Three classical Cepheid variable stars in the nuclear bulge of the Milky Way

The nuclear bulge is a region with a radius of about 200 parsecs around the centre of the Milky Way. It contains stars with ages ranging from a few million years to over a billion years, yet its star-formation history and the triggering process for star formation remain to be resolved. Recently, episodic star formation, powered by changes in the gas content, has been suggested. Classical Cepheid variable stars have pulsation periods that decrease with increasing age, so it is possible to probe the star-formation history on the basis of the distribution of their periods. Here we report the presence of three classical Cepheids in the nuclear bulge with pulsation periods of approximately 20?days, within 40 parsecs (projected distance) of the central black hole. No Cepheids with longer or shorter periods were found. We infer that there was a period about 25 million years ago, and possibly lasting until recently, in which star formation increased relative to the period of 30-70 million years ago.     

RR-Lyrae-type pulsations from a 0.26-solar-mass star in a binary system

RR Lyrae pulsating stars have been extensively used as tracers of old stellar populations for the purpose of determining the ages of galaxies, and as tools to measure distances to nearby galaxies. There was accordingly considerable interest when the RR Lyrae star OGLE-BLG-RRLYR-02792 (referred to here as RRLYR-02792) was found to be a member of an eclipsing binary system, because the mass of the pulsator (hitherto constrained only by models) could be unambiguously determined. Here we report that RRLYR-02792 has a mass of 0.26 solar masses M[symbol see text] and therefore cannot be a classical RR Lyrae star. Using models, we find that its properties are best explained by the evolution of a close binary system that started with M[symbol see text] and 0.8M[symbol see text]stars orbiting each other with an initial period of 2.9 days. Mass exchange over 5.4 billion years produced the observed system, which is now in a very short-lived phase where the physical properties of the pulsator happen to place it in the same instability strip of the Hertzsprung-Russell diagram as that occupied by RR Lyrae stars. We estimate that only 0.2 per cent of RR Lyrae stars may be contaminated by systems similar to this one, which implies that distances measured with RR Lyrae stars should not be significantly affected by these binary interlopers.     

A distance to the galaxy NGC4258 from observations of Cepheid variable stars

Cepheid variable stars pulsate in a way that is correlated with their intrinsic luminosity, making them useful as 'standard candles' for determining distances to galaxies; the potential systematic uncertainties in the resulting distances have been estimated to be only 8-10%. They have played a crucial role in establishing the extragalactic distance scale and hence the value of the Hubble constant. Here we report observations of Cepheids in the nearby galaxy NGC4258; the distance calculated from the Cepheids is 8.1 +/- 0.4 Mpc, where the uncertainty does not include possible systematic errors. There is an independently determined geometric distance to this galaxy of 7.2 +/- 0.5 Mpc, based on the observed proper motions of water masers orbiting the central black hole; the distances differ by 1.3sigma. If the maser-based distance is adopted and the Cepheid distance scale revised accordingly, the derived value of the Hubble constant would increase by 12 +/- 9%, while the expansion age of the Universe would decrease by the same amount.     

Direct detection of pulsations of the Cepheid star zeta Gem and an independent calibration of the period-luminosity relation

Cepheids are a class of variable (pulsating) stars whose absolute luminosities are related in a simple manner to their pulsational periods. By measuring the period and using the 'period-luminosity' relationship, astronomers can use the observed visual brightness to determine the distance to the star. Because these stars are very luminous, they can be observed in other galaxies, and therefore can be used to help determine the expansion rate of the Universe (the Hubble constant). Calibration of the period-luminosity relation is a necessary first step, but the small number of sufficiently nearby Cepheids has forced the use of a number of indirect means, with associated systematic uncertainties. Here we present a distance to the Cepheid zeta Geminorum, determined using a direct measurement (by an optical interferometer) of its changes in diameter as it pulsates. Within our uncertainty of 15 per cent, our distance is in agreement with previous indirect determinations. Planned improvements to the instrument will allow us to calibrate directly the period-luminosity relation to better than a few per cent.     

