全文获取类型
收费全文 | 703篇 |
免费 | 126篇 |
国内免费 | 179篇 |
专业分类
航空 | 521篇 |
航天技术 | 242篇 |
综合类 | 65篇 |
航天 | 180篇 |
出版年
2024年 | 1篇 |
2023年 | 11篇 |
2022年 | 20篇 |
2021年 | 35篇 |
2020年 | 41篇 |
2019年 | 35篇 |
2018年 | 40篇 |
2017年 | 27篇 |
2016年 | 40篇 |
2015年 | 48篇 |
2014年 | 37篇 |
2013年 | 47篇 |
2012年 | 56篇 |
2011年 | 67篇 |
2010年 | 62篇 |
2009年 | 55篇 |
2008年 | 73篇 |
2007年 | 55篇 |
2006年 | 56篇 |
2005年 | 40篇 |
2004年 | 22篇 |
2003年 | 23篇 |
2002年 | 17篇 |
2001年 | 11篇 |
2000年 | 9篇 |
1999年 | 17篇 |
1998年 | 11篇 |
1997年 | 3篇 |
1996年 | 8篇 |
1995年 | 14篇 |
1994年 | 6篇 |
1993年 | 3篇 |
1992年 | 3篇 |
1991年 | 3篇 |
1990年 | 4篇 |
1989年 | 4篇 |
1988年 | 2篇 |
1984年 | 2篇 |
排序方式: 共有1008条查询结果,搜索用时 15 毫秒
71.
为了建立电磁波在亚波长等离子体薄层中传播的物理数学模型,并针对通信频段的电磁波,研究电磁波在再入航天器表面等离子体薄层中的透射问题,相关研究成果可为再入航天器通信“黑障”现象研究提供理论基础。模型从麦克斯韦方程组出发,采用微分薄层法进行数值求解,获得了不同等离子体密度条件下亚波长等离子体中目标电磁波的透射特性及传播规律,揭示了截止反射效应和碰撞吸收效应在其中发挥的作用。本研究对于深入了解亚波长碰撞等离子体薄层中电磁波的传播过程具有意义。 相似文献
72.
飞翼布局飞行器等离子体激励滚转操控试验 总被引:2,自引:0,他引:2
飞翼布局飞行器采用多个气动舵面共同作用来控制飞行,常规气动舵面的结构复杂,在大迎角时由于流动分离,舵面操纵效率显著降低。等离子体激励器具有结构简单、重量轻和响应快等优势,常被用在流动控制上。本文利用激励器抑制单侧翼面流动分离产生不对称的气动力,对飞翼布局飞行器滚转通道的控制进行了试验研究,得出了激励器在飞行器上的最优布置位置和最佳控制参数,并和常规副翼舵面滚转操控效果进行了对比。结果表明:布置于内翼、中翼前缘的等离子体激励器能够获得最佳的滚转控制效果;激励器调制频率对飞行器滚转控制效果的影响较大,而激励电压对滚转控制效果的影响较小;与常规副翼相比,等离子体激励器在大迎角时对滚转通道的操控效果优于副翼。 相似文献
73.
Vladimir Pines Marianna ZlatkowskiArnon Chait 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
In this paper we study the charging process of small grain particles by anisotropic multi-component solar wind plasmas (electrons, protons and heavy ions), versus two-component (electron/proton) plasmas. We are focusing attention on the important characteristics of the charging process, namely the charging time, floating potential and current content as functions of plasma parameters such as He++/H+ (α/p) number density and Tα/Tp temperature ratios of alpha particles to protons, as well as plasma streaming velocity v0. Measured statistical properties of solar wind plasma parameters at 1 AU show considerable variations in α/p-temperature ratios from 1 to 10, in α/p-number density ratio from 0.01 to 0.35, as well as in values of streaming velocity v0 from 200 km/s to 1000 km/s and more. Periods of these variations could last for several days each, leading to significant variability in the charging process, according to newly derived general analytical expressions. Numerical calculations performed for protons/alphas plasmas showed large disparity in the charging characteristics. For example, in anisotropic plasma, grain charging time varies up to 90% depending on α/p-particles temperature and number density ratios, whereas changes in floating potential are up to 40%. In contrast, in isotropic plasma, charging characteristic for grains do not change very much for the same plasma parameters variations, with charging time varying about 12% and floating potential only varying about 4%. It is also shown that in highly anisotropic plasma, with all ballistic electrons and ions, dust grains could not hold their charges, and characteristic discharged time is calculated. We note that the analysis is equally applicable to any sized body immersed in solar wind plasma. 相似文献
74.
