广西天峨坪金矿区金银次生晕异常分布地质意义与金银表生地球化学性质差异分析

广西天峨坪金矿区多被土壤覆盖,区内局部出露轻变质粉砂岩及碳酸盐岩。为了圈定深部金矿体及了解金银表生地球化学行为,系统分析了区内土壤、原生晕及半风化原生晕金银元素含量。天峨坪金矿异常区金银次生晕异常分离,银次生晕异常中心分布于矿区中北部地势较高地区,而金次生晕异常中心却分布于矿区中南部较低洼地区,Au/Ag比从原生晕、半风化原生晕至全风化土壤逐渐降低。根据金银在不同风化程度岩石中的比值变化,结合金银在碳酸盐岩出露区地表流体中金比银更易形成金硫络合物迁移,提出在碳酸盐岩出露区地表中至弱碱性流体中金比银更易发生迁移,银次生晕异常中心指示深部金矿体。后经工程验证发现Ag的次生晕异常中心对应深部金矿体,而金异常中心偏离深部矿体。成果表明,碳酸盐岩出露区金银表生地球化学行为有差异,热带亚热带植被覆盖区次生晕找金过程中,不但要注意金的次生晕异常,也要注意银的次生晕异常。     

太阳附近α-元素的星系化学演化

利用银河系的三成份(即晕、厚盘和薄盘)及多相(气体，分子云，大、小质量恒星以及剩余物质)的化学演化模型，通过观测约束，对α-元素(O，Mg，Si，S和Ca)的化学演化进行了计算，得到这些元素的丰度分布随金属丰度的变化规律；同时将计算曲线与丰度观测结果进行了比较；并对理论结果进行了讨论。     

银河系形成新说

据英国New Scientist1992年9月19日报道,美国耶鲁大学的李养吾在分析研究核球内靠近银心处,内银晕中距银心比距太阳为近以及外银晕中的天琴座RR型变星时发现,三处天琴RR星的金属(比氦重的元素)含量不同,核球内的为太阳的1/10,内银晕中的为太阳的1/20,而外银晕中的只有太阳的1/40。天文学家早就知道,银河系核球的金属含量比银晕的金属含量多得多,但李养吾认为,仅此理由不足以说明上述现象。他相信,星龄大小在此也起作用,其根据是赫罗图“水平枝”上星的颜色受两个因素的制约:其金属含量和年龄。因此,如果天     

五百年来谁著史

主权货币与外贸凭证1567年，明穆宗朱载晕隆庆元年，明帝国开放“银禁”与“海禁”，通俗地说：这等于把帝国“央行”从北京搬到了托美矿山。道光年间，中国国库银先是因国际金融投机、继之以战败赔款出现大规模外流之际，《海国图志》的作者魏源在《军储篇》中就曾这样提醒国人说：“今人只知中国之银出漏于外洋，而不知白昔中国之银大半来于外洋也”；魏源明确地将白银的大规模进口，     

星系中心大黑洞的宇宙学演化

在冷暗物质晕等级成团宇宙学模型中,伴随着暗物质晕并合,星系中心黑洞也断地并合和增长.于展Press-Schechter公式（EPS）我们编写了一自适应时间长Monte Carlo程序,重构了表征暗物质晕等级成团并合树.在成功地建立了黑洞和暗物质晕宇宙学演化模型后,我们通过引入直接吸积（包标准薄盘吸积和磁流体力学吸积）和随吸积两类黑洞吸积模式,论了黑洞自旋和质量宇宙学演化.通过与观测到AGN光度函数比较,我们发现黑洞通过磁流体力学吸积模式增长,与观测符合最好.于以上理论框架,我们还研究了双大质量黑洞演化,发现双黑洞通过共转气体吸积盘吸积对双黑洞质量比分存在显著影响.     

