全文获取类型
收费全文 | 383篇 |
免费 | 81篇 |
国内免费 | 56篇 |
专业分类
航空 | 260篇 |
航天技术 | 184篇 |
综合类 | 35篇 |
航天 | 41篇 |
出版年
2024年 | 2篇 |
2023年 | 9篇 |
2022年 | 11篇 |
2021年 | 19篇 |
2020年 | 20篇 |
2019年 | 20篇 |
2018年 | 26篇 |
2017年 | 21篇 |
2016年 | 18篇 |
2015年 | 16篇 |
2014年 | 26篇 |
2013年 | 31篇 |
2012年 | 26篇 |
2011年 | 32篇 |
2010年 | 21篇 |
2009年 | 35篇 |
2008年 | 16篇 |
2007年 | 12篇 |
2006年 | 19篇 |
2005年 | 23篇 |
2004年 | 11篇 |
2003年 | 23篇 |
2002年 | 6篇 |
2001年 | 8篇 |
2000年 | 6篇 |
1999年 | 14篇 |
1998年 | 8篇 |
1997年 | 8篇 |
1996年 | 5篇 |
1995年 | 7篇 |
1994年 | 8篇 |
1993年 | 2篇 |
1992年 | 4篇 |
1991年 | 3篇 |
1990年 | 2篇 |
1987年 | 2篇 |
排序方式: 共有520条查询结果,搜索用时 46 毫秒
61.
Yen-Hsyang Chu Chin-Lung SuHsiao-Tsung Ko 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
With a network of ground-based ionosondes distributed around the world, the ionospheric peak electron density and its height measured by FORMOSAT-3/COSMIC satellites in terms of GPS radio occultation technique are extensively examined in this article. It is found that, in spite of the latitude, the mean values of the peak electron density measured by COSMIC satellites are systematically smaller than those observed by ground-based ionosondes. The discrepancy between them is dependent on the latitude, namely, it is small in low and mid-latitudes and large in high-latitude region. Moreover, statistical analysis shows that the slopes of the regression line that is best fitted to the scatter diagram of occultation-retrieved peak electron density (ordinate axis) versus ionosonde-observed peak density (abscissa axis) are universally less than one. This feature is believed to be the result of path average effect of non-uniform distribution of the electron density along the GSP ray during the occultation. A comparison between COSMIC-measured peak height and ionosonde-derived peak height hmF2 indicates that the former is systematically higher than the latter. The difference in the two can be as large as 20% or more in equatorial and low-latitude regions. This result implies that the peak height hmF2 derived from the virtual height through true height analysis based on Titheridge method seems to underestimate the true peak height. The correlation between COSMIC and ionosonde peak electron densities is analyzed and the result reveals that correlation coefficient seems to be dependent on the fluctuation of the occultation-retrieved electron density profile. The correlation will be higher (lower) for the electron density profiles with smaller (larger) fluctuations. This feature suggests that the inhomogeneous distribution of the electron density along the GPS ray path during the occultation plays an important role affecting the correlation between COSMIC and ionosonde measurements. 相似文献
62.
V. Truhlik D. Bilitza L. Triskova 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
A database of electron temperature (Te) measurements comprising of most of the available satellite measurements in the topside ionosphere is used for studying the solar activity variations of the electron temperature Te at different latitudes, altitudes, local times and seasons. The Te data are grouped into three levels of solar activity (low, medium, high) at four altitude ranges, for day and night, and for equinox and solstices. We find that in general Te changes with solar activity are small and comparable in magnitude with seasonal changes but much smaller than the changes with altitude, latitude, and from day to night. In all cases, except at low altitude during daytime, Te increases with increasing solar activity. But this increase is not linear as assumed in most empirical Te models but requires at least a parabolic approximation. At 550 km during daytime negative as well as positive correlation is found with solar activity. Our global data base allows to quantify the latitude range and seasonal conditions for which these correlations occur. A negative correlation with solar activity is found in the invdip latitude range from 20 to 55 degrees during equinox and from 20 degrees onward during winter. In the low latitude (20 to −20 degrees invdip) F-region there is almost no change with solar activity during solstice and a positive correlation during equinox. A positive correlation is also observed during summer from 30 degrees onward. 相似文献
63.
再入弹头滚转共振概率估算 总被引:2,自引:0,他引:2
本文分析了滚转共振之机理和影响滚转共振之因素,收集了国外资料有关小不对称量的数据,确定了各参数的概率分布特性,提出了一种直观的再入弹头滚转共振概率估算方法,给出了算例。 相似文献
64.
65.
用共振Rayleigh散射(RRS)光谱研究了酸性磺酞类染料溴甲酚绿和溴酚蓝分别与奈替米星的相互作用.溴甲酚绿和溴酚蓝在酸性介质中分别与奈替米星相互作用,导致RRS光谱显著增强,最大的RRS峰分别位于606nm和572nm处,散射强度与奈替米星的质量浓度在一定的范围内成正比.此方法具有很高的灵敏度,对于奈替米星的检测限(3σ)分别为30ng/mL和10ng/mL,据此发展了一种测定奈替米星的新方法. 相似文献
66.
Rajat Acharya Bijoy Roy M.R. Sivaraman Ashish Dasgupta 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
It is important to use models developed specifically for the equatorial ionospheric estimation for real-time applications, particularly in Satellite Navigation. This work demonstrates a methodology for improved predictions of VTEC in real time using the model developed for the equatorial ionosphere by the authors. This work has been done using TEC data of the low solar activity period of 2005 obtained using dual frequency GPS receivers installed under the GAGAN project of ISRO. For the purpose, the model is first used in conjunction with Kriging technique. Improvement in accuracy is observed when compared with the estimations from the model alone using the measurements as true reference. Further improvement is obtained by Bayesian combination of these estimates with independent Neural Network based predictions. Statistical performance of improvement is provided. An improvement of ∼1 m in confidence level of estimation of VTEC is obtained. 相似文献
67.
Using empirical velocity distributions derived from UVCS and SUMER ultraviolet spectroscopy, we construct theoretical models
of anisotropic ion temperatures in the polar solar corona. The primary energy deposition mechanism we investigate is the dissipation
of high frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which can heat and accelerate ions differently depending
on their charge and mass. We find that it is possible to explain the observed high perpendicular temperatures and strong anisotropies
with relatively small amplitudes for the resonant waves. There is suggestive evidence for steepening of the Alfvén wave spectrum
between the coronal base and the largest heights observed spectroscopically. Because the ion-cyclotron wave dissipation is
rapid, even for minor ions like O5+, the observed extended heating seems to demand a constantly replenished population of waves over several solar radii. This
indicates that the waves are generated gradually throughout the wind rather than propagated up from the base of the corona.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
68.
69.
70.
有磁场时电子在航天器光电子鞘层中的漂移运动 总被引:2,自引:1,他引:1
采用二级漂移近似理论,研究了在航天器光电子鞘层中与电流收集有关的电子在磁场中的运动轨道和收集电子有关的磁瓶结构,结果表明当磁场越强,航天器表面电势越弱,磁瓶在无穷远处横截面积就越小。在光电子鞘层中,势垒对电流收集影响较大,磁瓶的横截面积在略远于垫垒处有极大值,磁瓶在无穷远处的横截面积并非随着势垒距航天器距离的远近而单调变化。 相似文献