高前进比旋翼气动特性分析方法研究

提出一种前进比高达0.8的旋翼气动特性分析方法,该方法针对高前进比旋翼前行桨叶压缩性、后行桨叶失速效应严重以及桨叶偏流作用和反流区大的特点,建立了旋翼气动力模型以及与之相适应的旋翼诱导速度时变非均布模型与桨叶非定常挥舞运动模型,然后根据高前进比旋翼气动力、旋翼诱导速度和桨叶挥舞运动三者之间的内在耦合关系提出了高前进比旋翼气动特性的动态响应计算方法,最后以H-34旋翼为例计算了该旋翼高前进比状态的气动特性,并将计算结果与风洞试验数据进行对比验证,结果合理。     

由转速判断涡轮盘行波谐振

为找出液体火箭发动机涡轮盘疲劳裂纹故障产生的原因,对包含燃气在冲击式涡轮腔内形成的旋转激励与盘行波模态耦合谐振在内的盘的各种可能的耦合谐振进行了分析研究。在其它耦合谐振的可能性被排除后,将前者作为研究重点,并给出发生此种行波谐振的危险耦合转速范围计算公式。对某发动机大量热试转速数据作了分析,给出判断此类耦合谐振的判断依据。     

在地球极区无奇异的再入飞行器质心运动方程

传统的再入飞行器质心运动方程用经度和纬度描述地理位置，在南北极极点处奇异，在南北极区病态。本文提出利用位置矢量的三个方向余弦，称为“三余弦数”或“三元数”，代替经纬度，推导出无奇异再入质心运动方程。再入飞行器临近极点和到达极点的算例显示，使用三元数的无奇异再入方程完全避免了传统方程有关极点的奇异性。同时，无奇异方程所选状态变量与传统方程可进行很简便的转换。     

Analytical solutions for Earth discontinuous coverage of satellite constellation with repeating ground tracks

This paper presents an analytical model for calculating the Earth discontinuous coverage of satellite constellation with repeating ground tracks by integrating and extending the application of coverage region and route theory. Specifically, the visibility condition for a ground point is represented as a coverage region in the two-dimension map of visibility properties, and the trajectories of satellites with circular orbits and repeating ground tracks are converted to several inclined lines in t...     

日照边缘区域电离层对耀斑的响应特点研究

利用MSIS模型和背景太阳辐射谱模型,在一定大耀斑辐射谱假设的前提下,计算了耀斑期间日照边缘区域的电子产生率,分析了这一区域电离层电子密度的变化特点.结果表明,大耀斑期间在日照边缘区域,甚至大于太阳天顶角90°的区域都有明显的电子产生率的增加.从不同太阳天顶角处的电子产生率剖面的形态来看,随着天顶角的增加最大电离率减少,但高度增加.计算还显示了在太阳天顶角小于90°的区域内电子产生率的垂直分布有明显的双峰结构,这种结构对应着电离层的E区和F区,但在天顶角大于90°区域,F区的电子产生率要大得多.考虑到离子和电子的复合过程,这一区域的总电子含量的增加主要产生在高F区.      

一种平板螺旋式诱导轮的扬程计算法

目前平板螺旋式诱导轮的扬程计算法大都没有考虑诱导轮出口涡流区的影响,计算出的扬程和实际扬程有较大的偏差,涡流区的存在一方面会减小主流过流面积,使液流出口速度增大,损失增加,另一方面涡流运动自身也会消耗能量,使得诱导轮的扬程有所降低.以径向平衡理论为基础,考虑诱导轮出口涡流区的影响,提出一种扬程的修正计算法,用该方法对两种诱导轮进行了计算,计算结果和试验实测值比较接近,可以更准确的计算非空化工况下诱导轮的扬程.     

The Primordial Helium-4 Abundance from Observations of a Large Sample of Blue Compact Dwarf Galaxies

We use a sample of 45 low-metallicity H II regions in blue compact dwarf (BCD) galaxies to determine the primordial helium abundance YP with a precision better than 5%. We have carefully investigated the physical effects which may make the He I line intensities deviate from their recombination values such as collisional and fluorescent enhancements, underlying He I stellar absorption and absorption by Galactic interstellar Na I. By extrapolating the Y vs. O/H and Y vs. N/H linear regressions to O/H = N/H = 0, we obtain YP = 0.244±0.002 and 0.245±0.001, respectively, higher than previous determinations (YP = 0.230 - 0.234). Part of the difference comes from the fact that previous investigators have not taken into account underlying He I stellar absorption, especially in the NW component of the BCD I Zw 18 which, because of its extremely low metallicity plays a key role in the determination of YP. We derive a slope dY/dZ = 2.3±1.0, considerably smaller than those derived before. With this smaller slope and taking into account the errors, chemical evolution models with an outflow of well-mixed material can be built for star-forming dwarf galaxies which satisfy all the observational constraints. Our YP gives _bh ₅₀ ² = 0.058±0.007,f consistent with the lower limit set by dynamical measurements and X-ray observations of clusters of galaxies. It is also consistent, within the framework of standard big bang nucleosynthesis theory, with measurements of primordial 7Li in galactic halo stars and with the D/H abundance measured in absorption systems toward quasars by Burles and Tytler (1997).     

Solar activity dependence of total electron content derived from GPS observations over Mbarara

Vertical total electron content (VTEC) observed at Mbarara (geographic co-ordinates: 0.60°S, 30.74°E; geomagnetic coordinates: 10.22°S, 102.36°E), Uganda, for the period 2001–2009 have been used to study the diurnal, seasonal and solar activity variations. The daily values of the 10.7 cm radio flux (F_10.7) and sunspot number (R) were used to represent Solar Extreme Ultraviolet Variability (EUV). VTEC is generally higher during high solar activity period for all the seasons and increases from 0600 h LT and reaches its maximum value within 1400 h–1500 h LT. All analysed linear and quadratic fits demonstrate positive VTEC-F_10.7 and positive VTEC-R correlation, with all fits at 0000 h and 1400 h LT being significant with a confidence level of 95% when both linear and quadratic models are used. All the fits at 0600 h LT are insignificant with a confidence level of 95%. Generally, over Mbarara, quadratic fit shows that VTEC saturates during all seasons for F_10.7 more than 200 units and R more than 150 units. The result of this study can be used to improve the International Reference Ionosphere (IRI) prediction of TEC around the equatorial region of the African sector.     

On small active region filaments,fibrils and surges

High resolution Hα images and magnetograms (0.2 arc s) of an active region were obtained in alternating time series at 42 s cadences using the Swedish 1-m Solar Telescope on 2004 August 21. The Hα filtergrams reveal an active region filament and surges consisting of thread-like structures which have widths similar to the widths of chromospheric fibrils, both recorded down to the resolution limit in the best images. All observed structures in the active region appear highly dynamic. Fibrils show counterstreaming strongly resembling the counterstreaming threads in filaments.     

X线乳腺图像中微钙化检测的快速排除无病变区域法

介绍一种通过去除数字化乳腺x线照片中的无病变区域（TNR）间接地获取感兴趣区域（ROI）的方法。该方法可通过3个步骤来实现：（1）将图像划分为若干个不重合的相等大小块，并为每块计算5个特征；（2）通过域值法进行粗分析，排除肯定不含有病变的块；（3）使用代价敏感的支持向量分类器作更精细的分析，以进一步排除肯定不含有病变的块。在真实的数字化X线乳腺照片上的实验表明：该方法可以有效地去除高达81．71％的无病变区域。