Timing of mineralization at the Shihu gold deposit in the middle segment of the Taihang Mountain,China

The Shihu gold deposit, located in the middle-south section of the core of the Fuping mantle branch structure, is hosted in the Archean Fuping Group and adjacent to the quartz diorite porphyrite. The gold deposit is the only large gold deposit with reserves of more than 30 tons gold discovered in western Hebei Province so far. In order to constrain the timing of mineralization of this ore deposit, this paper focuses on the isotopic dating of zircon and pyrite. Zircons in gold-bearing quartz veins are magmatic in origin and no hydrothermal zircon has been found in such quartz veins, indicating that zircons were derived from the wall rocks. U–Pb ages of zircons fall mainly in the two domains: 2492 ± 82 and 136 ± 4 Ma, respectively, indicative of the contribution of the Fuping-Group TTG gneiss and Yanshanian igneous rocks, respectively. The Re–Os isotopic compositions of pyrites in the gold-bearing quartz veins yield an isochron age of 127 ± 31 Ma. Combined with other dating results, we suggest that the main metallogenic age of the Shihu gold deposit is 120–127 Ma.     

A New Ootype of Dinosaur Egg (Faveoloolithidae: Duovallumoolithus shangdanensis oogen. et oosp. nov.) from the Late Cretaceous in the Shangdan Basin,Shaanxi Province,China

A new ootype collected from the Upper Cretaceous Lijiacun Formation in the Shangdan Basin, Shaanxi Province is described in this paper. Based on general external shape, size, eggshell thickness and honeycomb‐like eggshell microstructure, eggs are referable to the oofamily Faveoloolithidae. Compared with other members of Faveoloolithidae, specimens described in this paper show special characteristics: adjacent pores are usually separated by two eggshell units between which often develop interspaces; columnar eggshell units are relatively closely arranged in radial view. According to these characteristics, we erect a new oogenus and a new oospecies: Duovallumoolithus shangdanensis oogen. et oosp. nov. The new discovery expands the diversity of Faveoloolithidae.     

Isotopic Geochemistry of Evaporite‐Carbonate Sediments in Majiagou Formation Euxinic Systems with Implications for Evaluating Ordovician Northern Shaanxi Epicontinental Sea,Ordos Basin

正Objective The Ordovician Shaanxi salt basin is located in the junction of the North China Sea and the Qilian Sea.In this basin the Majiagou Formation accumulated more than1000m thick evaporite-carbonate sediments,and this basin is divided into east and west saltern sags(ESS,WSS)according to the characteristics of geochemical analysis(Zhang Yongsheng et al.,2014).Isotope stratigraphy of evaporite sediments represents a fundamental tool in     

3500m岩心钻探装备在油气井勘查中的示范应用

3500 m岩心钻探装备（YDX—6型钻机）是我国自主研发的深部矿产资源勘查技术装备,采用N级口径钻深可达3500 m,其最大特点是采用长油缸钻进和起下钻。本文主要介绍了该钻机在油气井勘查中生产试验情况,同时对矿区地层、钻孔结构、钻进过程、钻进效果、遇到的主要问题及解决办法等进行了介绍。     

贵州松桃高地特大型富锰矿床主要地质特征

位于贵州铜仁松桃国家锰矿整装勘查区内的高地富锰矿床,(332)+(333)类碳酸锰富锰矿石资源量达7 166. 84万吨,锰平均品位25. 75%,矿体平均厚度4. 52 m,富锰矿体赋存于总资源量达1. 61亿吨的高地超大型锰矿床之中,由一个单一的富锰矿体构成,是我国新发现的首个特大型富锰矿床,富锰矿资源量相当于我国富锰矿资源量总和的2倍。成因类型属古天然气渗漏沉积型锰矿床,富锰矿产于古天然气渗漏沉积成矿系统中心相区。高地富锰矿床地处独特的"新月形"南华纪早期李家湾-高地-道坨(Ⅳ级)地堑盆地中心,菱锰矿体中均出现以块状构造夹被沥青充填的气泡状富菱锰矿石。地表燕山期北北东向的断裂构造十分发育,但主要为上陡下缓犁式正断层,未触及高地深部隐伏巨型锰矿体,以致富锰矿体保存亦十分完整,易于开发利用。     

Flooding a landscape: impact of Holocene transgression on coastal sedimentology and underwater archaeology in Kiladha Bay (Greece)

Franchthi Cave, bordering Kiladha Bay, in Greece, is a key archaeological site, due to its long occupation time, from?~?40,000 to?~?5000 year BP. To date, no clear evidence of Neolithic human dwellings in the cave was found, supporting the assumption that Neolithic people may have built a village where there is now Kiladha Bay. During the Neolithic period/Early Holocene, wide areas of the bay were indeed emerged above sea level. Bathymetric and seismic data identified a terrace incised by a valley in?~?1 to 2 m sediment depth. Eight sediment cores, up to 6.3-m-long, were retrieved and analysed using petrophysical, sedimentological, geochemical, and chronostratigraphic methods. The longest core extends into the exposure surface, consisting of a layer of carbonate rubble in a finer matrix, representing weathering processes. Dated organic remains place this unit at?~?8500 cal year BP. It is overlain by stiff silty mud representing an estuarine environment. This mud is capped by reduced sediments with roots marking an exposure surface. A shell-layer, dated to?~?6300 cal year BP, overlies this terrestrial sequence, reflecting the marine transgression. This layer occurs at 10.8 mbsl, 7.7 m deeper than the global sea level at that time, suggesting tectonic subsidence in the area. It is overlain by finer-grained marine carbonate-rich sediments. The top of the core shows traces of eutrophication, pebbles and marine shells, all likely a result of modern anthropogenic processes. These results are interpreted in the context of human occupation: the exposed surface contains pottery sherds, one dating to the Early to Middle Neolithic period, indicating that Neolithic people were present in this dynamic landscape interacting with a migrating coastline. Even if the artefacts are isolated, future investigations of the submerged landscape off Franchthi Cave might lead to the discovery of a Neolithic village, which eventually became buried under marine sediments.     

The Fragmentation in a Protoplanetary Disk and the Properties of the Resultant Self-Gravitating Clumps

We study the fragmentation properties in the protoplanetary disk and properties of the resultant self-gravitating clumps using our newly constructed disk model. Our disk model includes the mass inflall term from a molecular cloud core and the photoevaporation winds effect. We adopt the conventional fragmentation criterion to judge whether a protoplanetary disk can fragment. In this work, we follow our previous work to investigate the properties of the resultant self-gravitating clumps. In our calculation, the initial masses of the resultant self-gravitating clumps lie in the range of tens of M_J to more than one hundred of M_J, where M_J is the Jupiter mass. These initial masses can seemingly account for the masses of extrasolar planets in magnitude. We also calculate the subsequent gas accretion of clumps in 1.27 × 10⁴ yr after the formation of self-gravitating clumps. We find that the subsequent gas accretion of self-gravitating clumps is very efficient, and the clump masses grow to hundreds of M_J and the physical radii R_c of clumps increase to about 10 AU. Additionally, we also calculate the orbital migration of clumps. We find that most clumps have short migration timescale to be accreted onto the protostar, and only a small fraction of clumps have long migration timescale (>10⁶ yr) to successfully become gas giant planets. These results are consistent with previous studies.