Vladimir Pines Marianna ZlatkowskiArnon Chait 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
We present a general self-consistent kinetic theory for plasma sheath formation in solar wind plasma. The theory could be applied to anisotropic, as well as to isotropic collisionless plasma without resorting to any simplifications, limitations, or assumptions, such as the necessary existence of a ‘pre-sheath’ region of ions acceleration to ensure the Bohm criterion. The kinetic framework is first applied to sheath formation around an arbitrary oriented planar absorbing surface, charged by solar wind anisotropic plasma, under the condition of negligible photoelectric effect. We then make use of our kinetic approach for the plane geometry in isotropic collisionless plasma, as a particular case of a planar electrode orientation parallel to plasma streaming velocity, also analyzing the sheath structure around spherical and cylindrical absorbing electrodes submerged in isotropic collisionless plasma. Obtained results demonstrate principal differences in spatial charge distributions in sheath regions between spherical or cylindrical electrodes of large size and an unbound planar surface submerged in isotropic plasma. In the case of a planar electrode, we directly compare results obtained in our kinetic and hydrodynamic theories and conventional hydrodynamic theory of plasma sheath formation. The outcome from the present study have direct implications to the analysis of plasma sheath structure and associated distribution in space of charged dust grains, which is relevant to the moon exploration near the optical terminator region or in shadowed craters in the moon. 相似文献
75.
在Г.М.古尼耶夫中值老化公式的基础上,采用回归分析方法对碳纤维/环氧树脂基复合材料的实验室模拟加速腐蚀与自然大气腐蚀之间的相关性进行研究,确定了自然大气环境腐蚀试验的层间剪切强度的中值曲线方程,并得出实验室模拟加速腐蚀与自然大气环境腐蚀之间的当量关系.试样表面及断口微观形貌的观察分析进一步证明:实验室模拟加速腐蚀与自然大气环境腐蚀具有相似的腐蚀机理. 相似文献
76.
77.
78.
为了能够将脉冲等离子体推力器成功地运用于空间,需对其羽流进行研究。将一维 MHD双温放电模型的计算结果作为入口条件,运用DSMC(Direct Simulation Monte\|Carlo )/PIC(Particle in Cell)流体混合算法一体化模拟实验室PPT羽流。验证计算显示该模 型具有一体化模拟脉冲等离子体推力器羽流的能力。对不同初始放电能量下的羽流场进行模 拟,给出了离子、中性粒子、电子温度、轴线上质量流率和出口平面返流质量流率的变化情 况。计算结果显示高放电能量下返流量更大,同时中性粒子在返流中所占比例也越大。
相似文献
相似文献
79.
为了探讨非平衡等离子体对甲烷点火和火焰传播速度影响,采用化学动力学模型GRI-Mech3.0,利用零维、均质、完全混合模型和火焰传播速度模型,对甲烷点火过程和火焰传播过程进行数值模拟,计算得到了非平衡等离子体生成自由基(O自由基和NOX自由基)对甲烷点火延迟时间和火焰传播速度的影响规律。结果表明:当分别加入0.5% O和0.5% NOX活性基时,点火延迟时间减少了约94.7%,63.1%(加入NO)和94.2%(加入NO2)。通过反应路径分析和敏感度分析,揭示了非平衡等离子体生成自由基影响甲烷点火和火焰传播速度的化学反应机理。 相似文献
80.
Pedro Corona-Romero Americo Gonzalez-Esparza 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
We present an analytic model of a stationary bow shock which describes the interaction between a supermagnetosonic ambient wind and an obstacle with spherical-like frontal shape. We develop expressions for the bow shock’s geometry and the physical properties of the plasma sheath as functions of the upstream conditions. The solution is limited to magnetic fields parallel to the upstream velocity. The model allows to use any value of the upstream alfvenic and sonic Mach numbers and the polytropic index (γ), pointing out the influence of γ for the magnetosheath compression and the bow shock shape. When both Mach numbers are small, the upstream magnetic field intensity affects also the bow shock shape. We compare our results with other models finding important consistencies. We also compare our results with in-situ data, we fund a reasonable qualitative agreement; however, it seems that our model underestimates the magnetosheath size. 相似文献