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101.
102.
为实现对飞行器高热流密度热流的长时间测量,文章提出了一种以与高导热金属蜂窝材料复合的相变材料作为热沉的热流计,利用相变材料的潜热持续吸收热流计所接收的热量,可以对1 MW·m-2的热流密度持续测量2000 s以上。利用显热容数值方法建立了高热流密度长时间持续测量的分析模型,研究了热沉相变材料的热导率、相变温度、相变潜热等物性参数对测量方案的影响。研究结果表明,应选取热导率较大、相变温度较低且高于初始环境温度,以及相变潜热较大的相变材料作为长时间高热流密度测量的热沉材料。 相似文献
103.
在推进剂燃烧的建模上,传统的热力计算方法一般基于总焓守恒求解定压绝热燃烧温度和平衡组分,不能考虑壁面传热;在燃气流动的建模上,通常采用的冻结流模型认为本地的组分及热物理性质与燃烧室瞬时一致,忽略了这些参数因来流气体与本网格滞留气体掺混带来的随时间的缓变效应。提出了一种新颖的可以考虑壁面传热的基于总能量守恒的化学平衡流计算方法,运用Fortran2008语言,采用面向对象编程方法建立了化学平衡流燃气发生器管道的模块化仿真模型,并将该模型应用到一个包含42个组件的涡轮试验台气路系统的建模与仿真中。与早期模型仿真结果及试验数据的对比发现,新模型的仿真结果有一定改进,更加接近试验数据。 相似文献
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Hypervelocity impacts on the retrieved Hubble Space Telescope (HST) solar array was investigated by our extended Direct Simulation Monte Carlo (DSMC) model and the result matches well with the measured data in most of the particle mass range. The revelation of the altitude dependence of particles flux onto the retrieved surfaces provides some insight in understanding the observed higher flux onto Mir space station relative to that onto Long Duration Exposure Facility (LDEF). Our analysis suggests that a slightly higher primary flux onto Mir space station would be possible even without taking into account the secondary impacts, as a result of the existence of the highly eccentric orbits of small-sized debris. It is, furthermore, predicted that 43% of the measured impact flux onto Mir station in PIE experiment may be from secondary impacts, and a corresponding 7% for the detectors in Echantillions experiment. 相似文献
106.
蒲军平 《南京航空航天大学学报》2004,36(3):294-297
采用了一种高阶精度的Pade逼进的时间域上格栅取点的时间步积分的微分求积方法,对双质点系及梁在强迫力作用下的振动特性进行了数值分析。计算结果表明.这种方法具有明显的高精度及低耗时并且对于二阶初值问题是无条件稳定的。在所考虑的时域内的动力响应过程中,系统的总能量是守恒的。 相似文献
107.
Tong Xu Zhi Chen Chunbin Li Jian Wu Yanli Hu Zhensen Wu 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
The present paper describes the variations of the GPS total electron content (TEC) from the International GNSS service network and surface latent heat flux (SLHF) from the Scientific Computing Division of the National Center for Atmospheric Research (NCAR) before the 11 March 2011 M9.0 Sendai earthquake, respectively. The analysis shows pronounced enhancements in the GPS TEC and SLHF a few days prior to the earthquake event. The maximum increase in the GPS TEC was about 30 TECu with an extended spatial distribution on a geomagnetically quiet day (Dst ? −20 nT, between two moderate geomagnetic storms), 8 March, 3 days prior to the earthquake. This giant positive disturbance was possibly associated with the impending disastrous earthquake and contributed from the enhanced solar radiation. Moreover, there were several anomalous regions of SLHF on the global map, but an area of enhanced SLHF very close to the epicenter. The purpose of this paper is to report the existence of the changes in surface and ionosphere, and show the potential application of multi-source data to identify seismic precursors. 相似文献
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109.
王昆 《华北航天工业学院学报》2009,(4):26-27,47
本文主要叙述了LED作为新型光源与传统光源相比所具有的优势,以及目前各国将LED技术应用于照明、通讯等领域的突出优点,最后文章指出目前困扰我国LED技术发展的几点问题。 相似文献
110.
Pradip Kumar Bhuyan Saradi Bora 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
We investigated the diurnal, seasonal and latitudinal variations of ion density Ni over the Indian low and equatorial topside ionosphere within 17.5°S to 17.5°N magnetic latitudes by combining the data from SROSS C2 and ROCSAT 1 for the 9 year period from 1995 to 2003 during solar cycle 23. The diurnal maximum density is found in the local noon or in the afternoon hours and the minimum occurs in the pre sunrise hours. The density is higher during the equinoxes as compared to that in the June and December solstice. The local time spread of the daytime maximum ion density increases with increase in solar activity. A north south asymmetry with higher ion density over northern hemisphere in the June solstice and over southern hemisphere in December solstice has been observed in moderate and high solar activity years. The crest to crest distance increases with increase in solar flux. Ion density bears a nonlinear relationship with F10.7 cm solar flux and EUV flux in general. The density increases linearly with solar flux up to ∼150 sfu (1 sfu = 10−22Wm−2Hz−1) and EUV flux up to ∼50 units (109 photons cm−2 s−1). But beyond this the density saturates. Inverse saturation and linear relationship have been observed in some season or latitude also. Inter-comparison of the three solar activity indices F10.7 cm flux, EUV flux and F10.7P (= (F10.7 + F10.7A)/2, where F10.7A is the 81 day running average value of F10.7) shows that the ion density correlates better with F10.7P and F10.7 cm fluxes. The annual average daytime total ion density from 1995 to 2003 follows a hysteresis loop as the solar cycle reverses. The ion density at 500 km over the Indian longitude sector as obtained by the international reference ionosphere is in general lower than the measured densities during moderate and high solar activity years. In low solar activity years the model densities are equal or higher than measured densities. The IRI EIA peaks are symmetric (±10°) in equinox while densities are higher at 10°N in June solstice and at 10°S in the December solstice. The model density follows F10.7 linearly up to about F10.7 > ∼150 sfu and then saturates. 相似文献