWM(PulseWidth Modulation)波控制的变频器,能消除输出电压的5次谐波分量,使输出电压谐波分量小,电流波形好,系统运行时转矩脉动小,可靠、平稳、噪声低.已将这种控制技术应用于某种列车风扇异步电机的变频调速,实验结果与理论分析相吻合. 相似文献
200.
Impulsively starting flow, by a sudden attainment of a large angle of attack, has been well studied for incompressible and supersonic flows, but less studied for subsonic flow. Recently, a preliminary numerical study for subsonic starting flow at a high angle of attack displays an advance of stall around a Mach number of 0.5, when compared to other Mach numbers. To see what happens in this special case, we conduct here in this paper a further study for this case, to display and analyze the full flow structures. We find that for a Mach number around 0.5, a local supersonic flow region repeatedly splits and merges, and a pair of left-going and right-going unsteady shock waves are embedded inside the leading edge vortex once it is sufficiently grown up and detached from the leading edge. The flow evolution during the formation of shock waves is displayed in detail. The reason for the formation of these shock waves is explained here using the Laval nozzle flow theory. The existence of this shock pair inside the vortex, for a Mach number only close to 0.5, may help the growing of the trailing edge vortex responsible for the advance of stall observed previously. 相似文献