靖边气田南部Mu_(1-4)储层控制因素研究     

顾绍富  吴燕  雷卞军  夏湘玲  孟堃  陈波 《新疆地质》2010,28(3)

通过对靖边气田南部MU1-4储层的沉积微相、成岩作用、构造特征及古地貌单元特征进行分析,认为潮上带的(含)膏模膏核泥-细粉晶白云岩和潮间带上部的膏模泥-细粉晶云岩为最有利微相.对孔隙起建设性成岩作用主要是准同生白云石化作用、表生岩溶作用和埋藏溶解作用,构造高部位的储渗能力较强,岩溶斜坡及台丘,尤其古沟槽附近,是岩溶储层发育的有利区域.要准确把握本区碳酸盐岩储集层的分布规律,需以沉积微相、成岩作用为基础,结合现今构造特征和岩溶古地貌,展开多因素组合分析.  相似文献   

遥感技术在大狐狸山地区1：50000矿产远景调查中的应用     

刘颖璠  苏世杰  郑宝军  梁伟  许立权  嘎日迪 《西北地质》2010,43(2):195-201

以内蒙古自治区西部阿拉善盟额济纳旗大狐狸山地区1：5万矿产远景调查为例,论述了遥感技术在1：5万矿产远景调查中的应用和具体工作方法。研究结果表明,在1：5万矿产远景调查中充分利用遥感技术,进行线性构造、环形构造、地质体的信息提取,利用主成分分析法有效提取矿化蚀变信息,在RGMAP数字平台,将工作区的标准影像图与其它数据源进行叠加整合,多轮回遥感地质解译成图,结合地质、物探、化探工作成果,快速有效地指导了地面找矿工作,对合理圈定找矿预测靶区起到了重要作用。  相似文献   

四川绿水洞井田煤层稳定性探采对比及其影响因素探讨     

阳伟  苏时才  陈长永  张峰  王俊 《中国煤炭地质》2010,(10):1-4,16

绿水洞井田可采煤层为龙潭组一段的K1煤层,通过煤层稳定性探采对比及其影响因素的探讨,认为地质勘查阶段在确定煤层稳定性时,应当剔除因褶皱、断层和陷落柱等因素引起煤厚突变的地质点。通过大量地质资料分析了影响矿区煤层稳定性的因素,认为褶皱在侧压力及垂直压力作用下分别导致褶皱核部煤层增厚和变薄;正断层和逆断层分别导致其附近煤层变薄和增厚;陷落柱多使其附近煤层变薄。勘查阶段煤层稳定性的合理确定为煤矿合理布置采掘巷道和选择合理的采煤方法都具有一定的实际意义。  相似文献   

10Be and 26Al exposure‐age dating of bedrock surfaces on the Aran ridge,Wales: evidence for a thick Welsh Ice Cap at the Last Glacial Maximum     

Neil F. Glasser  Philip D. Hughes  Cassandra Fenton  Christoph Schnabel  Henrik Rother 《第四纪科学杂志》2012,27(1):97-104

This paper presents results of the analysis of paired cosmogenic isotopes (¹⁰Be and ²⁶Al) from eight quartz‐rich samples collected from ice‐moulded bedrock on the Aran ridge, the highest land in the British Isles south of Snowdon. On the Aran ridge, comprising the summits of Aran Fawddwy (905 m a.s.l.) and Aran Benllyn (885 m a.s.l.), ²⁶Al and ¹⁰Be ages indicate complete ice coverage and glacial erosion at the global Last Glacial Maximum (LGM). Six samples from the summit ridge above 750–800 m a.s.l. yielded paired ¹⁰Be and ²⁶Al ages ranging from 17.2 to 34.4 ka, respectively. Four of these samples are very close in age (¹⁰Be ages of 17.5 ± 0.6, 17.5 ± 0.7, 19.7 ± 0.8 and 20.0 ± 0.7 ka) and are interpreted as representing the exposure age of the summit ridge. Two other summit samples are much older (¹⁰Be ages of 27.5 ± 1.0 and 33.9 ± 1.2 ka) and these results may indicate nuclide inheritance. The ²⁶Al/¹⁰Be ratios for all samples are indistinguishable within one‐sigma uncertainty from the production rate ratio line, indicating that there is no evidence for a complex exposure history. These results indicate that the last Welsh Ice Cap was thick enough to completely cover the Aran ridge and achieve glacial erosion at the LGM. However, between c. 20 and 17 ka ridge summits were exposed as nunataks at a time when glacial erosion at lower elevations (below 750–800 m a.s.l.) was achieved by large outlet glaciers in the valleys surrounding the mountains. Copyright © 2011 John Wiley & Sons, Ltd.  相似文献   

