全文获取类型
收费全文 | 1906篇 |
免费 | 343篇 |
国内免费 | 566篇 |
专业分类
航空 | 877篇 |
航天技术 | 664篇 |
综合类 | 127篇 |
航天 | 1147篇 |
出版年
2024年 | 19篇 |
2023年 | 55篇 |
2022年 | 64篇 |
2021年 | 114篇 |
2020年 | 95篇 |
2019年 | 114篇 |
2018年 | 134篇 |
2017年 | 111篇 |
2016年 | 122篇 |
2015年 | 140篇 |
2014年 | 231篇 |
2013年 | 149篇 |
2012年 | 186篇 |
2011年 | 137篇 |
2010年 | 135篇 |
2009年 | 122篇 |
2008年 | 106篇 |
2007年 | 106篇 |
2006年 | 126篇 |
2005年 | 86篇 |
2004年 | 45篇 |
2003年 | 69篇 |
2002年 | 52篇 |
2001年 | 29篇 |
2000年 | 35篇 |
1999年 | 47篇 |
1998年 | 34篇 |
1997年 | 17篇 |
1996年 | 20篇 |
1995年 | 24篇 |
1994年 | 23篇 |
1993年 | 8篇 |
1992年 | 6篇 |
1991年 | 9篇 |
1990年 | 11篇 |
1989年 | 9篇 |
1988年 | 7篇 |
1987年 | 1篇 |
1986年 | 1篇 |
1985年 | 16篇 |
排序方式: 共有2815条查询结果,搜索用时 62 毫秒
81.
液体推进系统充填过程的有限元状态变量模型 总被引:9,自引:2,他引:9
研究了常温推进剂液体火箭发动机充填过程的建模问题。对推进剂充填管道系统进行有限元分割,应用基本守恒定律于充满推进剂的单元和充满气体的单元,两相单元则采用等效流容方程,建立了常温推进剂管道系统充填过程的有限元状态变量模型。模型面向液体推进系统动态过程控制与通用仿真。利用该模型,对一管道充填过程进行了仿真计算,给出了有关计算结果。 相似文献
82.
83.
J. C. Raymond 《Space Science Reviews》1999,87(1-2):55-66
Order of magnitude variations in relative elemental abundances are observed in the solar corona and solar wind. The instruments
aboard SOHO make it possible to explore these variations in detail to determine whether they arise near the solar surface
or higher in the corona. A substantial enhancement of low First Ionization Potential (FIP) elements relative to high FIP elements
is often seen in both the corona and the solar wind, and that must arise in the chromosphere. Several theoretical models have
been put forward to account for the FIP effect, but as yet even the basic physical mechanism responsible remains an open question.
Evidence for gravitational settling is also found at larger heights in quiescent streamers. The question is why the heavier
elements don't settle out completely.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
84.
J. L. Kohl S. Fineschi R. Esser A. Ciaravella S. R. Cranmer L. D. Gardner R. Suleiman G. Noci A. Modigliani 《Space Science Reviews》1999,87(1-2):233-236
Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI. 相似文献
85.
86.
航天飞机末端区域能量管理段制导技术概述 总被引:2,自引:2,他引:2
末端区域能量管理段主要是控制航天飞机的动能和势能.使航天飞机最终达到进场着陆段的初始要求,以保证其最终成功着陆。在最终制导系统引入一个能量基准剖面,通过调整飞行距离、动压或速度制动使航天飞机达到标准的能量状态。将末端区域能量管理段划分为四个飞行段,并对这四个飞行段的基本设计思想、制导技术及过程进行了研究。经过实际的航天飞机飞行验证.证明这种方案具有良好的制导效果。 相似文献
87.
88.
临近空间飞行器测控与信息传输系统频段选择 总被引:7,自引:0,他引:7
临近空间飞行器是高性能信息化武器平台,测控(TT&;C)与信息传输系统是其信息保障的核心,而选择合理、可行的频段是展开系统设计的前提和基础。频段选择影响到整个技术方案的制定,是一个需综合考虑、影响深远并具有战略意义的关键问题,从国际电联(ITU)国际标准、高速数传、接收信噪比(SNR)、“三抗”、超视距中继、黑障、雨衰以及设备研制成熟度8个方面全面、细致论证了近空间平台测控系统的频段选择问题,最终得出在视距链路中以Ka频段为宜,在超视距链路中以Ku/Ka双频段为宜的结论。 相似文献
89.
R. C. Wiens D. S. Burnett C. M. Hohenberg A. Meshik V. Heber A. Grimberg R. Wieler D. B. Reisenfeld 《Space Science Reviews》2007,130(1-4):161-171
The Genesis mission returned samples of solar wind to Earth in September 2004 for ground-based analyses of solar-wind composition,
particularly for isotope ratios. Substrates, consisting mostly of high-purity semiconductor materials, were exposed to the
solar wind at L1 from December 2001 to April 2004. In addition to a bulk sample of the solar wind, separate samples of coronal
hole (CH), interstream (IS), and coronal mass ejection material were obtained. Although many substrates were broken upon landing
due to the failure to deploy the parachute, a number of results have been obtained, and most of the primary science objectives
will likely be met. These objectives include He, Ne, Ar, Kr, and Xe isotope ratios in the bulk solar wind and in different
solar-wind regimes, and 15N/14N and 18O/17O/16O to high precision. The greatest successes to date have been with the noble gases. Light noble gases from bulk solar wind
and separate solar-wind regime samples have now been analyzed. Helium results show clear evidence of isotopic fractionation
between CH and IS samples, consistent with simplistic Coulomb drag theory predictions of fractionation between the photosphere
and different solar-wind regimes, though fractionation by wave heating is also a possible explanation. Neon results from closed
system stepped etching of bulk metallic glass have revealed the nature of isotopic fractionation as a function of depth, which
in lunar samples have for years deceptively suggested the presence of an additional, energetic component in solar wind trapped
in lunar grains and meteorites. Isotope ratios of the heavy noble gases, nitrogen, and oxygen are in the process of being
measured. 相似文献
90.