黔西比德-三塘向斜煤层气藏特征及甜点区段

黔西比德-三塘向斜煤层气藏主要赋存于龙潭组Ⅰ、Ⅱ、Ⅲ 3个煤组中,其中Ⅰ煤组6#和7#煤层、Ⅱ煤组16#和17#煤层、Ⅲ煤组20#、23#、27#、30#煤层分布稳定。煤层埋深受向斜构造控制明显,比德次向斜近轴部地区可达1500 m;煤岩以高变质的瘦煤、贫煤和无烟煤为主,最大镜质体反射率自西向东、由北到南逐渐增大;煤岩对甲烷吸附能力普遍较高（兰氏体积,18.32~39.32 m3/t）,区域上受煤变质程度影响显著;原位埋深条件下,煤岩渗透率较低,煤层含气量整体较高,平均10~15.78 m3/t,含气饱和度普遍大于50%。结合该地区多层合采效果发现,比德次向斜埋深超过800 m的气井产气效果差,珠藏和三塘次向斜煤层气开发地质条件较好,其中珠藏向斜Ⅲ煤组4套主力煤层（煤层间距小于60 m）为潜在的高产优质储层。     

新疆喀拉昆仑山大黄山稀土-铌-铁钛多金属矿化带地质特征及矿床成因

对喀喇昆仑山大黄山稀土-铌-铁钛多金属矿化带地质特征及矿床成因进行研究,为该区找矿勘查工作部署提供依据。通过详细的野外地质调查,在总结大黄山稀土-铌-铁钛多金属矿化带地质特征的基础上,配合镜下鉴定、矿床地球化学分析,探讨矿床成因类型与成矿作用,分析成矿期后的构造变形,预测矿化体的空间就位,提出找矿方向和找矿思路。大黄山稀土-铌-铁钛多金属矿化带含矿建造沉积环境为近陆滨-浅海碳酸盐岩台地相。矿化带处于石炭系帕斯群灰岩组（a组）上段（含矿泥质灰岩段）上部,区内延伸大于30km,西段发现2条矿化体（Ⅰ-1、Ⅰ-1）,东段发现7条矿化体（Ⅱ-1~Ⅱ-7）。单矿化体一般长170~2000 m,厚度10~32 m,矿化体产状与地层产状一致,层控特征明显。矿石化学测试结果表明,矿化体内含Fe、Al、Ti、LREE、Nb、Ta等多种金属成矿元素。矿床成因类型为近陆滨海相沉积型。矿源为古陆源区红土型风化壳,以沉积物重力流和胶体溶液混合流体形式快速搬运,并在近陆滨岸地带以事件沉积作用快速卸载堆积而成。成矿期后,含矿建造遭受了强烈的构造改造,形成了总体呈NWW向展布的断褶带,带内发育的复式-叠加反"S"型褶皱构造构成了区内最特征的控矿构造样式。该带找矿前景好,找矿潜力大,通过进一步的矿产地质工作,有望在该带实现Fe、Al、Ti,尤其是稀有、稀土元素的重要找矿突破。     

沂源煤田鲁村井田山西组层位的发现及其地质意义

通过采用地面物探、钻探和井下巷探、钻探相结合的综合勘探方法,对鲁村井田深部进行了补充勘探,并对井田以往地质资料进行了重新对比分析,发现该井田-400～-1 300 m的埋深范围内不但存在以往认为已被剥蚀缺失的太原组上部地层,还保存了较完整的山西组,尤其是在该段地层中新发现了5个局部可采煤层,为井田增加了资源储量、延长了服务年限。填补了沂源煤田太原组上部和山西组含煤地层资料的空白。     

山东青州地区炒米店组上部含白云岩层段剖面及区域地层对比

本区炒米店组上部出现了厚达几十米的白云岩夹灰岩层段,按地层清理对“三山子组”的定义—以连续的大套白云岩出现为其底界［１］,这段地层不属三山子组,应归炒米店组。然而,不但这里的三山子组白云岩均含燧石结核,炒米店组顶部的灰岩也含大量的燧石结核和条带。于白云岩夹灰岩之层段发现大量的头足类化石,其时代属早奥陶世。该段地层可与区域上的三山子组ａ段下部和ｂ段相对比。这是鲁西地区寒武—奥陶系剖面的一种新类型。     

Characteristics and formation causes of Qingdao Cold Water Mass

In this work,the main characteristics of the Qingdao Cold Water Mass were studied by using“the comparison analysis method”based on 1980 temperature,salinity and dissolved oxygen data on the western South Yellow Sea.The formation cause of the water mass was analyzed based on February of 1959 temperature and salinity data for this area and on some other authors’studies.The results showed that the Qingdao Cold Water Mass has growing and vanishing processes：appears in the last ten days of March;has stable pattern in April;is biggest in its area in May;becomes small in its area in June;vanishes in July.It comes from the northem Shandong Coastal Water and is characterized by low temperature and salinity and high disolved oxygen.The mass is formed under the joint effects of anticyclonic circulation and solar radiation.     

