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).     

双后掠乘波体设计及性能优势分析

根据密切锥乘波体的设计几何关系,提出双后掠乘波体概念,给出了双后掠乘波体设计的参数与生成乘波体外形之间的关系。使用非均匀有理B样条(NURBS)表达包括圆和直线的激波出口型线辅助设计,研究了钝头区域可控、后掠区域可控的乘波体外形设计方法。使用CFD数值计算方法验证了设计方法的有效性,同时研究了双后掠乘波体外形的性能优势,结果表明在保持高超声速高性能的基础上适当设计外形在低速状态、纵向稳定性和涡效应增升方面具有性能优势,为大空域宽速域高超声速飞行器的研制开拓了新的途径。     

变循环发动机组合变几何调节方案

基于面向对象的设计思想,设计出了一个双涵道变循环发动机(VCE)的性能计算模型,并选取了双涵道VCE具有代表性的典型工作点,进行了双涵道VCE的组合变几何调节的相关研究.结果表明:在双涵道VCE的亚声速巡航和超声速巡航工作点,合理调节风扇导流叶片角度可以更大程度发挥双涵道VCE性能优势;在亚声速巡航工作点时选取的方案4和超声速巡航工作点时选取的方案4均比双涵道VCE设计点的变几何调节方案性能更优.     

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.     

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.     

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。     

Microphysics of Magnetic Reconnection

Magnetic reconnection is a universal phenomenon where energy is efficiently converted from the magnetic field to charged particles as a result of global magnetic topology changes during which earlier separated plasma regions become magnetically connected. While the reconnection affects large volumes in space most of the topology changes and of the energization occur within small localized regions. Regions of special importance are the X-region and the separatrix region. The understanding of the microphysics of these regions is crucial for the overall understanding of the reconnection. The Earth magnetosphere is the best environment where the details of these regions can be studied in situ. We summarize their main properties and discuss recent spacecraft observations.     

圆柱度误差最小区域评定方法述评

本文简介圆柱度误差评定的常用数学模型，并对用最小区域法评定圆柱度误差的几种近似方法及其优缺点展开讨论。