涟源煤盆地测水组煤系的X射线衍射特征

通过对湘中涟源煤盆地测水组煤及其顶板泥岩的Ｘ射线衍射分析可知,区域岩浆热变质作用是湘中涟源煤盆地测水组煤系变质的主要原因,对测水组煤系化学结构影响较大,动力变质作用仅起局部和次要作用。     

东营凹陷页岩油储层特征

渤海湾盆地东营凹陷始新统—渐新统沙河街组第三段下亚段(E_(2-3)s~(3-x))和沙河街组第四段上亚段(E_(2-3)s~(4-s))泥页岩分布面积广、累计厚度大、有机质丰度高、有机质类型以Ⅰ型干酪根为主,具有良好的页岩油勘探潜力。泥页岩主要发育层状和纹层状构造,主要矿物组成为粘土矿物、碳酸盐矿物、石英和长石。宏观观察下,泥页岩发育的裂缝主要有成岩裂缝和构造裂缝,孔隙主要为溶蚀孔、结晶孔及生物孔隙。微观观察下,主要发育的孔隙有粒间孔、粒内孔、晶间孔和溶蚀孔等,在不同的有机质丰度、类型及热演化程度下孔隙发育特征差异明显。小角X射线散射能够得到样品介孔(2~50 nm)的分布特征,结合抽提实验,对比处理前后孔隙分布特征表明细介孔(2~10nm)是有效的页岩油储集空间,也是影响孔隙结构复杂化的主要贡献者。核磁共振冷孔计法(NMRC)能测量泥页岩纳米级(2~500 nm)开孔孔隙的分布特征,定量表征孔隙率,弥补其它表征方法的不足。东营凹陷地区泥页岩中广泛发育的纳米级粒间孔是页岩油主要的赋存空间。     

Quantitative P–T–X constraints on orthopyroxene-bearing high-pressure granulites in felsic–metapelitic rocks: evidence from the Huangtuling granulite, Dabieshan Orogen

High‐pressure granulites are generally characterized by the absence of orthopyroxene. However, orthopyroxene is reported in a few high‐pressure, felsic–metapelitic granulites, such as the Huangtuling felsic high‐pressure granulite in the North Dabie metamorphic core complex in east‐central China, which rarely preserves the high‐pressure granulite facies assemblage of garnet + orthopyroxene + biotite + plagioclase + K‐feldspar + quartz. To investigate the effects of bulk‐rock composition on the stability of orthopyroxene‐bearing, high‐pressure granulite facies assemblages in the NCKFMASHTO (Na₂O–CaO–K₂O–FeO–MgO–Al₂O₃–SiO₂–H₂O–TiO₂–Fe₂O₃) system, a series of P–T–X pseudosections based on the melt‐reintegrated composition of the Huangtuling felsic high‐pressure granulite were constructed. Calculations demonstrate that the orthopyroxene‐bearing, high‐pressure granulite facies assemblages are restricted to low X_Al [Al₂O₃/(Na₂O + CaO + K₂O + FeO + MgO + Al₂O₃) < 0.35, mole proportion] or high X_Mg [MgO/(MgO + FeO) > 0.85] felsic–metapelitic rock types. This study also reveals that the X_Al values in the residual felsic–metapelitic, high‐pressure granulites could be significantly reduced by a high proportion of melt loss. We suggest that orthopyroxene‐bearing, high‐pressure granulites occur in residual overthickened crustal basement under continental subduction–collision zones and arc–continent collision belts.     

南四湖的形成与水环境演变

Through high-resolution research of sedimental chronology and the sediment environmental indexes,such as graininess ,minerals,magnetic parameters,pigment content organic carbon and chronology in Ds-core and Ws-core in Nansihu Lake,the authors analyze the formation cause of the Nansihu Lake and its water environmental changes,Historical documents are also analyzed here in order to reach the conclusion .Researches indicate that the Nansihu Lake came into being about 2500 aBP and its evolution succession can be divided into four stages.In this evolution process ,several scattered lakes merge into one large lake in the east of China,This process is distinctively affected by the overflow of the Yellow River,the excavation of the Grand Canal and other human activities.     