The impact and rotational light curves of Comet 9P/Tempel 1     

Jean Manfroid  Damien Hutsemékers  Anita L. Cochran  William M. Jackson  Rita Schulz 《Icarus》2007,187(1):144-155

UVES and HIRES high-resolution spectra of Comet 9P/Tempel 1 are used to investigate the impact and rotational light curves of various species with a view toward building a simple model of the distribution and activity of the sources. The emission by OH, NH, CN, C₃, CH, C₂, NH₂, and OI, are analyzed, as well as the light scattered by the dust. It is found that a simple model reproduces fairly well the impact light curves of all species combining the production of the observed molecules and the expansion of the material throughout the slit. The impact light curves are consistent with velocities of 400-600 m/s. Their modeling requires a three-step dissociation sequence “Grand-Parent → Parent → Daughter” to produce the observed molecules. The rotational light curve for each species is explained in terms of a single model with three sources. The dust component can however not easily be explained that way.  相似文献   

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赵刚  李江  何案华  王军  秦久刚 《大地测量与地球动力学》2007,27(6):124-128

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X-ray Spectroscopy of Dips of Cir X-1     

Ya-Juan Lei Fang-Jun Lu Jin-Lu Qu Li-Ming Song Cheng-Min Zhang 《中国天文和天体物理学报》2007,7(5):693-704

We present X-ray spectral analyses of the low-mass X-ray binary Cir X-1 dur- ing X-ray dips,using the Rossi X-ray Timing Explorer(RXTE)data.Each dip was divided into several segments,and the spectrum of each segment was fitted with a three-component blackbody model,in which the first two components are affected by partial covering and the third one is unaffected.A Gaussian emission line is also included in the spectral model to represent the Fe Kαline at～6.4 keV.The fitted temperatures of the two partially covered components are about 2 keV and 1 keV,while the uncovered component has a temperature of～0.5-0.6 keV.The equivalent blackbody emission radius of the hottest component is the smallest and that of the coolest component is the largest.During the dips the fluxes of the two hot components are linearly correlated,while that of the third component does not show any significant variation.The Fe line flux remains constant,within the errors,during the short dips.However,during the long dips the line flux varies significantly and is positively correlated with the fluxes of the two hot components.These results suggest:(1)that the tem- perature of the X-ray emitting region decreases with radius,(2)that the Fe Kαline emitting region is close to the hot continuum emitting region,and(3)that the size of the Fe line emit- ting region is larger than that of the obscuring matter causing the short dips but smaller than the region of that causing the long dips.  相似文献   

The internal structure of Jupiter family cometary nuclei from Deep Impact observations: The “talps” or “layered pile” model     

Michael J.S. Belton  Peter Thomas  Peter Schultz  Lori Feaga  Olivier Groussin  Casey Lisse  Jessica Sunshine  W. Alan Delamere 《Icarus》2007,187(1):332-344