皖南西坑银矿床稳定同位素研究

本文研究了西坑银矿床的硫、铅、氢、氧稳定同位素．结合矿床地质特征，认为西坑银矿床成矿物质主要来源于地层，成矿热液为演化的大气降水与岩浆水的混合水．     

考虑时间延迟后较重r-过程元素的化学演化

考虑有效产生r-过程(快中子俘获过程)元素的Ⅱ型超新星延迟爆发的因素,大体上经过10次大质量Ⅱ型超新星(M>35 M⊙)先爆发后,产生r-过程元素的Ⅱ型超新星(M=(28～35) M⊙)才开始爆发. 从星系化学演化角度看,r-过程元素的主要来源为较大质量Ⅱ型超新星(M=(28～35) M⊙). Ⅱ型超新星占Ⅱ型超新星总数的4%.核合成区域内种子核和中子源主要来自恒星自身的核反应.经计算得到星系晕中较重的r-过程元素Eu,Ba,Ce,La,Nd,Pr,Sm等元素丰度的离散情况及其化学演化.     

浙东地区银铅锌矿床菱锰矿的形成与银的矿化关系初探

通过对浙东地区 银铅锌矿床的地质特征，菱锰矿的矿物学特征及锰，银的成矿地球化学特征的分析，结合该区矿床中成矿物理化学条件的研究成果，指出：尽管菱锰矿与银矿物紧密伴（共）生，但菱锰矿并非银的载体矿物，菱锰矿与银矿物的相伴产出主要是作为银金属矿床的相似性及菱锰矿的形成加速了自然银的析出等因素所造成的。     

银超微粒扩散中的孤立波拢动

以银超微粒为例提出了一个描述超微粒自发演化的“扩散提获．反应．凝聚”的模型,建立了它的演化动力学方程,同时求得了演化动力学方程的孤立破解,并对解作了较详细讨论．     

从序列到演化──天体演化学的重要研究方法

提出了从序列到演化方法是天体演化学的一种重要的研究方法．笔者认为该方法不仅适用于天体演化学领域研究天体演化问题，而且可以移植、推广到地质演化学、生物进化论等领域研究地质演化、生物进化等问题．     

Direct detection of a microlens in the Milky Way.

The nature of dark matter remains mysterious, with luminous material accounting for at most approximately 25 per cent of the baryons in the Universe. We accordingly undertook a survey looking for the microlensing of stars in the Large Magellanic Cloud (LMC) to determine the fraction of Galactic dark matter contained in massive compact halo objects (MACHOs). The presence of the dark matter would be revealed by gravitational lensing of the light from an LMC star as the foreground dark matter moves across the line of sight. The duration of the lensing event is the key observable parameter, but gives non-unique solutions when attempting to estimate the mass, distance and transverse velocity of the lens. The survey results to date indicate that between 8 and 50 per cent of the baryonic mass of the Galactic halo is in the form of MACHOs (ref. 3), but removing the degeneracy by identifying a lensing object would tighten the constraints on the mass in MACHOs. Here we report a direct image of a microlens, revealing it to be a nearby low-mass star in the disk of the Milky Way. This is consistent with the expected frequency of nearby stars acting as lenses, and demonstrates a direct determination of a lens mass from a microlensing event. Complete solutions such as this for halo microlensing events will probe directly the nature of the MACHOs.     

A high-velocity black hole on a Galactic-halo orbit in the solar neighbourhood

Only a few of the dozen or so known stellar-mass black holes have been observed away from the plane of the Galaxy. Those few could have been ejected from the plane as a result of a 'kick' received during a supernova explosion, or they could be remnants of the population of massive stars formed in the early stages of evolution of the Galaxy. Determining their orbital motion should help to distinguish between these options. Here we report the transverse motion (in the plane of the sky) for the black-hole X-ray nova XTE J1118+480 (refs 2, 3, 4, 5), from which we derive a large space velocity. This X-ray binary system has an eccentric orbit around the Galactic Centre, like most objects in the halo of the Galaxy, such as ancient stars and globular clusters. The properties of the system suggest that its age is comparable to or greater than the age of the Galactic disk. Only an extraordinary 'kick' from a supernova could have launched the black hole into an orbit like this from a birthplace in the disk of the Galaxy.     

