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451.
This paper describes experimental research into the initiation and propagation of rotating detonation for liquid Nitrogen TetrOxide (NTO) and liquid MonoMethylHydrazine (MMH). An annular rocket-type combustor without nozzle was designed to investigate detonation combustion. The propellants were injected through unlike impingement injectors. The combustion flame fronts and pressure waves were detected using optical diagnostics and dynamic pressure sensors, respectively. The propagation of rotating detonation was established spontaneously by increasing the mass flow rate of propellants. The velocity of propagation of the flame fronts and pressure waves was nearly equal and reaches supersonic speed. Two different detonation combustion patterns are present, single wave mode and double waves mode. And in double waves mode, the two detonation waves are always counter-rotating. The possibility of rotating detonation initiation in a combustor with nozzle was also checked. Stable rotating detonation can be initialized and sustained at similar operating conditions. 相似文献
452.
David G. Sibeck R. Allen H. Aryan D. Bodewits P. Brandt G. Branduardi-Raymont G. Brown J. A. Carter Y. M. Collado-Vega M. R. Collier H. K. Connor T. E. Cravens Y. Ezoe M.-C. Fok M. Galeazzi O. Gutynska M. Holmström S.-Y. Hsieh K. Ishikawa D. Koutroumpa K. D. Kuntz M. Leutenegger Y. Miyoshi F. S. Porter M. E. Purucker A. M. Read J. Raeder I. P. Robertson A. A. Samsonov S. Sembay S. L. Snowden N. E. Thomas R. von Steiger B. M. Walsh S. Wing 《Space Science Reviews》2018,214(4):79
Both heliophysics and planetary physics seek to understand the complex nature of the solar wind’s interaction with solar system obstacles like Earth’s magnetosphere, the ionospheres of Venus and Mars, and comets. Studies with this objective are frequently conducted with the help of single or multipoint in situ electromagnetic field and particle observations, guided by the predictions of both local and global numerical simulations, and placed in context by observations from far and extreme ultraviolet (FUV, EUV), hard X-ray, and energetic neutral atom imagers (ENA). Each proposed interaction mechanism (e.g., steady or transient magnetic reconnection, local or global magnetic reconnection, ion pick-up, or the Kelvin-Helmholtz instability) generates diagnostic plasma density structures. The significance of each mechanism to the overall interaction (as measured in terms of atmospheric/ionospheric loss at comets, Venus, and Mars or global magnetospheric/ionospheric convection at Earth) remains to be determined but can be evaluated on the basis of how often the density signatures that it generates are observed as a function of solar wind conditions. This paper reviews efforts to image the diagnostic plasma density structures in the soft (low energy, 0.1–2.0 keV) X-rays produced when high charge state solar wind ions exchange electrons with the exospheric neutrals surrounding solar system obstacles.The introduction notes that theory, local, and global simulations predict the characteristics of plasma boundaries such the bow shock and magnetopause (including location, density gradient, and motion) and regions such as the magnetosheath (including density and width) as a function of location, solar wind conditions, and the particular mechanism operating. In situ measurements confirm the existence of time- and spatial-dependent plasma density structures like the bow shock, magnetosheath, and magnetopause/ionopause at Venus, Mars, comets, and the Earth. However, in situ measurements rarely suffice to determine the global extent of these density structures or their global variation as a function of solar wind conditions, except in the form of empirical studies based on observations from many different times and solar wind conditions. Remote sensing observations provide global information about auroral ovals (FUV and hard X-ray), the terrestrial plasmasphere (EUV), and the terrestrial ring current (ENA). ENA instruments with low energy thresholds (\(\sim1~\mbox{keV}\)) have recently been used to obtain important information concerning the magnetosheaths of Venus, Mars, and the Earth. Recent technological developments make these magnetosheaths valuable potential targets for high-cadence wide-field-of-view soft X-ray imagers.Section 2 describes proposed dayside interaction mechanisms, including reconnection, the Kelvin-Helmholtz instability, and other processes in greater detail with an emphasis on the plasma density structures that they generate. It focuses upon the questions that remain as yet unanswered, such as the significance of each proposed interaction mode, which can be determined from its occurrence pattern as a function of location and solar wind conditions. Section 3 outlines the physics underlying the charge exchange generation of soft X-rays. Section 4 lists the background sources (helium focusing cone, planetary, and cosmic) of soft X-rays from which the charge exchange emissions generated by solar wind exchange must be distinguished. With the help of simulations employing state-of-the-art magnetohydrodynamic models for the solar wind-magnetosphere interaction, models for Earth’s exosphere, and knowledge concerning these background emissions, Sect. 5 demonstrates that boundaries and regions such as the bow shock, magnetosheath, magnetopause, and cusps can readily be identified in images of charge exchange emissions. Section 6 reviews observations by (generally narrow) field of view (FOV) astrophysical telescopes that confirm the presence of these emissions at the intensities predicted by the simulations. Section 7 describes the design of a notional wide FOV “lobster-eye” telescope capable of imaging the global interactions and shows how it might be used to extract information concerning the global interaction of the solar wind with solar system obstacles. The conclusion outlines prospects for missions employing such wide FOV imagers. 相似文献
453.
