弱s过程分量系数C2的研究

利用贫金属星中子俘获元素丰度的模型计算了30颗样品星的分量系数，并详细分析了弱s过程分量系数C     

恒星典型中子俘获元素丰度观测误差对分量系数的影响

根据贫金属星中子俘获元素丰度的计算模型，研究了典型中子俘获元素丰度的观测误差对代表各核合成过程相对贡献的分量系数的影响，给出了分量系数的变化范围。     

钡星重元素丰度的研究

提出了一种计算钡星重元素丰度的参数化模型,利用此模型很好地拟合了8颗钡星的重元素丰度,说明提出模型的有效性。对最佳拟合参数进行了比较和讨论,得到以下主要结论:强钡星的s-过程分量系数明显大于弱钡星的s-过程分量系数,强钡星和弱钡星的中子辐照量、重叠因子没有明显区别,它们的s-元素超丰程度不同主要是因为钡星系统轨道周期不同。     

弱电源侧稳态电压对称分量选相元件

针对输电线路弱馈侧母线稳态电压向量和故障点电压向量之间基本同向的特点，通过对输电线路各种短路故障情况下电压序分量关系的分析，提出了基于稳态电压序分量间相位关系和幅值关系的选相新原理．该原理所用的是电压稳态值，避免使用突变量，所以该选相元件可以在故障启动后整个过程都适用．该选相元件在选相过程中裕度角较大，有效地解决了弱电源侧的选相问题．EMTP仿真结果和动模试验表明，该选相元件能准确地选出故障相，完全能满足现场弱馈选相的要求．     

多余观测分量研究

为了对多余观测分量有较深入的了解，本文研究了在工程控制网中多余观测分量的形成过程，导出了多余观测分量与各条件式系数和观测权的关系。     

s+r星单辐照模型与对流模型参数的对比研究

将解释s r星元素丰度的单辐照和对流2种参数化模型的最佳拟合参数进行了对比,找出了这些参量的分布规律以及各参量之间的关系,得到了s-过程和r-过程核合成相关信息,进一步确定了s r星的主要形成机制.还对文献[13]做了有益的补充,给出了单辐照模型r-过程分量系数与s-过程分量系数之间的关系图.     

平行双回线路单回线不对称故障时提取故障分量的新方法

针对传统的只能在故障后2到3个周波提取故障分量的缺点,提出了单回线不对称故障在整个故障过程提取故障分量的新方法.该方法在平行双回线路的六序故障分量理论和单回线不对称故障复合序网图的基础上,根据同向网正、负序电流分布系数相等和反向网正、负序电流分布系数相等的特点,用正、负序电流反向量和负序电流同向量间接求得正序电流同向量的故障分量,进而合成得到每回线各相电流的故障分量.该方法不受负荷电流和电网参数波动的影响.PSASP和MATLAB仿真表明,通过该方法得到的故障分量同实际故障分量相同,而且可以长时间提取.     

基于双向二维加权主分量分析的面部表情识别

将二维主分量分析方法与加权的方法相结合,给出了一种双向二维加权主分量分析方法用于面部表情特征提取,该方法从水平和垂直两个方向对图像矩阵进行降维处理,大幅降低了所提取的特征数目;且考虑到面部不同部位包含不同的表情信息这一特点,对各个特征赋予不同的权重系数.经实验验证了该方法的有效性.     

方差分量估计和多余观测分量计算方法探讨

本文根据矩阵迹运算规则,对消去定向角未知数前后赫尔默特方差分量估计公式作了简化,简化后公式仍精确.本文还提出一种方差分量估计的近似方法.利用该法进行方差分量估计,其估值无偏.此外,本文还导出消去定向角未知数后多余观测分量计算公式.利用上述有关公式进行方差分量估计和多余观测分量计算,既能节省计算机内存,又能提高运算速度.     