Earth-mass dark-matter haloes as the first structures in the early Universe

The Universe was nearly smooth and homogeneous before a redshift of z = 100, about 20 million years after the Big Bang. After this epoch, the tiny fluctuations imprinted upon the matter distribution during the initial expansion began to collapse because of gravity. The properties of these fluctuations depend on the unknown nature of dark matter, the determination of which is one of the biggest challenges in present-day science. Here we report supercomputer simulations of the concordance cosmological model, which assumes neutralino dark matter (at present the preferred candidate), and find that the first objects to form are numerous Earth-mass dark-matter haloes about as large as the Solar System. They are stable against gravitational disruption, even within the central regions of the Milky Way. We expect over 10(15) to survive within the Galactic halo, with one passing through the Solar System every few thousand years. The nearest structures should be among the brightest sources of gamma-rays (from particle-particle annihilation).     

Observation of interstellar lithium in the low-metallicity Small Magellanic Cloud

The primordial abundances of light elements produced in the standard theory of Big Bang nucleosynthesis (BBN) depend only on the cosmic ratio of baryons to photons, a quantity inferred from observations of the microwave background. The predicted primordial (7)Li abundance is four times that measured in the atmospheres of Galactic halo stars. This discrepancy could be caused by modification of surface lithium abundances during the stars' lifetimes or by physics beyond the Standard Model that affects early nucleosynthesis. The lithium abundance of low-metallicity gas provides an alternative constraint on the primordial abundance and cosmic evolution of lithium that is not susceptible to the in situ modifications that may affect stellar atmospheres. Here we report observations of interstellar (7)Li in the low-metallicity gas of the Small Magellanic Cloud, a nearby galaxy with a quarter the Sun's metallicity. The present-day (7)Li abundance of the Small Magellanic Cloud is nearly equal to the BBN predictions, severely constraining the amount of possible subsequent enrichment of the gas by stellar and cosmic-ray nucleosynthesis. Our measurements can be reconciled with standard BBN with an extremely fine-tuned depletion of stellar Li with metallicity. They are also consistent with non-standard BBN.     

The Galactic population components and their structural parameter values

The Galactic population components and their structural parameter values have been analyzed using the data of three-color photometry and modem starcounts calibrated recently in the seven Baset fietds M67U, SA51, SA71, SA82, SA94, SA107 and NGC6171. It is an important part of studying the Galactic structure all-sidedly and constructing a unique Galactic model.     

The U/Th production ratio and the age of the Milky Way from meteorites and Galactic halo stars

Some heavy elements (with atomic number A > 69) are produced by the 'rapid' (r)-process of nucleosynthesis, where lighter elements are bombarded with a massive flux of neutrons. Although this is characteristic of supernovae and neutron star mergers, uncertainties in where the r-process occurs persist because stellar models are too crude to allow precise quantification of this phenomenon. As a result, there are many uncertainties and assumptions in the models used to calculate the production ratios of actinides (like uranium-238 and thorium-232). Current estimates of the U/Th production ratio range from approximately 0.4 to 0.7. Here I show that the U/Th abundance ratio in meteorites can be used, in conjunction with observations of low-metallicity stars in the halo of the Milky Way, to determine the U/Th production ratio very precisely (0.57(+0.037)(-0.031). This value can be used in future studies to constrain the possible nuclear mass formulae used in r-process calculations, to help determine the source of Galactic cosmic rays, and to date circumstellar grains. I also estimate the age of the Milky Way (14.5(+2.8)(-2.2)Gyr in a way that is independent of the uncertainties associated with fluctuations in the microwave background or models of stellar evolution.     

