A dissipative model of interacting winds for WR 140: A comparison with observations

A comparison between the stellar-wind interaction model with electron heat conduction and the ASCA X-ray observations of the (WR+O) binary system WR 140 has been made for the first time. This comparison shows that good agreement with observations can be achieved by varying the physical stellar-wind parameters within the ranges allowed by the accuracy of their determination. The self-consistent two-temperature model with heat conduction is an outgrowth of the model of interacting winds in such systems, which is required to properly interpret future detailed X-ray observations on the Chandra and Newton-XMM satellites.     

Soft X-ray sources at the centers of the elliptical galaxies NGC 4472 and NGC 4649

Analysis of recent observations of the elliptical galaxies NGC 4472 and NGC 4649 with the Chandra X-ray space telescope has revealed faint soft X-ray sources at their centers. The sources are located at the galactic centers, to within 1″, and are most likely associated with the radiation from the supermassive black holes that are assumed to be at the optical centers of these galaxies. Interest in these and several other similar objects stems from the unusually low luminosity of the supermassive black hole embedded in a dense interstellar medium. The sources have soft energy spectra in the Chandra energy range 0.2–10 keV. The source is detected at a 3σ confidence level only in the range 0.2–0.6 keV with a luminosity of ～6×10³⁷ erg s^?1 in NGC 4649 and in the range 0.2–2.5 keV with a luminosity of ～ 1.7×10³⁸ erg ^?1 in NGC 4472.     

Concept of High Speed Astronomical Instrumentation Based on Visible Light Photon Counters

The domain of high speed optical astrophysics is still quite unexplored. The availability of 10 meter diameter telescopes offers the unique possibility to investigate variability of faint objects at submillisecond time scales. In this paper I describe the concepts of a photometer and a spectrometer for high speed astronomical observations. The instruments are based on a photon counting detector developed for high energy physics, the Visible Light Photon Counter (VLPC). The detector has a quantum efficiency in the visible as high as 88% and performs photon counting with sub microsecond time resolution. The photometer is built using VLPC arrays. Adding a grating a VLPC array can be used in a time resolved spectrograph with medium resolution. This paper develops, starting from experimental data, the concept of the two VLPC based instruments and their application to time resolved photometry and spectroscopy of compact objects (pulsars, cataclysmic variables, low mass X-ray binary systems etc) and optical counterparts of Gamma Ray Bursts. The high speed optical observations are the ideal complement to X/γ rays and gravitational wave studies. The application of the instruments to the optical photometry of pulsars, the spectrophotometry of the prompt optical flash from Gamma Ray Bursts and the study of binary systems are discussed in detail: in the last two applications the instruments offer better opportunities than existing instruments.     

On the Nature of the Unidentified X-ray/γ-ray Sources Igr J18027–1455 and Igr J21247+5058

We present a multiwavelength study of the environment of the unidentified X-ray/γ-ray sources IGR J18027–1455 and IGR J21247 + 5058, recently discovered by the IBIS/ISGRI instrument, onboard the INTEGRAL satellite. The main properties of the sources found inside their position error circles, give us clues about the nature of these high-energy sources.     

Nearby young single black holes

We consider nearby young black holes formed after supernova explosions in close binaries whose secondary components are currently observed as the so-called runaway stars. Using data on runaway stars and making reasonable assumptions about the mechanisms of supernova explosion and binary breakup, we estimate the present positions of nearbyyoung black holes. For two objects, we obtained relatively small error regions (～50–100 deg²). The possibility of detecting these nearby young black holes is discussed.     

X-ray emission lines in the early afterglows of gamma-ray bursts

We computed the thermal time-dependent X-ray spectrum of a hot plasma in the vicinity of a gamma-ray burst (GRB). An allowance for time-dependent processes in a hot rarefied plasma is shown to strongly affect the observed spectrum. These computations can give an alternative explanation for the observed X-ray emission lines in the early afterglows of GRBs (e.g., GRB 011211). Our technique allows the GRB collimation angle and the environment clumpiness parameters to be independently constrained.     