Epicyclic oscillation modes of a Newtonian,non‐slender torus

All normal modes of oscillations of slender tori have been expressed analytically in the classic work by Blaes (1985). We adopt his approach in order to calculate the eigenfunctions and eigenfrequencies of a particular class of epicyclic modes for slightly non‐slender tori, and present results of our numerical simulation of torus epicyclic modes of oscillations, which will be compared with the analytical results. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

High frequency QPOs,nonlinear oscillations in strong gravity

Some of the more promising ideas about the origin of the high frequency variability (kHz QPOs) in the observed X‐ray emissions of low‐mass X‐ray binaries are contrasted with less promising ones. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Boundary layer emission in luminous LMXBs

We show that aperiodic and quasiperiodic variability of bright LMXBs – atoll and Z‐sources – on ∼ sec‐msec time scales is caused primarily by variations of the luminosity of the boundary layer. The emission of the accretion disk is less variable on these time scales and its power density spectrum follows P _disk(f ) ∝ f ^–1 law, contributing to observed flux variation at low frequencies and low energies only. The kHz QPOs have the same origin as variability at lower frequencies, i.e. independent of the nature of the “clock”, the actual luminosity modulation takes place on the neutron star surface. The boundary layer spectrum remains nearly constant in the course of the luminosity variations and is represented to certain accuracy by the Fourier frequency resolved spectrum. In the investigated range of ∼ (0.1 – 1) _Edd it depends weakly on the global mass accretion rate and in the limit ∼ _Edd is close toWien spectrum with kT ∼ 2.4 keV. Its independence on the global value of lends support to the theoretical suggestion by Inogamov & Sunyaev (1999) that the boundary layer is radiation pressure supported. Based on the knowledge of the boundary layer spectrum we attempt to relate the motion along the Z‐track to changes of physically meaningful parameters. Our results suggest that the contribution of the boundary layer to the observed emission decreases along the Z‐track from conventional ∼50% on the horizontal branch to a rather small number on the normal branch. This decrease can be caused, for example, by obscuration of the boundary layer by the geometrically thickened accretion disk at ∼ _Edd. Alternatively, this can indicate significant change of the structure of the accretion flow at ∼ _Edd and disappearance of the boundary layer as a distinct region of the significant energy release associated with the neutron star surface. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Suzaku observations of iron lines and reflection in AGN

Initial results on the iron K‐shell line and reflection component in several AGN observed as part of the Suzaku Guaranteed Time program are reviewed. This paper discusses a small sample of Compton‐thin Seyferts observed to date with Suzaku; namely MCG‐5‐23‐16, MCG‐6‐30‐15, NGC4051, NGC3516, NGC2110, 3C 120 and NGC2992. The broad iron Kα emission line appears to be present in all but one of these Seyfert galaxies, while the narrow core of the line from distant matter is ubiquitous in all the observations. The iron line in MCG‐6‐30‐15 shows the most extreme relativistic blurring of all the objects, the red‐wing of the line requires the inner accretion disk to extend inwards to within 2.2R _g of the black hole, in agreement with the XMM‐Newton observations. Strong excess emission in the Hard X‐ray Detector (HXD) above 10 keV is observed in many of these Seyfert galaxies, consistent with the presence of a reflection component from reprocessing in Compton‐thick matter (e.g. the accretion disk). Only one Seyfert galaxy (NGC 2110) shows neither a broad iron line nor a reflection component. The spectral variability of MCG‐6‐30‐15, MCG‐5‐23‐16 and NGC 4051 is also discussed. In all 3 cases, the spectra appear harder when the source is fainter, while there is little variability of the iron line or reflection component with source flux. This agrees with a simple two component spectral model, whereby the variable emission is the primary power‐law, while the iron line and reflection component remain relatively constant. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Connection between spectral complexity and X‐ray weakness: testing the reflection interpretation

In recent work it was demonstrated that narrow‐line Seyfert 1 galaxies, which possessed spectral complexity in the 2–10 keV band were at the same time X‐ray weak. In this contribution I show how X‐ray weakness can be understood in the context of reflection and light bending picture. In fact, X‐ray weakness should be expected from objects that are in a reflection dominated state. With simultaneous UV and X‐ray data available with most XMM‐Newton observations, an estimate of the X‐ray weakness is relatively straightforward. As such, it is an easy way to substantiate conclusions of reflection dominated spectra, and we use this method to examine recent claims. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

The origin of the strong soft excess and puzzling iron line complex in Mkn 841

Mkn 841 has been observed during 3 different periods (January 2001, January 2005 and July 2005) by XMM‐Newton for a total cumulated exposure time of ∼108 ks. We present in this paper a broad band spectral analysis of the complete EPIC‐pn data sets. These observations confirm the presence of the strong soft excess and complex iron line profile known to be present in this source since a long time. They also reveal their extreme and puzzling spectral and temporal behaviors. Indeed, the 0.5–2 keV soft X‐ray flux decreases by a factor 3 between 2001 and 2005 and the line shape appears to be a mixed of broad and narrow components, both variable but on different timescales. The broad‐band 0.5–10 keV spectra are well described by a model including a primary power law continuum, a blurred photoionized reflection and a narrow iron line, the blurred reflection fitting self‐consistently the soft excess and the broad line component. The origin and nature of the narrow component is unclear. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)