A 15.65-solar-mass black hole in an eclipsing binary in the nearby spiral galaxy M 33

Stellar-mass black holes are found in X-ray-emitting binary systems, where their mass can be determined from the dynamics of their companion stars. Models of stellar evolution have difficulty producing black holes in close binaries with masses more than ten times that of the Sun (>10; ref. 4), which is consistent with the fact that the most massive stellar black holes known so far all have masses within one standard deviation of 10. Here we report a mass of (15.65 +/- 1.45) for the black hole in the recently discovered system M 33 X-7, which is located in the nearby galaxy Messier 33 (M 33) and is the only known black hole that is in an eclipsing binary. To produce such a massive black hole, the progenitor star must have retained much of its outer envelope until after helium fusion in the core was completed. On the other hand, in order for the black hole to be in its present 3.45-day orbit about its (70.0 +/- 6.9) companion, there must have been a 'common envelope' phase of evolution in which a significant amount of mass was lost from the system. We find that the common envelope phase could not have occurred in M 33 X-7 unless the amount of mass lost from the progenitor during its evolution was an order of magnitude less than what is usually assumed in evolutionary models of massive stars.     

Discovery of two young brown dwarfs in an eclipsing binary system

Brown dwarfs are considered to be 'failed stars' in the sense that they are born with masses between the least massive stars (0.072 solar masses, M(o)) and the most massive planets (approximately 0.013M(o)); they therefore serve as a critical link in our understanding of the formation of both stars and planets. Even the most fundamental physical properties of brown dwarfs remain, however, largely unconstrained by direct measurement. Here we report the discovery of a brown-dwarf eclipsing binary system, in the Orion Nebula star-forming region, from which we obtain direct measurements of mass and radius for these newly formed brown dwarfs. Our mass measurements establish both objects as brown dwarfs, with masses of 0.054 +/- 0.005M(o) and 0.034 +/- 0.003M(o). At the same time, with radii relative to the Sun's of 0.669 +/- 0.034R(o) and 0.511 +/- 0.026R(o), these brown dwarfs are more akin to low-mass stars in size. Such large radii are generally consistent with theoretical predictions for young brown dwarfs in the earliest stages of gravitational contraction. Surprisingly, however, we find that the less-massive brown dwarf is the hotter of the pair; this result is contrary to the predictions of all current theoretical models of coeval brown dwarfs.     

剪切型结构动力模型物理参数模态识别方法及应用

提出结构动力模型物理参数的模态识别方法,它利用递归算法对结构进行解耦,只用是的１个或２个模态数据即可识别结构物理参数,利用这种民识别的物理参数考虑了结构各杆件、各楼层裼 动态耦合效应及柱轴向变形的影响。使简化模型更接近原始模型,从而提高了动力反应的计算精度,给出了具体工程应用实例。     

A test of general relativity from the three-dimensional orbital geometry of a binary pulsar.

Binary pulsars provide an excellent system for testing general relativity because of their intrinsic rotational stability and the precision with which radio observations can be used to determine their orbital dynamics. Measurements of the rate of orbital decay of two pulsars have been shown to be consistent with the emission of gravitational waves as predicted by general relativity, but independent verification was not possible. Such verification can in principle be obtained by determining the orbital inclination in a binary pulsar system using only classical geometrical constraints. This would permit a measurement of the expected retardation of the pulse signal arising from the general relativistic curvature of space-time in the vicinity of the companion object (the 'Shapiro delay'). Here we report high-precision radio observations of the binary millisecond pulsar PSR J0437-4715, which establish the three-dimensional structure of its orbit. We see the Shapiro delay predicted by general relativity, and we determine the mass of the neutron star and its white dwarf companion. The determination of such masses is necessary in order to understand the origin and evolution of neutron stars.     

