X射线吸收谱在宝石学研究中的应用

许多宝玉石的颜色成因都与致色元素的电子结构和局域环境相关.X射线吸收谱(XAS)是一种探测物质结构的有力工具,能够识别吸收原子的局域结构和化学环境,如价态、配位数、键长等.本文以红宝石、金绿宝石、翡翠和象牙等为例,简要介绍同步辐射XAS技术在宝石研究中的应用和优势.     

高压消解-石墨炉原子吸收测定近海生物样品中的铅、镉

采用高压消解-石墨炉原子吸收测定近海生物样品中的铅、镉,探讨了硝酸+过氧化氢不同配比,消解时间的选择,以及准确度、精密度和检出限试验。通过对国家一级标准物质及实际样品进行方法验证,结果表明该分析方法的准确度好,精密度高,检出限达到规范要求,实际样品加标回收率在90%~105%,测试结果准确可靠,能满足近海生物样品的测试要求。     

AAS次灵敏吸收线测定高银物料中银

研究了利用银次灵敏线338.28nm测定高银物料中银的含量,克服了用银的灵敏线328.08nm测定高含量银的不足,采用冶金部标准物质铅精矿YT88011,锌精矿ZnS-02分析验证,测定结果与标准值吻合。方法精密度(RSD,n=10)为0.5%~1.5%。该方法适用于各种含铅高银物料和含银量高达1%~10%的铅阳极泥及需要大称样量的粗铅中银的测定。     

The extremely intense CNA events observed at Zhongshan Station in July, 2000

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SELECTION OF BRILLOUIN SHIFT DISCRIMINATOR FOR BRILLOUIN LIDAR

For the measurement of vertical profiles of sound speed in the sea using laser excited Brillouin scattering, a high-resolution measurement of Brillouin frequency shift is required. In this work, a molecular absorption cell was selected as the frequency shift discriminator and several kinds of absorption gases were tried. It was found that the strong line ( # 1095) of ^127 I2 at 18783. 3297 cm^-1 and two absorption lines of ^129 I2 located at the two sides of the # 1095 line of ^127 I2 could be used as frequency shift discriminator to detect the changes of the Brillouin frequency shift. This selection is the best one within the range from 532.0131 run to 532.5154 nm. But it is not perfect and there is a lot of work to do before its practical application.     

Tracking the shadows through GMRT

The structures of faint high redshift galaxies cannot be observed directly. But if a luminous quasar is located farther along their line of sight, high resolution absorption lines offer a valuable and reliable probe to their structure. GMRT is suited to monitor the absorption spectra, if the redshifted neutral hydrogen or OH doublet fall in one of the windows of the telescope. We present the OH doublet absorption spectra for the system B0218+357, taken at GMRT this year at resolution of approx. 9.5 km/sec with an rms noise of the order of 1 mJy. Based on our study of the OH doublet and 21cm neutral hydrogen line we infer that, in the lensing spiral galaxy of B0218 + 357, neutral hydrogen and OH coexist in tenous clouds and there is possibly a hole in the central part of the galaxy. In contrast, the gas is seen in high density clouds in the lens in an otherwise similar system PKS1830-211.     

Semi-analytic approach to understanding the distribution of neutral hydrogen in the Universe

Analytic derivations of the correlation function and the column density distribution for neutral hydrogen in the intergalactic medium (IGM) are presented, assuming that the non-linear baryonic mass density distribution in the IGM is lognormal. This ansatz was used earlier by Bi & Davidsen to perform one-dimensional simulations of lines of sight and analyse the properties of absorption systems. We have taken a completely analytic approach, which allows us to explore a wide region of the parameter space for our model. The analytic results have been compared with observations to constrain various cosmological and IGM parameters, whenever possible. Two kinds of correlation functions are defined: (i) along the line of sight (LOS); and (ii) across the transverse direction. We find that the effects on the LOS correlation owing to changes in cosmology and the slope of the equation of state of the IGM, γ , are of the same order, which means that we cannot constrain both the parameters simultaneously. However, it is possible to constrain γ and its evolution using the observed LOS correlation function at different epochs provided that one knows the background cosmology. We suggest that the constraints on the evolution of γ obtained using the LOS correlation can be used as an independent tool to probe the reionization history of the Universe. From the transverse correlation function, we obtain the excess probability, over random, of finding two neutral hydrogen overdense regions separated by an angle θ . We find that this excess probability is always less than 1 per cent for redshifts greater than 2. Our models also reproduce the observed column density distribution for neutral hydrogen, and the shape of the distribution depends on γ . Our calculations suggest that one can rule out γ >1.6 for z ≃2.31 using the column density distribution. However, one cannot rule out higher values of γ at higher redshifts.     

Metal enrichment of the intergalactic medium

I demonstrate by means of high-resolution cosmological simulations, which include modelling of a two-phase interstellar medium, that the dominant mechanism for transporting heavy elements from protogalaxies into the intergalactic medium (IGM) is the merger mechanism as discovered by Gnedin & Ostriker. Direct ejection of the interstellar gas by supernovae plays only a minor role in transporting metals into the IGM: for a realistic cosmological scenario only a small fraction of all metals in the IGM is delivered by the supernova-driven winds, while most of the metals in the IGM are transported by the merger mechanism. As a result, the metallicity distribution in the IGM is highly inhomogeneous, in agreement with studies of the QSO metal absorption systems, and the predicted metallicity distribution of Lyman alpha absorbers as a function of their column density is in excellent agreement with the observational data.     

Improved constraints on possible variation of physical constants from H i 21-cm and molecular QSO absorption lines

Quasar (QSO) absorption spectra provide an extremely useful probe of possible cosmological variation in various physical constants. Comparison of H  i 21-cm absorption with corresponding molecular (rotational) absorption spectra allows us to constrain variation in     , where α is the fine-structure constant and g _p is the proton g -factor. We analyse spectra of two QSOs, PKS 1413+135 and TXS 0218+357, and derive values of     at absorption redshifts of     and 0.6847 by simultaneous fitting of the H  i 21-cm and molecular lines. We find     and     respectively, indicating an insignificantly smaller y in the past. We compare our results with other constraints from the same two QSOs given recently by Drinkwater et al. and Carilli et al., and with our recent optical constraints, which indicated a smaller α at higher redshifts.