关于太阳白光耀斑连续发射起源的讨论

白光耀斑研究近年来获得较大进展，对其连续发射起源机制目前流行三种解释．一是耀斑形成过程中所产生的色球凝聚[1-3]，二是非热粒子注入大气致氢原子非热激发和电离[4-6]，三是色球强加热所引起的对大气深层的辐射反加热[7]．这三类解释具有一个共性，即除了自身直接对连续谱     

The state of gold in phases of the Cu-Fe-S system: In situ X-ray absorption spectroscopy study

Chalcopyrite and bornite are the main Au-bearing minerals at Cu porphyry deposits, volcanogenic massive sulfide (VMS) deposits, Cu-Ni deposits of the mafic magmatic complexes, and ores of submarine sulfide edifices. Bornite and intermediate solid solutions with wide compositional variations (bnss and iss – high-temperature chalcopyrite, correspondingly), which can scavenge economic concentrations of Au, appear in the Cu-Fe-S system at ore-forming conditions. However, the state of Au in bnss and iss is yet unknown. To solve this conundrum, we synthesized samples with net chemical composition of bnss and iss, studied them by in situ X–ray absorption spectroscopy (XAS), and used the experimental data to explain the Au distribution among natural ore-forming minerals. The sulfide samples were obtained at 495–700 °C in Au-saturated system by means of salt flux method. The bnss contained ～1.2–1.6 log units more Au than iss: up to 18 wt.% Au in bnss vs 0.4 wt.% Au in iss at 700 °C. An increase of temperature resulted in the sharp increase of Au concentration in both phases, ～1 log unit per 100 °C at f(S₂) close to S_(l) saturation. Analysis of Au L₃-edge spectra recorded at 25–675 °C revealed that at 25 °C Au exists mainly in the metallic state. At t > 500 °C the spectral features of Au° disappear, and “chemically bound” Au predominates. The Au form of occurrence in the iss field is interpreted as Au-bearing clusters with a stromeyerite-like (CuAgS) structure. Digenite Cu_2–xS and bnss contain Au in a mixture of stromeyerite-like and petrovskaite-like (Au_0.8Ag_1.2S) clusters. The chemical composition of both forms is close to CuAuS, where the nearest Au neighbors are two S atoms at R_Au-S = 2.34–2.36 Å. Results of the present study allow to determine the state of Au and its concentration in the main Cu-bearing minerals of sulfide ores as a function of the T-f(S₂)-compositional parameters. Due to the sharp increase of the CuAuS clusters stability with increasing temperature, in high-temperature ores formed at t > 350 °C Au enriches Cu-bearing minerals in comparison with Cu-free or Cu-deficient ones. As a result, in these ores native gold, being a product of decomposition of the Au-bearing clusters, is associated with Cu-rich minerals – chalcopyrite, bornite, digenite, chalcocite.     

安徽金寨迎峰崖含金银富铅锌多金属矿工艺矿物学研究

为查清安徽金寨迎峰崖含金银富铅锌多金属矿矿区内矿石的物质组分及矿物嵌布特征,采用化学多元素分析、光片和薄片镜下鉴定、X射线衍射分析以及单矿物组分分析等方法,对矿石的物质组分、矿物的嵌布特征进行分析测试。结果表明,矿石中主要矿物为方铅矿、闪锌矿、黄铜矿、黄铁矿、石英等。方铅矿、闪锌矿以包裹嵌镶或黏连镶布为主,细小的方铅矿与其他矿物毗邻,交代成因的闪锌矿呈融滴状分布于被交代矿物之上。Au充填于黄铁矿晶隙中;Ag在方铅矿中富集,主要以化合物形式存在;闪锌矿中有害组分Cd（2 697 mg/kg）严重超标,其他有害组分为Fe、S、As等。矿石矿物颗粒粒度以中粗粒为主。研究结果可为矿物分离及后期的开发利用提供参考。     

基于CT图像的花岗岩矿物组分与细观结构分析

获取准确的岩石矿物组分与细观结构特征,对从细观层面认识岩石宏观力学性质具有重要意义。CT扫描技术是研究岩石矿物细观结构的有力工具。本文采用高分辨率三维CT扫描系统,获得了花岗岩CT扫描图像;采用阈值分割的方法,综合X射线衍射试验结果确定合理的分割阈值,实现了对花岗岩CT灰度图像的三值化分析;最终获得了花岗岩的主要矿物含量与细观结构特征。研究结果表明:选择合理的分割阈值,可实现花岗岩主要矿物石英、长石、云母的自动识别和定量分析;基于三维重构模型,可获得不同矿物的形状、粒径和空间分布特征。本文方法对定量测试岩石矿物组分和认识其细观结构具有一定的参考意义和价值。