基于DCT域直流分量的数字水印技术

在离散余弦变换 (DCT)域 ,人们通常将水印嵌入到交流 (AC)分量的中低频系数上 .近年来 ,有学者提出直流(DC)分量更适合于嵌入水印 .提出了一种水印算法 ,在DC分量上嵌入二值水印图像 ,水印的嵌入结合人眼视觉掩蔽特性 ;采用自适应水印编码方法增强了该算法的实用性 .实验结果表明 ,此方法产生的水印具有很好的不可见性和鲁棒性     

Superflares on solar-type stars

Solar flares are caused by the sudden release of magnetic energy stored near sunspots. They release 10(29) to 10(32)?ergs of energy on a timescale of hours. Similar flares have been observed on many stars, with larger 'superflares' seen on a variety of stars, some of which are rapidly rotating and some of which are of ordinary solar type. The small number of superflares observed on solar-type stars has hitherto precluded a detailed study of them. Here we report observations of 365 superflares, including some from slowly rotating solar-type stars, from about 83,000 stars observed over 120 days. Quasi-periodic brightness modulations observed in the solar-type stars suggest that they have much larger starspots than does the Sun. The maximum energy of the flare is not correlated with the stellar rotation period, but the data suggest that superflares occur more frequently on rapidly rotating stars. It has been proposed that hot Jupiters may be important in the generation of superflares on solar-type stars, but none have been discovered around the stars that we have studied, indicating that hot Jupiters associated with superflares are rare.     

Transiting extrasolar planetary candidates in the Galactic bulge

More than 200 extrasolar planets have been discovered around relatively nearby stars, primarily through the Doppler line shifts owing to reflex motions of their host stars, and more recently through transits of some planets across the faces of the host stars. The detection of planets with the shortest known periods, 1.2-2.5 days, has mainly resulted from transit surveys which have generally targeted stars more massive than 0.75 M(o), where M(o) is the mass of the Sun. Here we report the results from a planetary transit search performed in a rich stellar field towards the Galactic bulge. We discovered 16 candidates with orbital periods between 0.4 and 4.2 days, five of which orbit stars of masses in the range 0.44-0.75 M(o). In two cases, radial-velocity measurements support the planetary nature of the companions. Five candidates have orbital periods below 1.0 day, constituting a new class of ultra-short-period planets, which occur only around stars of less than 0.88 M(o). This indicates that those orbiting very close to more-luminous stars might be evaporatively destroyed or that jovian planets around stars of lower mass might migrate to smaller radii.     

Infall of gas as the formation mechanism of stars up to 20 times more massive than the Sun

Theory predicts and observations confirm that low-mass stars (like the Sun) in their early life grow by accreting gas from the surrounding material. But for stars approximately 10 times more massive than the Sun (approximately 10M(o)), the powerful stellar radiation is expected to inhibit accretion and thus limit the growth of their mass. Clearly, stars with masses >10M(o) exist, so there must be a way for them to form. The problem may be solved by non-spherical accretion, which allows some of the stellar photons to escape along the symmetry axis where the density is lower. The recent detection of rotating disks and toroids around very young massive stars has lent support to the idea that high-mass ( > 8M(o)) stars could form in this way. Here we report observations of an ammonia line towards a high-mass star forming region. We conclude that the gas is falling inwards towards a very young star of approximately 20M(o), in line with theoretical predictions of non-spherical accretion.     

The formation of a massive protostar through the disk accretion of gas

The formation of low-mass stars like our Sun can be explained by the gravitational collapse of a molecular cloud fragment into a protostellar core and the subsequent accretion of gas and dust from the surrounding interstellar medium. Theoretical considerations suggest that the radiation pressure from the protostar on the in-falling material may prevent the formation of stars above ten solar masses through this mechanism, although some calculations have claimed that stars up to 40 solar masses can in principle be formed via accretion through a disk. Given this uncertainty and the fact that most massive stars are born in dense clusters, it was suggested that high-mass stars are the result of the runaway merging of intermediate-mass stars. Here we report observations that clearly show a massive star being born from a large rotating accretion disk. The protostar has already assembled about 20 solar masses, and the accretion process is still going on. The gas reservoir of the circumstellar disk contains at least 100 solar masses of additional gas, providing sufficient fuel for substantial further growth of the forming star.     

