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1.
证明了最小二乘直线函数是一种严格的凸函数。F(a,b)=∑(y-ax_i-b)~2是一个椭圆抛物面。a=[n∑x_iy_i-∑x_i∑y_i]/[n∑x_i^2-(∑x_i)~2]和b=[∑x_i^2∑y_i-∑x_i∑x_i∑y_i]/[n∑x_i^2-(∑x_i)~2]仅表示极值点。a=∑x_iy_i/∑x_i和 b=[∑x_i^2∑y_i-∑x_i∑x_iy_i]/[n∑x_i^2]在某些情况下可以是极值点,但不是在每种情况下都是极值点。 相似文献
2.
《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2007,39(5):661-667
Monthly median values of foF2, hmF2 and M(3000)F2 parameters, with hourly time interval resolution for the diurnal variation, obtained with DPS-4 digisonde observations at Hainan (19.4°N, 109.0°E) are used to study the low latitude ionospheric variation behavior. The observational results are compared with the International Reference Ionospheric Model (IRI) predictions. The time period coverage of the data used for the present study is from March 2002 to February 2005. Our present study showed that: (1) In general, IRI predictions using CCIR and URSI coefficients follow well the diurnal and seasonal variation patterns of the experimental values of foF2. However, CCIR foF2 and URSI foF2 IRI predictions systematically underestimate the observed results during most time period of the day, with the percentage difference ΔfoF2 (%) values changing between about −5% and −25%, whereas for a few hours around pre-sunrise, the IRI predictions generally overestimate the observational ones with ΔfoF2 (%) sometimes reaching as large as ∼30%. The agreement between the IRI results and the observational ones is better for the year 2002 than for the other years. The best agreement between the IRI results and the observational ones is obtained in summer when using URSI coefficients, with the seasonal average values of ΔfoF2 (%) being within the limits of ±10%. (2) In general, the IRI predicted hmF2 values using CCIR M(3000)F2 option shows a poor agreement with the observational results. However, when using the measured M(3000)F2 as input, the diurnal variation pattern of hmF2 given by IRI2001 has a much better agreement with the observational one with the detailed fine structures including the pre-sunrise and post-sunset peaks reproduced reasonably well. The agreement between the IRI predicted hmF2 values using CCIR M(30,000)F2 option and the observational ones is worst for the afternoon to post-midnight hours for the high solar activity year 2002. During daytime hours the agreement between the hmF2 values obtained with CCIR M(30,000)F2 option and the observational ones is best for summer season. The discrepancy between the observational hmF2 and that obtained with CCIR M(30,000)F2 option stem from the CCIR M(3000)F2 model, which does not produce the small scale structures observed in the measured M(3000)F2. 相似文献
3.
数据采集系统的总体评价 总被引:5,自引:0,他引:5
从性能指标出发,综述了数据采集系统总结评价技术的发展状况。并提出了对数据采集系统性能指标的两类分类方法 。 相似文献
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尺寸参数对气动液阀启动特性的影响 总被引:1,自引:0,他引:1
为气动液阀的启动过程建立了数学模型,分析了尺寸参数对该阀启动特性的影响。计算结果表明:在保证必要的工作寿命的前提下,适当地增大控制腔气孔的直径或增大靠近控制腔的活塞端面直径有利于提高该阀的响应能力。本文所得的结论有利于此类阀门的设计。 相似文献
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空间遥控作业系统的自适应无源控制 总被引:15,自引:2,他引:15
遥控作业系统是实现空间危险环境中作业的有力手段。由于空间工作站和地面控制站之间的通讯时延,造成了遥控作业系统的不稳定和操作性能的降低。本文利用二端口网络理论,提出了可定量评价系统操作性能的指标函数,并导出操作性能最优(临场感状态)的无源控制算法,同时针对环境的不确定性,给出参数自调节的自适应无源控制器的结构。实验验证了本文提出的无源控制算法的有效性 相似文献
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一种综合性能与寿命数据的Bayes-Bootstrap方法 总被引:1,自引:0,他引:1
对现代长寿命、高可靠产品进行可靠性评估,传统大样本寿命试验和统计推断方法存在很大困难,包括伪寿命数据方法在内的性能与寿命数据综合的可靠性评估方法也存在很多问题。提出了将性能可靠性建模与Bayes方法相结合的方式解决这一困难问题,其中对性能试验数据建立性能退化模型,并利用Bootstrap方法处理伪寿命数据导致的随机性误差和构造融合Bayes验前分布,然后利用Bayes验后分析进行可靠性统计推断。对随机斜率模型和长寿命卫星动量轮轴承组件润滑寿命的应用表明,提出的方法可以充分利用产品研制、使用过程中各种类型的信息,特别是性能试验信息,具有一定的适用性。 相似文献
10.
We describe work that has recently been completed on deriving the fundamental parameters of eight WR stars through the photoionization modelling of their surrounding nebulae using non-LTE WR flux distributions. The resulting effective temperatures range from 57 000–71 000 K for the WN4-5 stars and <30 000–42 000 K for the WN6-8 stars. The derived stellar parameters are compared with those obtained from stellar emission line modelling. We find good agreement for the hot early WN stars, indicating that the non-LTE WR flux distributions have essentially the correct shape in the crucial far-UV region. We find lower temperatures for the four cooler late WN stars, particularly for the two WN6 stars. For the nebulae surrounding these stars, we find that the model flux distributions produce too much nebular ionization. We suggest that these discrepancies arise because of the lack of line-blanketing in the WR atmospheres. For the WO1 central star of G2.4+1.4, with strong nebular He II 4686 A emission, we derive a temperature of 105 000 K, somewhat less than previous estimates. The positions of our eight WR stars on the H-R diagram are compared with the evolutionary tracks of Maeder (1990) for solar metallicity. In common with previous workers, we find that our derived luminosities are too low, giving an initial mass range of 25–40 M, below that expected for the majority of WR stars. 相似文献