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41.
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
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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). 相似文献
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43.
A.O. Adewale E.O. Oyeyemi J. Olwendo 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
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 (F10.7) 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-F10.7 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 F10.7 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. 相似文献
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Y. Lin S.F. Martin O. Engvold L.H.M. Rouppe van der Voort M. van Noort 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
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. 相似文献
45.
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。 相似文献
46.
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. 相似文献
47.
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。 相似文献
48.
算术平均序列的收敛性 总被引:1,自引:0,他引:1
下述命题是熟知的:假设 {x_n)_(n=1)~∞是一数列且x_n=a 则1/n x_=a,并且我们知道它的逆命题是不真的。本文给出两个定理和两个推论,定理1断言S_n=1/nx_i 收敛于 a 和 b 的某种组合,这里 a 是(x_n)的子列极限,b 亦如此。在定理2中我们给出1/nx_i=0的一个充要条件,两个推论也是有趣的。 相似文献
49.
针对传统侦察星座目标单一、弹性低的问题,提出了多等级区域侦察弹性星座的设计方法。该方法将星座设计过程按区域等级信息分为多个子星座逐步设计,直到整体星座对所有的区域性能满足设计要求。以区域被划分为3个等级为例,首先对星座设计需求、设计指标及设计步骤进行了分析。其次推导了地面最低分辨率和轨道高度的关系并确定了不同子星座的轨道高度。最后考虑轨道倾角、一箭多星发射、光照和升交点漂移同步约束,构建基础星座、子星座1和子星座2的优化模型。最终设计星座为3层混合星座,共8个轨道面和70颗卫星,星座对各等级区域的最大重访时间分别为10937s,12241s和17437s,弹性指数为2213%,2420%和6361%。结果表明该方法设计的星座可实现对区域覆盖和弹性分级的设计要求,证明了方法的有效性。对比Walker星座设计方法,在同等设计要求下,Walker星座所需卫星数为156颗,多等级区域侦察弹性星座所需卫星数远低于Walker星座,结果进一步证明了该星座设计方法的优越性。 相似文献
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