Transiting circumbinary planets Kepler-34 b and Kepler-35 b

Most Sun-like stars in the Galaxy reside in gravitationally bound pairs of stars (binaries). Although long anticipated, the existence of a 'circumbinary planet' orbiting such a pair of normal stars was not definitively established until the discovery of the planet transiting (that is, passing in front of) Kepler-16. Questions remained, however, about the prevalence of circumbinary planets and their range of orbital and physical properties. Here we report two additional transiting circumbinary planets: Kepler-34 (AB)b and Kepler-35 (AB)b, referred to here as Kepler-34 b and Kepler-35 b, respectively. Each is a low-density gas-giant planet on an orbit closely aligned with that of its parent stars. Kepler-34 b orbits two Sun-like stars every 289?days, whereas Kepler-35 b orbits a pair of smaller stars (89% and 81% of the Sun's mass) every 131?days. The planets experience large multi-periodic variations in incident stellar radiation arising from the orbital motion of the stars. The observed rate of circumbinary planets in our sample implies that more than ～1% of close binary stars have giant planets in nearly coplanar orbits, yielding a Galactic population of at least several million.     

First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star

It has been proposed theoretically that the first generation of stars in the Universe (population III) would be as massive as 100 solar masses (100 M(O)), because of inefficient cooling of the precursor gas clouds. Recently, the most iron-deficient (but still carbon-rich) low-mass star--HE0107-5240--was discovered. If this is a population III star that gained its metals (elements heavier than helium) after its formation, it would challenge the theoretical picture of the formation of the first stars. Here we report that the patterns of elemental abundance in HE0107-5240 (and other extremely metal-poor stars) are in good accord with the nucleosynthesis that occurs in stars with masses of 20-130 M(O) when they become supernovae if, during the explosions, the ejecta undergo substantial mixing and fallback to form massive black holes. Such supernovae have been observed. The abundance patterns are not, however, consistent with enrichment by supernovae from stars in the range 130-300 M(O). We accordingly infer that the first-generation supernovae came mostly from explosions of approximately 20-130 M(O) stars; some of these produced iron-poor but carbon- and oxygen-rich ejecta. Low-mass second-generation stars, like HE0107-5240, could form because the carbon and oxygen provided pathways for the gas to cool.     

年轻类太阳星的测光研究

以X-ray亮度为标准,选取了16颗G型的年轻类太阳恒星进行了测光观测,并通过眦软件经行了测光处理,获得了9颗年轻类太阳恒星的自转周期.结合一些T Tauri型星、零龄主序恒星的自转周期,X-ray亮度得到自转较快的类太阳恒星与自转较慢的这些恒星比较,前者具有更强的X-ray辐射.但是,当恒星自转极快时,却并未发现自转和X-ray辐射强度之间的明显相关性.     

The age of the Milky Way inner halo

The Milky Way galaxy has several components, such as the bulge, disk and halo. Unravelling the assembly history of these stellar populations is often restricted because of difficulties in measuring accurate ages for low-mass, hydrogen-burning stars. Unlike these progenitors, white dwarf stars, the 'cinders' of stellar evolution, are remarkably simple objects and their fundamental properties can be measured with little ambiguity. Here I report observations of newly formed white dwarf stars in the halo of the Milky Way, and a separate analysis of archival data in the well studied 12.5-billion-year-old globular cluster Messier 4. I measure the mass distribution of the remnant stars and invert the stellar evolution process to develop a mathematical relation that links this final stellar mass to the mass of their immediate progenitors, and therefore to the age of the parent population. By applying this technique to a small sample of four nearby and kinematically confirmed halo white dwarf stars, I calculate the age of local field halo stars to be 11.4?±?0.7 billion years. The oldest globular clusters formed 13.5?billion years ago. Future observations of newly formed white dwarf stars in the halo could be used to reduce the uncertainty, and to probe relative differences between the formation times of the youngest globular clusters and the inner halo.     

基于伊巴谷数据分析的红团簇巨星的铁丰度

给出了１７颗红团簇巨星的观测资料,确定了这些样本得的恒星大气参数,得到了这些巨星的铁丰度,并且讨论了铁丰度与恒星大气参数的相关性,根据铁丰度与表面重力以及恒星质量和有效温度之间的相关性,可以将这类红团簇巨星细分为２类,一类质量较大,具有较大的表面重力和金属丰度,另一类贫金属星,其质量和表面重力都相对偏小。对每一类恒星,其质量和表面重力都随着有效温度的增高而线性增大。