We consider the hypothesis that the layering observed on the surface of Comet 9P/Tempel 1 from the Deep Impact spacecraft and identified on other comet nuclei imaged by spacecraft (i.e., 19P/Borrelly and 81P/Wild 2) is ubiquitous on Jupiter family cometary nuclei and is an essential element of their internal structure. The observational characteristics of the layers on 9P/Tempel 1 are detailed and considered in the context of current theories of the accumulation and dynamical evolution of cometary nuclei. The works of Donn [Donn, B.D., 1990. Astron. Astrophys. 235, 441-446], Sirono and Greenberg [Sirono, S.-I., Greenberg, J.M., 2000. Icarus 145, 230-238] and the experiments of Wurm et al. [Wurm, G., Paraskov, G., Krauss, O., 2005. Icarus 178, 253-263] on the collision physics of porous aggregate bodies are used as basis for a conceptual model of the formation of layers. Our hypothesis is found to have implications for the place of origin of the JFCs and their subsequent dynamical history. Models of fragmentation and rubble pile building in the Kuiper belt in a period of collisional activity (e.g., [Kenyon, S.J., Luu, J.X., 1998. Astron. J. 115, 2136-2160; 1999a. Astron. J. 118, 1101-1119; 1999b. Astrophys. J. 526, 465-470; Farinella, P., Davis, D.R., Stern, S.A., 2000. In: Mannings, V., Boss, A.P., Russell, S.S. (Eds.), Protostars and Planets IV. Univ. of Arizona Press, Tucson, pp. 1255-1282; Durda, D.D., Stern, S.J., 2000. Icarus 145, 220-229]) following the formation of Neptune appear to be in conflict with the observed properties of the layers and irreconcilable with the hypothesis. Long-term residence in the scattered disk [Duncan, M.J., Levison, H.F., 1997. Science 276, 1670-1672; Duncan, M., Levison, H., Dones, L., 2004. In: Festou, M., Keller, H.U., Weaver, H.A. (Eds.), Comets II. Univ. of Arizona Press, Tucson, pp. 193-204] and/or a change in fragmentation outcome modeling may explain the long-term persistence of primordial layers. In any event, the existence of layers places constraints on the environment seen by the population of objects from which the Jupiter family comets originated. If correct, our hypothesis implies that the nuclei of Jupiter family comets are primordial remnants of the early agglomeration phase and that the physical structure of their interiors, except for the possible effects of compositional phase changes, is largely as it was when they were formed. We propose a new model for the interiors of Jupiter family cometary nuclei, called the talps or “layered pile” model, in which the interior consists of a core overlain by a pile of randomly stacked layers. We discuss how several cometary characteristics—layers, surface texture, indications of flow, compositional inhomogeneity, low bulk density low strength, propensity to split, etc., might be explained in terms of this model. Finally, we make some observational predictions and suggest goals for future space observations of these objects.  相似文献   

Nuclear spin temperature of ammonia in Comet 9P/Tempel 1 before and after the Deep Impact event     

Hideyo Kawakita  Emmanuel Jehin  Jean Manfroid 《Icarus》2007,187(1):272-275

The Deep Impact mission succeeded in excavating inner materials from the nucleus of Comet 9P/Tempel 1 on 2005 July 04 (at 05:52 UT). Comet 9P/Tempel 1 is one of Jupiter family short period comets, which might originate in the Kuiper belt region in the solar nebula. In order to characterize the comet and to support the mission from the ground-based observatory, optical high-dispersion spectroscopic observations were carried out with the echelle spectrograph (UVES) mounted on the 8-m telescope VLT (UT2) before and after the Deep Impact event. Ortho-to-para abundance ratios (OPRs) of cometary ammonia were determined from the NH₂ emission spectra. The OPRs of ammonia on July 3.996 UT and 4.997 UT were derived to be 1.28±0.07 (nuclear spin temperature: Tspin=24±2 K) and 1.26±0.08 (Tspin=25±2 K), respectively. There is no significant change between before and after the impact. Actually, most materials ejected from the impact site could have moved away from the nucleus on July 4.997 UT, about 17 h after the impact. However, a small fraction of the ejected materials might remain in the slit of UVES instrument at that time because an excess of about 20% in the NH₂ emission flux is observed above the normal activity level was found [Manfroid, J., Hutsemékers, D., Jehin, E., Cochran, A.L., Arpigny, C., Jackson, W.M., Meech, K.J., Schulz, R., Zucconi, J.-M., 2007. Icarus. This issue]. If the excess of NH₂ on July 04.997 UT was produced from icy materials excavated by the Deep Impact, then an upper-limit of the ammonia OPR would be 1.75 (Tspin>17 K) for those materials. On the other hand, the OPR of ammonia produced from the quiescent sources was similar to that of the Oort cloud comets observed so far. This fact may imply that physical conditions where cometary ices formed were similar between Comet 9P/Tempel 1 and the Oort cloud comets.  相似文献   

Determination of Platinum-Group Elements and Forty Two Other Elements in Two Candidate Danish Cretaceous-Tertiary Boundary Clay Reference Materials by INAA, ENAA and RNAA     

Xueying Mao  Xiaolin Hou  Chungsheng Li  Hong Ouyang  Zhifang Chai 《Geostandards and Geoanalytical Research》2001,25(1):167-171

Ruthenium, rhodium, palladium, osmium, iridium and platinum (PGEs) and forty two other elements in two candidate geological Cretaceous-Tertiary boundary clay reference materials taken from the Fish Clay, Stevns Klint, Denmark, were determined by a combination of neutron activation analysis (NAA) consisting of instrumental, epithermal and radiochemical NAA with or without nickel sulfide fire assay preconcentration. The accuracy of the experimental values was assessed by the comparative analysis of the certified reference materials.  相似文献