从民歌看民族“文化上的共同心理素质”

川南汉族民歌《槐花几时开》和鄂西土家族民歌《高高山上一树槐》极度相似,或者本就是同一首民歌,应该是川南、鄂西两地所属的武陵地区各民族,因相同的自然环境、相同或相似的社会生产、生活方式,各民族长期较为稳定的杂居聚集、交流融合而产生的相同或相似的审美观,进而形成"文化上的共同心理素质"。     

高超声速飞行器跨流域气动力／热预测技术研究

分析了跨流域流动特点、工程背景需求、国内外研究现状,针对高超声速飞行器跨流域气动力／热预测存在的主要问题,从粘性干扰参数与克努森数搭接的跨流域模拟准则、微量天平结构优化及测力技术、红外大面积中低量值热流测量技术、流场显示与测量技术和 N-S／DSMC 自适应紧耦合数值模拟方法等方面,总结了近年来取得的研究进展,并讨论了下一步研究方向。     

深冷组合循环发动机吸气模态循环分析与设计可行域研究

为了研究类似SABRE3结构的深冷组合循环发动机,建立了基于部件法的发动机设计点热力学计算模型,提出了发动机氦循环新的循环效率和循环特征参数的定义。考虑发动机参数的物理限制条件及不同工质循环之间的相互影响,求解得到了空气路、氦气路重要参数的设计可行域。在可行域内开展了空气路和氦气路的循环分析,获到了冷却当量比、性能参数等主要参数的分布结果。结果表明:此发动机空气热功转换比ηt2为0.02～0.746。氦循环设计可行域受ηt2及换热器热负荷限制;循环起始温度和热负荷限制确定的情况下,ηt2越低氦循环可行域越窄。降低发动机冷却当量比的关键是:提高换热器1的氦出口温度以降低氦流量;当换热器1和换热器2的氦出口温度同时取得最大值时,冷却当量比取得最小值。换热器1和2的氦出口温度分别取1200K和1300K时,空气路可行域内冷却当量比为0.917～2.64。     

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.     

Longitudinal variation of the equatorial ionosphere: Modeling and experimental results

We describe a new version of the Parameterized Regional Ionospheric Model (PARIM) which has been modified to include the longitudinal dependences. This model has been reconstructed using multidimensional Fourier series. To validate PARIM results, the South America maps of critical frequencies for the E (foE) and F (foF2) regions were compared with the values calculated by Sheffield Plasmasphere-Ionosphere Model (SUPIM) and IRI representations. PARIM presents very good results, the general characteristics of both regions, mainly the presence of the equatorial ionization anomaly, were well reproduced for equinoctial conditions of solar minimum and maximum. The values of foF2 and hmF2 recorded over Jicamarca (12°S; 77°W; dip lat. 1°N; mag. declination 0.3°) and sites of the conjugate point equatorial experiment (COPEX) campaign Boa Vista (2.8°N; 60.7°W; dip lat. 11.4°; mag. declination −13.1°), Cachimbo (9.5°S; 54.8°W; dip lat. −1.8°; mag. declination −15.5°), and Campo Grande (20.4°S; 54.6°W; dip lat. −11.1°; mag. declination −14.0°) have been used in this work. foF2 calculated by PARIM show good agreement with the observations, except during morning over Boa Vista and midnight-morning over Campo Grande. Some discrepancies were also found for the F-region peak height (hmF2) near the geomagnetic equator during times of F₃ layer occurrences. IRI has underestimated both foF2 and hmF2 over equatorial and low latitude sectors during evening-nighttimes, except for Jicamarca where foF2 values were overestimated.     

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.     

Pro／E二次开发技术在卫星结构设计中的应用

为解决卫星协同设计过程中总体、结构信息同步滞后问题，基于Pro／E软件进行二次开发，实现对总体与结构接口文件的自动解析；利用解析出来的接口数据，在模型上进行表阵列的自动创建，使总体设计模型的变更能够在结构设计模型中及时得到反映，从而实现“总体一结构”设计结果的快速同步。文章中开发的软件工具，在多颗卫星的研制过程中得到了应用。     

单输入系统的最优闭环极点区域探讨

本文基于无限时域二次型性能指标的最优控制,讨论单输入线性定常系统闭环极点的分布区域问题。文中引入最优闭环极点区的概念,提出不等式寻优法和加权阵寻优法,并举例说明了两种方法在研究最优闭环极点区问题上的应用。     

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.