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

The Hubble Deep Field provides one of the deepest multiwavelength views of the distant Universe and has led to the detection of thousands of galaxies seen throughout cosmic time. An early map of the Hubble Deep Field at a wavelength of 850?micrometres, which is sensitive to dust emission powered by star formation, revealed the brightest source in the field, dubbed HDF?850.1 (ref. 2). For more than a decade, and despite significant efforts, no counterpart was found at shorter wavelengths, and it was not possible to determine its redshift, size or mass. Here we report a redshift of z = 5.183 for HDF?850.1, from a millimetre-wave molecular line scan. This places HDF?850.1 in a galaxy overdensity at z?≈?5.2, corresponding to a cosmic age of only 1.1?billion years after the Big Bang. This redshift is significantly higher than earlier estimates and higher than those of most of the hundreds of submillimetre-bright galaxies identified so far. The source has a star-formation rate of 850 solar masses per year and is spatially resolved on scales of 5 kiloparsecs, with an implied dynamical mass of about 1.3?×?10(11) solar masses, a significant fraction of which is present in the form of molecular gas. Despite our accurate determination of redshift and position, a counterpart emitting starlight remains elusive.     

最优二元自正交码

构造一般二元自正交码是经典纠错码和量子纠错码研究的难点。研究基于并置二元循环矩阵的1-生成子拟循环码结构。以向量移位等价、线性码等价以及二元自正交码码字偶重量特点等为基础,设计特殊二元拟循环码结构,构造了28个最优或已知最优二元拟循环自正交码。提出自正交码截短-删除方法,构造出所获得自正交码的62个衍生码。文中的90个二元自正交码与文献[13]中最优或已知最优线性码比较,分别有67和23个二元自正交码是最优和已知最优。构造结果验证2个方法对一般二元自正交码构造的有效性,同时能较好解决量子纠错码构造中具有尽可能大对偶重量自正交码的设计问题。     

An unusually massive stellar black hole in the Galaxy.

The X-ray source known as GRS1915+105 belongs to a group dubbed 'microquasars'. These objects are binary systems which sporadically eject matter at speeds that appear superluminal, as is the case for some quasars. GRS1915+105 is also one of only two known binary sources thought to contain a maximally spinning black hole. Determining the basic parameters of GRS195+105, such as the masses of the components, will help us to understand jet formation in this system, as well as providing links to other objects which exhibit jets. Using X-ray data, indirect methods have previously been used to infer a variety of masses for the accreting compact object in the range 10-30 solar masses (M middle dot in circle). Here we report a direct measurement of the orbital period and mass function of GRS1915+105, which allow us to deduce a mass of 14 +/- 4 M middle dot in circle for the black hole. Black holes with masses >5-7 M middle dot in circle challenge the conventional picture of black-hole formation in binary systems. Based on the mass estimate, we interpret the distinct X-ray variability of GRS1915+105 as arising from instabilities in an accretion disk that is dominated by radiation pressure, and radiating near the Eddington limit (the point where radiation pressure supports matter against gravity). Also, the mass estimate constrains most models which relate observable X-ray properties to the spin of black holes in microquasars.     

中等年龄疏散星团NGC752中的QXAnd变星的测光研究

QxAnd变星是中等年龄疏散星团NGC752中的一个短周期的WUMa类型的相接双星．在2007年9月10日到12月25日期间,利用国家天文台兴隆85cm反射式望远镜对QXAnd变星进行B和V测光研究．我们得到了B和V两个波段的光变曲线;利用K—W方法定出光变极小时刻;通过经典的O—C方法得到QXAnd变星的周期P=4．12168117d和周期变化率dp／dt=1．89×10^-7d／a．     

基于后悔理论的区间二元语义多属性群决策方法

针对评价信息为区间语言变量的多属性群决策问题,提出了一种基于后悔理论的区间二元语义多属性群决策方法,该方法能够有效考虑决策者在决策过程中产生的一种风险规避,及其在后悔与欣喜之间存在的心理差异变化。首先,介绍关于区间二元语义信息的一些基本概念,并给出了区间二元语义均值与方差的定义;针对决策矩阵元素为区间二元语义变量属性权重部分未知的多属性群决策问题,利用区间二元语义的方差,通过构建优化模型确定最优属性权重,并提出了一种基于后悔理论的区间二元语义多属性群决策方法;最后将提出的方法应用至企业设计方案的选择中,结果与比较分析表明该方法具有一定可行性和有效性。     