The importance of interactions for mass loss from satellite galaxies in cold dark matter haloes

We investigate the importance of interactions between dark matter substructures for the mass loss they suffer whilst orbiting within a sample of high-resolution galaxy cluster mass cold dark matter (CDM) haloes formed in cosmological N -body simulations. We have defined a quantitative measure that gauges the degree to which interactions are responsible for mass loss from substructures. This measure indicates that interactions are more prominent in younger systems when compared to older more relaxed systems. We show that this is due to the increased number of encounters a satellite experiences and a higher mass fraction in satellites. This is in spite of the uniformity in the distributions of relative distances and velocities of encounters between substructures within the different host systems in our sample.
Using a simple model to relate the net force felt by a single satellite to the mass loss it suffers, we show that interactions with other satellites account for ∼30 per cent of the total mass loss experienced over its lifetime. The relation between the age of the host and the importance of interactions increases the scatter about this mean value from ∼25 per cent for the oldest to ∼45 per cent for the youngest system we have studied. We conclude that satellite interactions play a vital role in the evolution of substructure in dark matter haloes and that a significant fraction of the tidally stripped material can be attributed to these interactions.     

Estimating open boundary conditions from coastal tidal observations by adjoint approach

A numerical study for estimating the tidal open boundary conditions of a shelf current modrl from tb coastal tidal observations is presented. The method is based on the optimal control/adjoint method. A lrast square fitting of the model state to simulated data is used. Two ideal domains and coastlines are considered. Using the IAP shallow. water model and its adjoint model, some identical twin experiments are carried out to test efficiency and lirnilsd of the method. The results show that the adjoint method can efficiently estimate the open boundary conditions well for gulf/bay like domains. The adjoint method seems to have great potential to improve the accuracy of tide and shelf current modeling in coastal regions. Project supported hy the National Natural Science Fuundation of China (Grant No. 49376256)     

Star formation in the Cepheus Flare region – II. A-type stars associated with IRAS sources

In order to reveal the star-forming history of the molecular cloud complex we studied the intermediate mass stellar population in the Cepheus Flare region. (Paper I dealt with the distance and the young stellar object candidates of the region.) Correlating the IRAS Point Source Catalogue and Faint Source Catalogue positions with those of 1214 B8–A8 and 1760 F0–F5 type stars brighter than     and classified during an objective prism survey, we identified 19 stars showing far-infrared excess emission in the Cepheus Flare region. In addition to the 16 stars whose counterparts are given in the IRAS catalogues, we found three more stars with infrared excess not recognized before. In order to identify the young medium-mass stars associated with the Cepheus Flare molecular clouds we observed the optical spectra of the IR-excess stars, and using published optical photometry and the IRAS data we examined their spectral energy distributions (SEDs) and IRAS two-colour diagram. The observations resulted in the discovery of a new Herbig Ae/Be star, BD +68°1118, coinciding with IRAS 21169+6842. More evolved HAe/Be stars may be SAO 19953, BD +67°1314 and BD +69°1231, whose H α lines showed weak emission components. Possible β Pictoris- or Vega-type stars may be HD 203854, HD 212826 and HD 216486, whereas the far-infrared fluxes at the positions of BD +72°1018, HD 210806 and HD 217903 can be attributed to the heating of the interstellar environment. We used distances and radial velocities of the stars derived from the spectroscopy and published optical photometry as indicators of their relations to the clouds. Information on the environment of the observed stars deduced from the diffuse interstellar band at λ 6613 is briefly discussed.     

Confirming a population of hot-dust dominated, star-forming, ultraluminous galaxies at high redshift

We identify eight   z > 1  radio sources undetected at 850 μm but robustly detected at 70 μm, confirming that they represent ultraluminous infrared galaxies (ULIRGs) with hotter dust temperatures  (〈 T _d〉= 52 ± 10 K)  than submillimetre galaxies (SMGs) at similar luminosities and redshifts. These galaxies share many properties with SMGs: ultraviolet spectra consistent with starbursts, high stellar masses and radio luminosities. We can attribute their radio emission to star formation since high-resolution Multi-Element Radio Linked Interferometer Network (MERLIN) radio maps show extended emission regions (with characteristic radii of 2–3 kpc), which are unlikely to be generated by active galactic nucleus (AGN) activity. These observations provide the first direct confirmation of hot, dusty ULIRGs which are missed by current submillimetre surveys. They have significant implications for future observations from the Herschel Space Observatory and Submillimetre Common-User Bolometer Array 2 (SCUBA2), which will select high-redshift luminous galaxies with less selection biases.