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991.
Numerical simulations of energy depositions in the middle and upper solar chromosphere result in ejection of chromospheric material into the corona and heating of the chromospheric gas. These simulations may be capable of describing some of the features seen by the soft X-ray telescope on board theYohkoh satellite. 相似文献
992.
Bhanu B. Das S. Symosek P. Snyder S. Roberts B. 《IEEE transactions on aerospace and electronic systems》1994,30(3):709-721
Range measurements to objects in the world relative to mobile platforms such as ground or air vehicles are critical for visually aided navigation and obstacle detection/avoidance. An approach is presented that consists of a synergistic combination of two types of passive ranging method: binocular stereo and motion stereo. We show a new way to model the errors in binocular and motion stereo in conjunction with an inertial navigation system (INS) and derive the appropriate Kalman filter to refine the estimates from these two stereo ranging techniques. We present results using laboratory images that show that refined estimates can be optimally combined to give range values which are more accurate than any one of the individual estimates from binocular and motion stereo. By incorporating a blending filter, the approach has the potential of providing accurate, dense range measurements for all the pixels in the field of view (FOV) 相似文献
993.
本文在稀颗粒群双流体简化模型下,采用算子分裂技术,综合应用高分辨率GRP格式,全二阶精度的FCT格式及预估校正格式,取三种不同粒相固壁边界条件,数值模拟了粉尘气体激波在刚性固壁上的正反射,确证了由理想平衡混合气体分析所预示的三类激波反射结构,给出了非平衡反射时波后流场的松弛特性,并评价了不同的粒相固壁边界条件假定的适用性。 相似文献
994.
企业经济效益综合评价与分级管理方法 总被引:1,自引:1,他引:1
本文针对财政部设计的企业经济效益评价指标体系,用多目标优化方法的思想对其进行优化处理,并且数理统计方法将各指标值折算成分数以符合人们的习惯;同时,用数理分析等方法将所得的评价序列进行分级归类管理。 相似文献
995.
996.
根据上限法原理建立了一种适用于分析变薄拉深的上限模型,包括两个用于优化上限解的独立参数。通过优化计算,变薄拉深力理论值与实验值吻合良好;用该模型研究了变薄拉深系数、凹模半锥角、原始筒形件内外径比、定径带相对长度以及内外摩擦因子等主要工艺参数对变薄拉深力的影响规律。 相似文献
997.
998.
We highlight the effect on space-telescope temperatures of thedirectionality of the radiative properties of materials, by showing results from a Monte-Carlo simulation of telescope cooling. The need for further measurements of directional properties is stressed. 相似文献
999.
As Ulysses moved inward and southward from mid-1992 to early 1994 we noticed the occasional occurrence of inter-events, lasting about 10 days and falling between the recurrent events, observed at proton energies of 0.48–97 MeV, associated with Corotating Interaction Regions (CIR). These inter-events were present for several sequences of two or more solar rotations at intensity levels around 1% of those of the neighbouring main events. When we compared the Ulysses events with those measured on IMP-8 at 1 AU we saw that the inter-events appeared at Ulysses after the extended emission (>10 days) of large fluxes of solar protons of the same energy that lasted at least one solar rotation at 1 AU. The inter-events fell completely within the rarefaction regions (dv/dt<0) of the recurrent solar wind streams. The interplanetary magnetic field (IMF) lines in the rarefactions map back to the narrow range of longitudes at the Sun which mark the eastern edge of the source region of the high speed stream. Thus the inter-events are propagating at mid-latitudes to Ulysses along field lines free from stream-stream interactions. They are seen in the 0.39–1.28 MeV/nucleon He, which exhibit a faster decay, but almost never in the 38–53 keV electrons. We show that the inter-events are unlikely to be accelerated by reverse shocks associated with the CIRs and that they are more likely to be accelerated by sequences of solar events and transported along the IMF in the rarefactions of the solar wind streams. 相似文献
1000.
M. Pick A. Buttighoffer A. Kerdraon T. P. Armstrong E. C. Roelof S. Hoang L. J. Lanzerotti G. M. Simnett J. Lemen 《Space Science Reviews》1995,72(1-2):315-320
A remarkable streaming beam-like particle event of 60 keV-5 MeV ions and of 38–315 keV electrons has been reported previously. This event has been associated with the passage of a Coronal Mass Ejection (CME) over the Ulysses spacecraft on June 9–13, 1993. At this time, the spacecraft was located at 4.6 AU from the sun and at an heliolatitude of 32° south. It was proposed (Armstrong et al., 1994) that the particle injection source could have been of coronal origin. In this study, we analyse the solar activity during this period. We identify a region of solar radio noise storms in the corona and in particular, a flare on June 7 that presents all the required characteristics to produce the hot plasma beam observed in the interplanetary medium. 相似文献