超声速化学非平衡流动的数值模拟一直是计算流体力学领域的难点,主要体现在如下几个方面:物理过程非常复杂,存在着激波、燃烧波等各种复杂波系的相互作用;超声速化学非平衡流动属于典型的时空多尺度物理问题,其控制方程存在严重的刚性,给数值求解带来了很大困难。对国内外的解耦算法研究现状简单综述后,主要介绍1993年刘君提出的解耦算法的理论基础,流动方程采用冻结流模型,源项方程模拟流体微团在当地绝热、定容的热力学系统内发生的化学反应过程。通过引入两个中间变量,即等效内能和等效比热比,将与温度无关的生成焓从流动方程组能量项中分离出去,源项方程组中包含等效内能,使用不同算子对流动方程和源项方程解耦求解。与传统解耦算法相比,源项方程的求解过程中包含状态参数和组元同时变化。结合刘君解耦算法机理和有限体积法空间平均特性,介绍近期在提高算法计算效率方面的研究进展,包括流动方程优化算法和耦合过程优化。采用优化算法对经典的激波诱导燃烧算例进行数值模拟,与不同文献结果进行对比,验证了优化算法的时空精度。通过总结经验发现化学非平衡反应仅发生在流场局部区域,提出质量生成率判据,结合相应模拟结果验证了方法的可行性,可以进一步提高化学反应算子的计算效率。 相似文献
454.
大量残存太空的空间垃圾对在轨运行航天器的安全构成严重威胁,对其进行主动移除已迫在眉睫。火箭末级、失效卫星等非合作目标已失去姿态调整能力,且长期在失控状态下运行,受太阳光压、重力梯度等摄动力矩及失效前自身残余角动量等因素的影响往往会出现翻滚运动。对翻滚非合作目标直接捕获存在碰撞风险,为降低风险系数采取消旋后再捕获是较为合适的方式。在对火箭末级、失效卫星等典型非合作目标运动形式及消旋过程进行分析的基础上,综述了目前国内外所提出的接触式及非接触式消旋方法,并对非合作目标翻滚运动测量及动力学参数辨识和消旋控制这两项消旋共性关键技术进行了归纳总结。本综述将为中国空间碎片主动清除技术的发展提供有益参考。 相似文献
455.
为深入了解真实航空发动机内燃烧流场,采用动态亚网格模型结合单步快速化学反应(FC)、火焰面(FLM)及反应进度变量(FPV)等三种燃烧模型对径向两级反向旋流燃烧室单头部构型进行了大涡模拟。为避免模型简化误差,对燃烧室包括全部气膜冷却孔在内的精细结构进行了完全仿真。在已达到统计定常状态的冷态流场基础上首先模拟了燃料喷注和掺混过程,约2.6ms后燃料到达真实的点火位置,随后采用FPV模型在半径3mm的球形区域数值模拟了点火,展示了在主燃孔横向射流作用下初始火焰沿化学恰当比混合分数等值线传播并充满整个火焰筒的发展过程,结果显示火焰到达燃烧室出口的耗时约为6~7ms。不同模型算法预测的平均温度场与CARS测量结果作了对比,LES-FPV,RANS-FPV,LES-FLM以及参考文献中RANS-FLM计算平均误差分别为3.47%,4.17%,7.76%和11.22%,表明LES改进了模拟精度,且FPV模型显著优于FLM模型。RANS-FPV预测的出口存在严重热斑,导致其给出的出口温度分布因子(OTDF)及最大径向温度分布因子(RTDF)值分别达到0.593和0.313;LES-FPV结果均匀性最好,其预测值分别为0.284和0.193。 相似文献
456.
457.
458.
为研究甲烷添加对RP-3航空煤油燃烧特性的影响,在定容燃烧弹中获得初始温度420K,初始压力0.1MPa,当量比0.8~1.5和甲烷含量0~0.8工况下CH_4/RP-3航空煤油混合燃料火焰发展特性图片、火焰半径扩散速率、拉伸火焰传播速度、马克斯坦长度、无拉伸火焰传播速度和层流燃烧速度等燃烧特性,并分析了甲烷添加对混合燃料马克斯坦长度及层流燃烧速度等的影响。结果表明,CH_4/RP-3航空煤油混合燃料在当量比1.3,甲烷含量0工况时燃烧稳定性较差,但随着混合燃料中甲烷含量的增加,火焰前锋面逐渐趋于稳定;混合燃料当量比分别为0.8,1.0和1.2时,甲烷含量的增加对火焰半径扩散速率和拉伸火焰传播速度分别起促进、无明显影响和抑制作用;混合燃料马克斯坦长度曲线在当量比0.9~1.2交叉,当量比为0.8时,混合燃料马克斯坦长度随甲烷含量增加而减小,而当量比为1.3时,混合燃料马克斯坦长度接近于0,燃烧变得极不稳定;混合燃料层流燃烧速度峰值出现在当量比1.0~1.1内,当量比在0.9~1.1,甲烷添加对RP-3航空煤油层流燃烧速度影响较小,当量比大于1.1时,混合燃料层流燃烧速度随甲烷含量增加显著减低。 相似文献
459.
460.
叶盘结构趋于轻薄,盘片耦合振动不能忽略。本文旨在揭示缘板阻尼器对叶盘不同节径模态减振性能的影响规律。建立了考虑缘板转动的叶盘-缘板阻尼器集中参数模型,采用结合解析雅可比矩阵的多阶谐波平衡法求解稳态响应,利用非线性周期减缩技术,在不损失精度的情况下使计算效率提高至少3倍以上。研究结果表明,针对叶片主导的一阶弯曲模态,缘板阻尼器总体上对节径数越高的模态阻尼效果越好,但在盘片耦合区阻尼效果显著下降,约为25%至50%;此外,忽略缘板的转动效应可能导致对阻尼器减振效果高估约70%至100%。 相似文献