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511.
软件缺陷管理是提高软件质量和软件开发效率的重要技术途径之一。基于地面测控系统中软件缺陷的基本概念,详细介绍地面测控软件缺陷管理的思想和方法,给出软件缺陷管理体系结构的分析和设计,并对软件缺陷管理在地面测控系统软件中应用实践情况进行总结和分析。指出软件缺陷管理系统应用的不足与需要解决的问题。实践中,软件缺陷管理系统对于提高团队开发效率和软件产品质量效果明显。 相似文献
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徐建艳 《运载火箭与返回技术》2007,28(3):40-43
帧格式同步是卫星原始数据地面处理前端的必经步骤。软件帧格式同步具有很好的灵活性,易于修改以适应各种情况的变化,缺点是处理速度较硬件慢。文章介绍了在软件帧格式同步程序设计中,应用各种查找表来提高处理速度,快速锁定同步字和还原帧数据的方法。经过实际应用验证,效果很好。 相似文献
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对卫星用掺铈玻璃型二次表面镜(SSM)的热控性能在空间辐照环境中的长期稳定性进行了研究。给出了经紫外、电子和质子模拟辐照试验后,导电和非导电掺传玻璃型二次表面镜热控性能的数据,并对其衰退机理进行了分析。结果表明,掺铈玻璃型二次表面镜的热控性能在地球同步轨道空间辐照环境中的长期稳定性可以满足卫星设计要求。 相似文献
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文章介绍了美国火星探测器降落伞系统组成和验证试验情况;分析了5种不同探测器降落伞系统的具体差异;归纳了探测器降落伞系统的结构和性能参数;重点介绍了“凤凰号”和“火星科学实验室”降落伞系统研制过程和性能验证试验。 相似文献
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Effect of temperature on corrosion behavior of 3003 aluminum alloy in ethylene glycol–water solution
The effect of temperature on the corrosion behavior of 3003 aluminum alloy in ethylene glycol–water solution was investigated by potentiodynamic polarization and electrochemical impedance spectroscopy(EIS) techniques. The surface characterization was observed and determined by scanning electron microscopy(SEM), atomic force microscopy(AFM) and energy dispersive spectrometer(EDS). The results demonstrate that the anodic aluminum dissolution and the cathodic oxygen reduction were accelerated by the increased temperature. However, as temperature was over60 °C, the solubility and concentration of oxygen decreased, resulting in the inhibition of cathodic reaction. The cathodic reaction rate of 3003 aluminum alloy rose to the maximum at 60 °C. The Warburg impedance in Nyquist diagram diminished and then was replaced by a negative capacitance caused by the absorption of intermediate corrosion product on electrode. On the other hand,after potentiodynamic measurements, 3003 aluminum alloy suffered pitting corrosion. The dissolution of aluminum alloy around secondary phase particles expanded both horizontally and vertically. 相似文献
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Emission heights of coronal bright points on Fe XII radiance map 总被引:1,自引:0,他引:1
H. Tian C.-Y. Tu J.-S. He E. Marsch 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2007,39(12):1853-1859
The study of coronal bright points (BPs) is important for understanding coronal heating and the origin of the solar wind. Previous studies indicated that coronal BPs have a highly significant tendency to coincide with magnetic neutral lines in the photosphere. Here we further studied the emission heights of the BPs above the photosphere in the bipolar magnetic loops that are apparently associated with them. As BPs are seen in projection against the disk their true emission heights are unknown. The correlation of the BP locations on the Fe XII radiance map from EIT with the magnetic field features (in particular neutral lines) was investigated in detail. The coronal magnetic field was determined by an extrapolation of the photospheric field (derived from 2-D magnetograms obtained from the Kitt Peak observatory) to different altitudes above the disk. It was found that most BPs sit on or near a photospheric neutral line, but that the emission occurs at a height of about 5 Mm. Some BPs, while being seen in projection, still seem to coincide with neutral lines, although their emission takes place at heights of more than 10 Mm. Such coincidences almost disappear for emissions above 20 Mm. We also projected the upper segments of the 3-D magnetic field lines above different heights, respectively, on to the tangent x–y plane, where x is in the east–west and y in the south–north direction. The shape of each BP was compared with the respective field-line segment nearby. This comparison suggests that most coronal BPs are actually located on the top of their associated magnetic loops. Finally, we calculated for each selected BP region the correlation coefficient between the Fe XII intensity enhancement and the horizontal component of the extrapolated magnetic field vector at the same x–y position in planes of different heights, respectively. We found that for almost all the BP regions we studied the correlation coefficient, with increasing height, increases to a maximal value and then decreases again. The height corresponding to this maximum was defined as the correlation height, which for most bright points was found to range below 20 Mm. 相似文献