A two-solar-mass neutron star measured using Shapiro delay

Neutron stars are composed of the densest form of matter known to exist in our Universe, the composition and properties of which are still theoretically uncertain. Measurements of the masses or radii of these objects can strongly constrain the neutron star matter equation of state and rule out theoretical models of their composition. The observed range of neutron star masses, however, has hitherto been too narrow to rule out many predictions of 'exotic' non-nucleonic components. The Shapiro delay is a general-relativistic increase in light travel time through the curved space-time near a massive body. For highly inclined (nearly edge-on) binary millisecond radio pulsar systems, this effect allows us to infer the masses of both the neutron star and its binary companion to high precision. Here we present radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature. We calculate the pulsar mass to be (1.97?±?0.04)M(⊙), which rules out almost all currently proposed hyperon or boson condensate equations of state (M(⊙), solar mass). Quark matter can support a star this massive only if the quarks are strongly interacting and are therefore not 'free' quarks.     

双星形成的非线性动力学机制和定性分析理论

 把星云的复杂的磁流体动力学方程,近似简化为只与速度相关的方程,则得到一个可解的简单模型.应用非线性方程的定性分析理论,获得双星演化的非线性动力学机制.在一定条件下,二维空间中的某些奇点相应于双星.而在别的条件下,奇点相应于单星.因此,各种星的形成是星云演化的结果.     

确定岩体渗透参数的结构面控制反演法

从裂隙渗流的基本运动方程出发,反求岩体的渗透参数是工程控制论中一类典型的偏微分方程分布参数控制反问题,对于这类反问题常用数值法求解．考虑到结构面控水特点,依据岩体渗透系数张量与结构面产状的基本关系式,提出了一种结构面控制反演法．该方法不仅可以反算出岩体的渗透系数张量,而且可以反求出岩体控水结构面的当量渗透系数、渗透系数张量的主值和主方向,同时应用该方法计算的解具有较好的唯一性．以溪洛渡水电站工程为例介绍了这种数值反演方法在确定岩体渗透参数中的应用．     

基于Hoek-Brown经验强度的滑移线理论体系

摘要滑移线理论是求解地基极限承载力、挡土墙土压力的理论基础,是以Mohr-Coulomb屈服准则建立的.本文考虑岩体的非线性破坏特性,参考Serrao的研究成果,基于Hoek-Brown经验强度,完善了适于完整、软弱、破碎等均质岩体的滑移线理论,从而为滑移线法求解岩基极限承载力和挡墙压力奠定了基础.     

勒庞与马克思的群体思想对我国群体性事件的启示

古斯塔夫.勒庞认为聚集在一起的群众是＂乌合之众＂,群众对于历史是被动的,是受众。而卡尔.马克思则认为历史是由人民大众经过长期努力创造的,并且肯定人民群众在社会中的作用,二者涉及到了一个共同问题———群体性事件。群体事件中存在严重的盲从现象且涉及多种社会矛盾,所以政府及相关部门应及时关注群众心理,以马克思主义的群体思想为指导,正确处理群体性事件。     

关于混沌动力系统Poincaré映射的分形维数

现代数值试验结果表明混沌动力系统的Poincare映射具有分形维数。然而,根据经典维数论Poincare映射根本不可能是分形的。为了解决这一现代数值试验和经典数学理论间的悖论,有必要对Poincare映射的现行定义进行修正。对此进行了若干探讨。     

云母双折射率色散关系不一致性对波片设计的影响—波片光相位延迟色散的补偿方法

云母体材料本身性质所决定的双折射率色散关系不一致性,对于波片设计是一个棘手的问题。与传统的样品普遍鉴别测量方法不同的是,该文试图从介绍分析双折射率的精确测量方法入手,通过必要的技术处理,达到直接采用单波长的测量结果代替多波长的测量结果,最终推断出任意波长或任意样品材料对应的波片相位延迟,此方法较之传统测量方式简捷快速实用,可满足云母波片系列化生产需要。