Magnetic Fabric Characteristics of Zhuganhe Loess-Palaeosols Profile on Northern Slope of Dabie Mountains and Their Environmental Significances

大别山北麓竹竿河黄土—古土壤样品的磁组构特征显示,研究剖面0 ～ 1480 cm层段的平均Pj、F值小于1.02,而底部Pj、F大于1.02.F-L、Pj-q组合关系图反映磁化率椭球体为压扁状,磁面理较磁线理发育.磁化率椭球体主轴方位显示0～ 1480cm层段样品的椭球体轴向分布分散,长轴的倾角大于60°,短轴的倾角小于15°,而底部的分布聚集,长轴的倾角一般小于10°,短轴的倾角大于80°,上述特征综合揭示了0 ～ 1480cm层段属于典型风成沉积而底部属于典型水成沉积.磁化率椭球体最大主轴的偏角暗示风成沉积的主导风向为NW-SE方向,而水成沉积的古流向为SW-NE方向,与现代竹竿河水系的方向基本一致.磁化率各向异性最大轴方向的优选方向可能与大别山抬升等构造运动有关.     

广西东部地区金矿的控矿作用和稳定同位素地球化学研究

该区金矿产于寒武系水口群浅变质岩系砂页岩内,矿化类型主要有蚀变岩型和石英脉型两大类。矿体主要受近东西向和北东向两组脆-韧性剪切带控制。硫同位素组成特征表明,硫源应以深源同熔岩浆热液为主,部分来自地层;氢、氧同位隶组成特征反映成矿溶液以岩浆水为主,混有少量变质水和大气降水;铅同位索组成特征表明铅源以深源为主,混有少量壳源物质,矿床具多源成矿特点。硫、铅、氢氧等稳定同位素研究结合矿床地质特征表明,该区金矿具多源、多成因及多期次成矿特征,矿床成因主要有岩浆热液、变质热液和复合叠加成矿,而以后者为主。     

扰动动能与平均动能转换率及其角动量涡旋输送与新疆暴风雪过程的关系

用1995年5月至1999年4月KWBC北半球500 hPa高度场5°×5°客观分析资料,应用谐波分析把等压面高度场沿纬圈作富利叶级数展开,计算逐日25°~80°N每隔5°纬度递增的沿纬圈的扰动动能与平均动能转换率(E)、角动量涡旋输送(RM),分析了E和RM的年、季分布特征及其与新疆暴风雪过程的关系.结果表明:E和RM具有显著的季节变化和周期性;E的正高值中心与新疆暴风雪过程有较好的关系,出现E正高值中心的日期作为预报指标日,其后3~6 d新疆将出现暴风雪天气过程,出现RM负低值中心的日期作为预报指标日,其后3~8 d新疆有暴风雪过程发生;当E的正高值中心和RM的负值中心同时出现时,更确定了新疆暴风雪过程出现的可能性.     

西太平洋俯冲带的演变:来自东北亚陆缘增生杂岩的制约

本文系统总结了东北亚陆缘晚古生代和中生代增生杂岩的构成与形成时代,并结合同时代火成岩组合及其时空变异以及沉积建造组合,重塑了西太平洋板块俯冲带的演变历史.结果表明:①位于佳木斯地块东缘的跃进山杂岩代表了二叠纪俯冲带,它是古亚洲洋构造体制的产物;②侏罗纪增生杂岩代表了侏罗纪俯冲带,与陆缘同期钙碱性火成岩组合以及含煤建造一...     

断盖配置渗漏油气时期确定方法及其应用

为了客观把握含油气系统中断裂处的油气纵向分布规律,在断盖配置渗漏油气机制及其渗漏油气时期构成研究的基础上,通过厘定断裂开始破坏泥岩盖层封闭时刻、断层岩开始封闭时刻和断裂活动停止时刻,确定断盖配置渗漏时期,并结合源岩排烃史,建立了一套确定断盖配置渗漏油气时期的方法,并将其应用于渤海湾盆地南堡凹陷南堡5号油田,研究F3断裂...     

Measurements of visual double stars with PISCO2 at the Nice 76-cm refractor in 2013–2014 (new data) and in 2015

We present relative astrometric and photometric measurements of visual double stars made in 2013–2015, with PISCO2 installed at the 76-cm refractor of Côte d'Azur Observatory in Nice (France). Our observing list contains orbital couples as well as double stars whose motion is still uncertain. Most of the observations were done in 2015, but some other observations of wide couples were done in 2013–2014 (0.3% of the total of the observations). Three different techniques were used for obtaining measurements: lucky imaging, speckle interferometry and the direct vector autocorrelation method. From our observations of 2837 multiple stars, we obtained 5182 new measurements with angular separations in the range of 0 ${}^{″}$.1–32 ${}^{″}$ and an average accuracy of $0^{″}.018$. The mean error on the position angles is 0°.8. Most of the position angles were determined without the usual 180° ambiguity with the application of the direct vector autocorrelation technique and/or by inspection of the Lucky images or the long integration files. We managed to routinely monitor faint systems ( $m_V\approx 9-11$) with large magnitude difference (up to $\mathrm{\Delta }{m}_V\approx 4.5$). We have thus been able to measure 21 systems containing red dwarf stars that had been poorly monitored since their discovery, from which we estimated the stellar masses thanks to Gaia measurements. We also measured the magnitude difference of the two components of 1079 double stars with an estimated error of 0.2 mag. Except for a few objects that are discussed, our measurements are in good agreement with the ephemerides computed with published orbital elements, even for the double stars whose separation is smaller than the diffraction limit. Thanks to good seeing images and with the use of high-contrast numerical filters, we have also been able to obtain 196 measurements with an angular separation smaller than the diffraction limit of our instrumentation, and consistent with those obtained with larger telescopes. We also report measurements of the 164 new double stars that we found in the files obtained during the observations. Finally, from a study of the DR3 Gaia release, it is shown that all the objects of the Tycho Double Star Catalog that we did not resolve in 2015 are probably false detections by Tycho.