Deuterium in the Galactic Centre as a result of recent infall of low-metallicity gas

The Galactic Centre is the most active and heavily processed region of the Milky Way, so it can be used as a stringent test for the abundance of deuterium (a sensitive indicator of conditions in the first 1,000 seconds in the life of the Universe). As deuterium is destroyed in stellar interiors, chemical evolution models predict that its Galactic Centre abundance relative to hydrogen is D/H = 5 x 10(-12), unless there is a continuous source of deuterium from relatively primordial (low-metallicity) gas. Here we report the detection of deuterium (in the molecule DCN) in a molecular cloud only 10 parsecs from the Galactic Centre. Our data, when combined with a model of molecular abundances, indicate that D/H = (1.7 +/- 0.3) x 10(-6), five orders of magnitude larger than the predictions of evolutionary models with no continuous source of deuterium. The most probable explanation is recent infall of relatively unprocessed metal-poor gas into the Galactic Centre (at the rate inferred by Wakker). Our measured D/H is nine times less than the local interstellar value, and the lowest D/H observed in the Galaxy. We conclude that the observed Galactic Centre deuterium is cosmological, with an abundance reduced by stellar processing and mixing, and that there is no significant Galactic source of deuterium.     

Clumps and streams in the local dark matter distribution

In cold dark matter cosmological models, structures form and grow through the merging of smaller units. Numerical simulations have shown that such merging is incomplete; the inner cores of haloes survive and orbit as 'subhaloes' within their hosts. Here we report a simulation that resolves such substructure even in the very inner regions of the Galactic halo. We find hundreds of very concentrated dark matter clumps surviving near the solar circle, as well as numerous cold streams. The simulation also reveals the fractal nature of dark matter clustering: isolated haloes and subhaloes contain the same relative amount of substructure and both have cusped inner density profiles. The inner mass and phase-space densities of subhaloes match those of recently discovered faint, dark-matter-dominated dwarf satellite galaxies, and the overall amount of substructure can explain the anomalous flux ratios seen in strong gravitational lenses. Subhaloes boost gamma-ray production from dark matter annihilation by factors of 4 to 15 relative to smooth galactic models. Local cosmic ray production is also enhanced, typically by a factor of 1.4 but by a factor of more than 10 in one per cent of locations lying sufficiently close to a large subhalo. (These estimates assume that the gravitational effects of baryons on dark matter substructure are small.).     

Active galactic nuclei as scaled-up Galactic black holes

A long-standing question is whether active galactic nuclei (AGN) vary like Galactic black hole systems when appropriately scaled up by mass. If so, we can then determine how AGN should behave on cosmological timescales by studying the brighter and much faster varying Galactic systems. As X-ray emission is produced very close to the black holes, it provides one of the best diagnostics of their behaviour. A characteristic timescale--which potentially could tell us about the mass of the black hole--is found in the X-ray variations from both AGN and Galactic black holes, but whether it is physically meaningful to compare the two has been questioned. Here we report that, after correcting for variations in the accretion rate, the timescales can be physically linked, revealing that the accretion process is exactly the same for small and large black holes. Strong support for this linkage comes, perhaps surprisingly, from the permitted optical emission lines in AGN whose widths (in both broad-line AGN and narrow-emission-line Seyfert 1 galaxies) correlate strongly with the characteristic X-ray timescale, exactly as expected from the AGN black hole masses and accretion rates. So AGN really are just scaled-up Galactic black holes.     

An asymmetric distribution of positrons in the Galactic disk revealed by gamma-rays

Gamma-ray line radiation at 511 keV is the signature of electron-positron annihilation. Such radiation has been known for 30 years to come from the general direction of the Galactic Centre, but the origin of the positrons has remained a mystery. Stellar nucleosynthesis, accreting compact objects, and even the annihilation of exotic dark-matter particles have all been suggested. Here we report a distinct asymmetry in the 511-keV line emission coming from the inner Galactic disk ( approximately 10-50 degrees from the Galactic Centre). This asymmetry resembles an asymmetry in the distribution of low mass X-ray binaries with strong emission at photon energies >20 keV ('hard' LMXBs), indicating that they may be the dominant origin of the positrons. Although it had long been suspected that electron-positron pair plasmas may exist in X-ray binaries, it was not evident that many of the positrons could escape to lose energy and ultimately annihilate with electrons in the interstellar medium and thus lead to the emission of a narrow 511-keV line. For these models, our result implies that up to a few times 10(41) positrons escape per second from a typical hard LMXB. Positron production at this level from hard LMXBs in the Galactic bulge would reduce (and possibly eliminate) the need for more exotic explanations, such as those involving dark matter.