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521.
522.
Bernard H. Foing Pascale Ehrenfreund 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
The upcoming fleet of lunar missions, and the announcement of new lunar exploration initiatives, show an exciting “Journey to the Moon”, covering recent results, science, future robotic and human exploration. We review some of the questions, findings and perspectives given in the papers included in this issue of Advances in Space Research. 相似文献
523.
李川 《西安航空技术高等专科学校学报》2012,(5):68-70
SDD-1算法是分布式数据库查询优化的一种算法,研究SDD-1算法的过程,分析SDD-1算法的优缺点,并针对该算法的不考虑最后一点传输代价的缺点提出了改进的SDD-1算法。 相似文献
524.
通过对RIPv1有类路由协议在普通网络结构中的路由传播和更新情况进行研究分析和总结,然后将总结结果应用到特殊网络结构中。调试命令观察和分析特殊结构中使用RIPv1协议的路由传播情况,通过分析特殊结构中的路由更新问题,得出结论。 相似文献
525.
采用第一性原理的平面波赝势方法和局域密度近似(LDA),计算了压力对Li1/2TiS2的形成能和光学性质的影响。研究发现,Li1/2TiS2体系在压强为3GPa时形成能最小,体系最稳定,之后体系的形成能随压力的增大而单调增大;随着压力的增大,导带向高能移动而价带向低能方向移动,体系费米能级上的态密度增大,各个态密度峰值降低且数目增多;光学参量峰值的位置与介电函数虚部的峰值位置很接近,随着压力增大,均向高能方向移动(蓝移),且峰值升高。 相似文献
526.
基于嫦娥一号高能粒子数据的地球磁层屏蔽效应研究 总被引:1,自引:0,他引:1
月球绕地球运行轨道约有1/4位于地球磁层内,因此,地球磁层是否会为月球轨道附近高能粒子提供足够的磁场屏蔽对于探索月球活动具有重要影响.嫦娥一号是中国首颗绕月人造卫星,其绕月飞行的工作轨道距离月球表面200 km.通过对嫦娥一号高能粒子探测器(HPD)的探测数据进行分析,比较了当月球位于地球磁层内外6个不同能道(能量范围4~400 MeV)时质子通量的变化,发现当月球位于地球磁层内时,这些能道的质子通量并没有发生显著减少,结果表明地球磁层不能为月球轨道附近高能粒子提供显著的磁屏蔽. 相似文献
527.
Y. Haba Y. Terashima H. Kunieda K. Ohsuga 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(1):174-179
We present the results of a systematic study of narrow-line Seyfert 1 galaxies (NLS1s) observed with XMM-Newton. The 2–12 keV X-ray spectra of NLS1s are well represented by a single power law with a photon index Γ ∼ 2. When this hard power law continuum is extrapolated into the low energy band, we found that all objects in our sample show prominent soft excess emission. This excess emission is well parameterized by the thermal emission expected from an optically thick accretion disk, and we found the following three peculiar features: (1) The derived disk temperatures are significantly higher than the expectation from a standard Shakura-Sunyaev accretion disk, if we assume a central mass of a black hole to be 106–8M⊙. (2) The temperatures are distributed within narrow range (ΔkT ∼ 0.08 keV) with an average temperature of 0.18 keV in spite of the range of four orders of magnitude in luminosity (1041–45 erg s−1). (3) We found a peculiar temperature–luminosity relation, where the luminosity seems to be almost saturated in spite of the significant change in temperature, during the observations of the most luminous NLS1 PKS 0558-504. These results strongly suggest that the standard accretion disk picture is no longer appropriate in the nuclei of NLS1s. We discuss a possible origin for the soft excess component, and suggest that a slim disk may be able to explain the observational results, if the photon trapping effect is properly taken into account. 相似文献
528.
S. Hayakawa 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,3(10-12)
X-ray astronomy satellite TENMA observed that the X-ray pulsation of Vela X-1 suddenly disappeared for tens of minutes. This phenomenon may be interpreted in terms of the eclipse by a planet of HD77581, the optical companion of Vela X-1. 相似文献
529.
综述现代工业工程主要特点、基本工作方法及其在QC小组活动中的运用,提出了质量管理与工业工程有机结合,能够控制成本并使工作方法达到最优化。介绍了一个工业工程在QC小组活动中的运用实例。 相似文献
530.
Peter H. Schultz Carolyn M. Ernst Jennifer L. B. Anderson 《Space Science Reviews》2005,117(1-2):207-239
The NASA Discovery Deep Impact mission involves a unique experiment designed to excavate pristine materials from below the
surface of comet. In July 2005, the Deep Impact (DI) spacecraft, will release a 360 kg probe that will collide with comet
9P/Tempel 1. This collision will excavate pristine materials from depth and produce a crater whose size and appearance will
provide fundamental insights into the nature and physical properties of the upper 20 to 40 m. Laboratory impact experiments
performed at the NASA Ames Vertical Gun Range at NASA Ames Research Center were designed to assess the range of possible outcomes
for a wide range of target types and impact angles. Although all experiments were performed under terrestrial gravity, key
scaling relations and processes allow first-order extrapolations to Tempel 1. If gravity-scaling relations apply (weakly bonded
particulate near-surface), the DI impact could create a crater 70 m to 140 m in diameter, depending on the scaling relation
applied. Smaller than expected craters can be attributed either to the effect of strength limiting crater growth or to collapse
of an unstable (deep) transient crater as a result of very high porosity and compressibility. Larger then expected craters
could indicate unusually low density (< 0.3 g cm−3) or backpressures from expanding vapor. Consequently, final crater size or depth may not uniquely establish the physical
nature of the upper 20 m of the comet. But the observed ejecta curtain angles and crater morphology will help resolve this
ambiguity. Moreover, the intensity and decay of the impact “flash” as observed from Earth, space probes, or the accompanying
DI flyby instruments should provide critical data that will further resolve ambiguities. 相似文献