内蒙古八大关斑岩型铜钼矿床成岩成矿年代学研究

八大关斑岩铜钼矿床是中国内蒙大兴安岭地区典型的斑岩型铜钼矿床之一。对矿区Ⅱ号岩体不同位置的2件岩石样品采用高精度的LA_ICP_MS锆石U_Pb测年,获得的锆石U_Pb年龄分别为(230.6±2.8)Ma和(230.5±4.4)Ma,两者在误差范围内非常一致,由此确认花岗闪长斑岩体的形成年龄约为230 Ma;对矿区7件辉钼矿样品采用Re_Os同位素测年,获得的Re_Os等时线年龄为(228.7±3.1)Ma,指示了八大关铜钼矿床辉钼矿的沉淀时间约为228.7 Ma。结合矿区岩相学、矿物学特征,辉钼矿呈浸染状分布于花岗闪长斑岩体内,且辉钼矿与黄铜矿密切共生,以及上述2种精确方法获得的年龄在误差范围内的一致性,说明花岗闪长斑岩即为成矿岩体,成岩与成矿大致同时或成矿略晚于成岩,表明八大关铜钼矿床形成于中三叠世,属于印支期成矿。     

Color-Redshift Relations and Photometric Redshift Estimations of Quasars in Large Sky Surveys

With a recently constructed composite quasar spectrum and the X2 minimization technique, we describe a general method for estimating the photometric redshifts of a large sample of quasars by deriving theoretical color-redshift relations and comparing the theoretical colors with the observed ones. We estimated the photometric redshifts from the 5-band SDSS photometric data of 18678 quasars in the first major data release of SDSS and compared them with their spectroscopic redshifts. The difference is less than 0.1 for 47% of the quasars and less than 0.2 for 68%. Based on the calculation of the theoretical color-color diagrams of stars, galaxies and quasars both on the SDSS system and on the BATC system, we expect that we would be able to select candidates of high redshift quasars more efficaciously with the latter than with the former, provided the BATC survey can detect objects with magnitudes fainter than 21.     

基于密集台阵的青藏高原东北缘地壳精细结构及九寨沟地震震源区结构特征分析

基于青藏高原东北缘密集宽频带野外流动观测台阵以及固定台站资料,利用双差层析成像方法对地震位置和研究区的地壳速度结构进行了反演.最终用于联合反演的地震事件合计9644个.结果显示青藏高原东北缘速度结构具有明显的横向不均匀性.从整体上看,青藏高原地区表现为低速异常,鄂尔多斯表现为高速异常,而扬子地块亦表现为高速异常.不同深度处速度结构表现不一致,同一深度处P波速度结构和S波速度结构也有明显差异.由西秦岭北缘断裂带、临潭-宕昌断裂以及礼县-罗家堡断裂围限的地震活动强烈的区域中,P波速度结构由深度0 km时呈现的低速异常,逐渐过渡到5 km时高低速相间分布的特征;而S波速度结构在此区域中,由近地表0 km时高低速相间分布的特征,逐渐过渡到30 km时几乎表现为低速异常.2017年8月8日九寨沟7级地震所在的塔藏断裂、岷江断裂和雪山断裂围限区域,在深度20 km处的P波速度结构和周围存在明显差异,九寨沟地震处于高速异常与低速异常的过渡带内.此外,2013年7月22日发生在青藏高原东北缘的岷漳县6.6级地震,震源区所在的临潭-宕昌断裂附近的P波速度结构在15 km深度处也有明显特征,震源位置所在区域也处于高低速过渡带.该区域这种地壳内部高低速过渡带可能是应力比较容易积累而发生中强地震的一个重要场所.     

Discovery of Three Variable Stars in Direction toward NGC 4565

We present the results of a variable star search in a field next to the edge-on galaxies NGC 4565 from the archive data of Beijing-Arizona-Taibei-Connecticut Multicolor Sky Survey. Three new variable stars were discovered. Based on spectra obtained from the 2.16 m NAOC telescope, we identify two of these as RR Lyr stars and one as a special T Tauri star.     

