麻黄山西区延长组长4+5至长6储层成岩作用及成岩演化史研究

麻黄山西区长4＋5至长6储层为一套三角洲前缘亚相的细砂岩,研究证明砂岩目前处于中成岩A期。机械压实与胶结作用是孔隙减少的主要作用,也是本区原生孔隙少、储集物性差的直接原因;而大气淡水的淋滤作用及有机酸溶蚀作用,尤其是有机酸溶蚀作用,是产生次生孔隙的主要作用,使局部储层物性有所改善,因此次生孔隙是本区油气的主要储集空间,下一步油气勘探开发应注重对有利次生孔隙空间的预测。     

A two-zone model for the broad iron line emission in MCG–6-30-15

We reanalyse the ASCA and BeppoSAX data of MCG–6-30-15, using a double-zone model for the iron line profile. In this model, the X-ray source is located around ≈10 Schwarzschild radii and the regions interior and exterior to the X-ray source produce the line emission. We find that this model fits the data with a similar reduced χ ² to the standard single-zone model. Thus we show that the presence of a broad iron line feature does not necessarily require that the X-ray source be located close to the last stable orbit or in the disc rotation axis.
Within the framework of this model, the best-fitting inclination angle of the source     for the intermediate-intensity ASCA data set is compatible with that determined by earlier modelling of optical lines. The observed variability of the line profile with intensity can be explained as variations of the X-ray source size. That several active galactic nuclei with broad lines have the peak centroid near 6.4 keV can be explained under certain conditions.
We also show that the simultaneous broad-band observations of this source by BeppoSAX rule out the Comptonization model which was an alternative to the standard inner-disc one. We thereby strengthen the case that line broadening occurs as a result of the strong gravitational influence of a black hole.     

含钙铝铁水解聚合产物的矿物学研究Ⅱ:热分解特性

分别以NaOH和Ca(OH)2作为碱化剂,合成了聚合氯化铝铁(PAFCNa,PAFCCa),比较样聚合氯化铝(PACNa,PACCa)、聚合氯化铁(PFCNa,PFCCa),制成低温干燥样进行热分解检测.热重分析证明,PAFCCa中的含水量高,主要是配位水与结晶水.当n(Al)/n(Fe)>5:5后,PAFCCa的含水量平均为42.3%.按Ca6Al2(SO4)3(OH)12·26H2O分子式计算,钙矾石的结构水(含OH水)含量为43.06%,两者含水量相当接近.TG-DTG热分析结果支持XRD对PAFCCa中存在含Ca3Al2(OH)12柱体的类钙矾石结构体的认定.PAFC-Ca根据其DTG曲线上的125℃和180℃两个脱水速率(肩)峰可以判别其中有无钙矾石结构体,以及相对量的多少.     

An extended multi-zone model for the MCG–6-30-15 warm absorber

The variable warm absorber seen with ASCA in the X-ray spectrum of MCG–6-30-15 shows complex time behaviour in which the optical depth of O  viii anticorrelates with the flux whereas that of O  vii is unchanging. The explanation in terms of a two-zone absorber has since been challenged by BeppoSAX observations. These present a more complicated behaviour for the O  viii edge. We demonstrate here that the presence of a third, intermediate, zone can explain all the observations. In practice, warm absorbers are likely to be extended, multi-zone regions of which only part causes directly observable absorption edges at any given time.     

鄂尔多斯盆地南部旬邑-宜君地区中生界储层特征

对鄂尔多斯盆地南部旬邑 -宜君地区中生界主要储集层——直罗组、延安组、延长组储层特征从沉积相、砂体纵向展布、岩性和物性等几方面进行了简要论述。通过研究指出本区储层具有低孔、低渗的特点。在纵向上以直罗组储层相对最好 ,延安组次之 ,之后才是三叠系延长组。储集层普遍具有岩性细、成岩后生变化强烈的特点。由于储层低孔、低渗 ,因此 ,油层的压裂改造措施必不可少     

鄂尔多斯盆地子北地区长6段油藏成藏条件及主控因素

分析了鄂尔多斯盆地子北地区延长组长6段油层构造特征、沉积相分布及砂体展布特征,从烃源岩、储层、盖层等方面对长6段油藏成藏条件进行了探讨,并就油藏类型、主控因素及成藏期次进行了讨论。结果表明:子北地区长6段油藏具有较好的生、储、盖配置关系,主要受沉积微相及储层物性控制;长6段油气主要储存在长61、62、63段河道砂体内,油藏类型主要为岩性圈闭;长6段油藏主控因素有主分流河道、储层物性及其非均质性、原油分布;长6段油层中,油气包裹体均一温度分布呈双峰状,主要在100℃~110℃和130℃~140℃;利用热演化史与流体包裹体均一温度法对油气成藏期次进行判断,长7段烃源岩生成的油气在早白垩世运移并大量聚集至长6段油层组,形成长6段油藏。     

MS 1603.6+2600: an accretion disc corona source?

We have observed the eclipsing low-mass X-ray binary MS 1603.6+2600 with Chandra for 7 ks. The X-ray spectrum is well fit with a single absorbed power law with an index of ∼2. We find a clear sinusoidal modulation in the X-ray light curve with a period of  1.7 ± 0.2 h  , consistent with the period of 1.85 h found before. However, no (partial) eclipses were found. We argue that if the X-ray flare observed in earlier X-ray observations was a type I X-ray burst, then the source can only be an accretion disc corona source at a distance of ∼11–24 kpc (implying a height above the Galactic disc of ∼8–17 kpc). It has also been proposed in the literature that MS 1603.76+2600 is a dipper at ∼75 kpc. We argue that, in this dipper scenario, the observed optical properties of MS 1603.6+2600 are difficult to reconcile with the optical properties one would expect on the basis of comparisons with other high-inclination, low-mass X-ray binaries, unless the X-ray flare was not a type I X-ray burst. In that case, the source can be a nearby soft X-ray transient accreting at a quiescent rate, as was proposed by Hakala et al., or a high-inclination source at ∼15–20 kpc.     

Evolution of the near-infrared in rich galaxy clusters

We present the K -band (2.2 μm) luminosity functions (LFs) of the X-ray-luminous clusters MS1054–0321 ( z  = 0.823), MS0451–0305 ( z  = 0.55), Abell 963 ( z  = 0.206), Abell 665 ( z  = 0.182) and Abell 1795 ( z  = 0.063) down to absolute magnitudes M _K  = −20. Our measurements probe fainter absolute magnitudes than do any previous studies of the near-infrared LFs of clusters. All the clusters are found to have similar LFs within the errors, when the galaxy populations are evolved to redshift z  = 0. It is known that the most massive bound systems in the Universe at all redshifts are X-ray-luminous clusters. Therefore, assuming that the clusters in our sample correspond to a single population seen at different redshifts, the results here imply that not only had the stars in present-day ellipticals in rich clusters formed by z  = 0.8, but that they existed in as luminous galaxies then as they do today.   Additionally, the clusters have K -band LFs which appear to be consistent with the K -band field LF in the range −24 <  M _K  < −22, although the uncertainties in both the field and cluster samples are large.