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261.
针对新型航空发动机管路连接副,研究了其在安装过程和松动过程中的接触特性。首先,将连接副的安装-松动过程划分为3个阶段,并对这3个阶段的摩擦力和接触压力进行了解析推导,分析了摩擦力和接触压力的变化规律。然后,建立了管路连接副的轴对称有限元模型,并对其进行了非线性瞬态分析。最后,基于施加位移载荷的方法模拟了连接副的安装和松动过程,研究了接触面的滑移量、接触压力、摩擦力和接触压应力的变化规律。同时研究了不同预紧力对连接副接触压应力的影响。结果表明:松动过程在滑移点前后可以分为2个阶段,这2个阶段中接触面的接触特性有明显区别;连接副接触面的接触特性只与接触面参数和预紧力大小相关,与管径、材料等其他因素无关。本文研究的安装与松动过程中接触特性变化规律在工程上可以指导新型管路连接副的设计工作。 相似文献
262.
温储备系统是冷储备与热储备系统的推广,在实际中有广泛应用。针对不可修温储备系统的可靠性建模问题,已有基于多值决策图(MDD)的系统可靠性建模方法。该方法以系统中的单元故障为建模对象,分别构建故障级MDD与系统级MDD,进而获得系统可靠度的解析表达式。然而,该表达式中不同维度积分相互混杂,计算给定时刻的系统可靠度需要首先梳理系统可靠度的表达式,以利用数值方法求解其中的积分。为实现系统可靠度的程序化计算,在已有研究基础上提出将系统级MDD按故障数分解为一系列子决策图,通过对MDD中边的概率重新赋值获得每一子决策图的发生概率,得到系统可靠度的规范形式,形成一套完整的系统可靠度计算方法。 相似文献
263.
利于减少配平损失的太阳能飞机构型设计 总被引:2,自引:1,他引:2
针对具有静稳定性的太阳能飞机一般采用尾翼配平造成气动配平损失的问题,提出了一种“T”构型太阳能飞机。概述该太阳能飞机的总体构型,分析该构型飞机巡航状态下降低重心的自配平原理,建立能量平衡和质量分析模型,给出适合于该构型太阳能飞机的概念设计方法,并优化构型设计参数。结果表明,“T”构型太阳能飞机不仅具有静稳定性,还降低了配平损失。在巡航状态下,“T”构型太阳能飞机单位面积平飞需用功率比常规构型太阳能飞机减少了6.2%,具有明显的应用效果。 相似文献
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266.
精密单点定位(PPP)时间比对数据会受到观测噪声的影响,因此对时间比对数据进行消噪是一项重要工作。提出一种基于经验模分解(EMD)的PPP时间比对数据消噪方法,并将该方法与Vondrak滤波方法的消噪效果进行对比。结果表明,两种方法的消噪效果相当,均能有效滤除PPP时间比对数据中的随机噪声,明显改善时间比对的稳定度。 相似文献
267.
S. M. Krimigis D. G. Mitchell D. C. Hamilton S. Livi J. Dandouras S. Jaskulek T. P. Armstrong J. D. Boldt A. F. Cheng G. Gloeckler J. R. Hayes K. C. Hsieh W.-H. Ip E. P. Keath E. Kirsch N. Krupp L. J. Lanzerotti R. Lundgren B. H. Mauk R. W. McEntire E. C. Roelof C. E. Schlemm B. E. Tossman B. Wilken D. J. Williams 《Space Science Reviews》2004,114(1-4):233-329
The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R
S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm2 sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm2 sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm2 sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm2 sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R
S every 2–3 h (every ∼10 min from ∼20 R
S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date. 相似文献
268.
Geiss J. Bühler F. Cerutti H. Eberhardt P. Filleux Ch. Meister J. Signer P. 《Space Science Reviews》2004,110(3-4):307-335
Space Science Reviews - The Apollo Solar Wind Composition (SWC) experiment was designed to measure elemental and isotopic abundances of the light noble gases in the solar wind, and to investigate... 相似文献
269.
Louise M. Prockter Rosaly M. C. Lopes Bernd Giese Ralf Jaumann Ralph D. Lorenz Robert T. Pappalardo Gerald W. Patterson Peter C. Thomas Elizabeth P. Turtle Roland J. Wagner 《Space Science Reviews》2010,153(1-4):63-111
The surfaces of the Solar System’s icy satellites show an extraordinary variety of morphological features, which bear witness to exchange processes between the surface and subsurface. In this paper we review the characteristics of surface features on the moons of Jupiter, Saturn, Uranus and Neptune. Using data from spacecraft missions, we discuss the detailed morphology, size, and topography of cryovolcanic, tectonic, aeolian, fluvial, and impact features of both large moons and smaller satellites. 相似文献
270.
本文以我们在文献[1~4]中提出的“AP/HTPB/Al”推进剂燃烧模型为基础,首先讨论了催化剂作用部位与推进剂燃速、压力指数变化的关系,然后引入一个催化剂作用因子B.并以二茂铁系列催化剂为例,对模型中的几个与二茂铁催化剂作用部位相连系的反应动力学参数作“催化作用因子”校正,计算研究了四种二茂铁催化剂用量对燃速、压力指数的影响规律.计算结果与实验符合得很好,相对误差均小于±10%,证明本文提出的模拟计算方法具有较高的可靠性. 相似文献