内蒙古敖包吐铅锌矿床花岗岩类年代学及其地球化学特征

内蒙古敖包吐铅锌矿是大兴安岭南段成矿带上新发现的矿床,成矿与花岗闪长斑岩关系密切。对矿区内花岗闪长斑岩和花岗岩的LA-ICP-MS锆石U-Pb测年结果表明,形成年龄分别为（140.0±0.5）Ma（MSWD=1.3）和（151.6±0.4）Ma（MSWD=1.2）,为晚侏罗世—早白垩世岩浆活动的产物。岩石地球化学测试结果显示,花岗闪长斑岩具有高硅（w（SiO₂）=65.51%~67.85%）,富碱（w（Na₂O+K₂O）=6.86%~7.81%）,贫P₂O₅的特征,A/CNK在0.95~1.02之间,富集微量元素K、Rb、Nd,亏损Ta、Nb、P、Ti,为I型花岗岩。花岗岩的A/CNK值为1.58,属强过铝质岩石。Rb/Sr比值大于0.9,为S型花岗岩。敖包吐花岗岩的全岩Pb同位素组成显示,其²⁰⁶Pb/²⁰⁴Pb为18.398~18.755,²⁰⁷Pb/²⁰⁴Pb为15.534~15.541,²⁰⁸Pb/²⁰⁴Pb为38.386~38.542,铅具有混合来源特征。岩浆很可能来源于岩石圈地幔,并受到一定程度的混染。敖包吐花岗岩类可能与兴蒙造山带东段的后碰撞环境有关,并受到与古太平洋板块俯冲有关的弧后伸展影响。     

内蒙古红花尔基白钨矿矿床流体包裹体研究

红花尔基白钨矿矿床为内蒙古大兴安岭中北段地区新发现的一处钨矿规模接近大型的W-Mo矿床。文章通过系统的岩相学、矿相学、流体包裹体和碳、氢、氧同位素研究,表明红花尔基白钨矿矿床属岩浆期后热液充填-交代矿床,可划分为钾长石、钠长石阶段→白钨矿-石英阶段→辉钼矿-石英阶段→铜、铁、铅、锌硫化物-石英阶段→碳酸盐-石英阶段5个成矿阶段。矿床内的白钨矿、石英以及碳酸盐中的流体包裹体均以富液相气液两相水溶液包裹体为主。白钨矿-石英阶段的均一温度范围为290~395℃,峰值为360~370℃,盐度w(Na Cleq)范围为0.88%~7.02%,峰值为2%~3%,结合包裹体激光拉曼分析,得出与钨矿形成有关的流体为中高温、低盐度的Na Cl-H2O体系的结论。白钨矿和石英的H-O以及碳酸盐的C-H-O同位素特征表明,成矿流体主要是岩浆水,并有少量大气降水的混合。成矿流体为岩浆结晶分异作用形成的富钨等成矿元素的热液。矿区花岗岩的云英岩化可能将钙萃取进入流体,参与白钨矿结晶、沉淀。     

青藏高原东北缘壳幔各向异性研究:基于SKS和Pms震相分析

利用甘肃和青海两省固定宽频带地震台记录的远震波形资料,挑选高质量SKS震相,联合使用最小切向能量方法和旋转互相关方法获得230对高信噪比分裂参数;同时对接收函数中Pms震相随方位角的变化进行拟合,得到了24个台站的地壳各向异性分裂参数.整个区域SKS分裂快波方向均值为123°,Pms分裂快波方向均值为132°,且大部分区域SKS、Pms快波方向与地表构造走向相一致,说明青藏高原东北缘以岩石圈垂直连贯变形为主,地壳上地幔相互耦合.SKS、Pms分裂时差均值分别为1.0s和0.6s,显示地壳各向异性对于SKS分裂时差有较大贡献.昆仑断裂附近Pms、SKS分裂快波方向与昆仑断裂走向基本一致,说明昆仑断裂可能是岩石圈尺度深大断裂;而阿尔金断裂东缘二者快波方向显著差异意味着阿尔金断裂在东缘可能仅为地壳尺度的断裂.     

Evolution of M81 with Exponentially Decreasing Star Formation Rate of PEGASE

Based on the large field multicolor observations of Beijing-Arizona-Taiwan-Connecticut (BATC) program, we obtain the spectral energy distribution (SED) for individual regions of M81. We study the structure and evolution of M81 with an evolutionary population synthesis (EPS) model, PEGASE. We find that the exponentially deceasing star formation rate (SFR) with star formation scale 3 Gyr (hereafter Exp, τ=3 Gyr) gives the best agreement between the model predictions and the observed SEDs. We then obtain the structure, age distribution and evolutionary history of M81. There is a clear age gradient between the central and outer regions. The populations in the central regions are older than 7 Gyr,those in the outer regions are younger, at about 4.5 Gyr. The youngest components in the spiral arms have ages of about 2.5 Gyr or less.