河北省石人沟地区麻粒岩-紫苏花岗岩套岩石的矿物学和结晶温压条件

研究区内广泛出露的太古代岩石属于迁西群麻粒岩,包括麻粒岩、紫苏花岗岩、辉石-斜长片麻岩、角闪岩等。对这些岩石中辉石、角闪石、黑云母等矿物的研究结果表明,这些矿物具有明显的麻粒岩相成因特征,角闪石、黑云母同辉石等平衡共存。紫苏花岗岩中矿物除有序度增高外,其他特征与麻粒岩、片麻岩中的矿物相似。 根据矿物对地质温压计计算得到:本区第一期变质作用p-t条件为770-870℃,7.2-8.4k bar第二期为740-760℃,6.6-8.4k bar;矿物氧同位素温度为470-570℃,代表另一次程度较低的变质作用。     

Fluvial channels on Titan: Initial Cassini RADAR observations

Cassini radar images show a variety of fluvial channels on Titan's surface, often several hundreds of kilometers in length. Some (predominantly at low- and mid-latitude) are radar-bright and braided, resembling desert washes where fines have been removed by energetic surface liquid flow, presumably from methane rainstorms. Others (predominantly at high latitudes) are radar-dark and meandering and drain into or connect polar lakes, suggesting slower-moving flow depositing fine-grained sediments. A third type, seen predominantly at mid- and high latitudes, have radar brightness patterns indicating topographic incision, with valley widths of up to 3 km across and depth of several hundred meters. These observations show that fluvial activity occurs at least occasionally at all latitudes, not only at the Huygens landing site, and can produce channels much larger in scale than those observed there. The areas in which channels are prominent so far amount to about 1% of Titan's surface, of which only a fraction is actually occupied by channels. The corresponding global sediment volume inferred is not enough to account for the extensive sand seas. Channels observed so far have a consistent large-scale flow pattern, tending to flow polewards and eastwards.     

非静力平衡层结大气中的重力惯性波和惯性对流

本文根据一些新的流体力学实验结果及某些天气事实,建立了一个非静力平衡条件下旋转地球大气中重力惯性波和惯性对流的理论模型,并分别求出它在稳定层结,中性层结及不稳定层结三种情况下的点源扰动函数形式的解。 分析解的性质得知,中性及弱不稳定大气中可以激发一种主要由地球旋转惯性决定的大幅度垂直速度振动,其周期大于(至少等于)地球在该纬度的惯性周期2π/f。这也许能说明文献[1]所发现的那种准周期性惯性对流的某些动力性质。在稳定层结流体中,地球旋转参数对流体重力振荡的频率影响不大,层结越稳定,越类似于单纯的重力振荡,只有在层结接近中性时,f对重力振荡的频率修正作用才明显起来。 最后给出不同纬度处不稳定层结大气中所能产生的惯性对流的最大临界尺度。     

苏北盆地高邮凹陷侵入岩形成时期及成因机制探讨

通过对苏北盆地高邮凹陷的上、下两套侵入岩与断层的错断及其与构造运动强弱的关系、与油气成藏期的关系以及侵入岩的平面分布研究,提出了侵入岩的侵入时期为三垛期,而非盐城期。通过对晚白垩世以来苏北盆地各期构造运动及其伴生火山活动的分析,认为高邮凹陷侵入岩的成因主要由于晚始新世至渐新世末,该区发生了三垛运动,并发育一系列北东及北西向的断裂构造,导致了岩浆活动,并以侵入特征为主。     

REANALYSIS OF PRINCIPAL COMPONENT ANALYSIS TO RESUME PAST VEGETATION AND ENVIRONMENT——Taking Fenzhuang Profile in Beijing as an Example

Ｉ．ＩＮＴＲＯＤＵＣＴＩＯＮＡｔｐｒｅｓｅｎｔ,ｇｌｏｂａｌｃｌｉｍａｔｅｃｈａｎｇｅｈａｖｅｂｅｅｎｗｉｄｅｌｙｐａｉｄａｔｅｎｔｉｏｎｔｏｉｎｔｅｒｎａｔｉｏｎａｌｙ．Ｃｌｉｍａｔｉｃａｎｄｅｎｖｉｒｏｎｍｅｎｔａｌｃｈａｎｇｅｓｆｒｏｍｌｏｃ...     

《华北地震科学》征稿简则

一、《华北地震科学》是河北省地震局主办的地震科学综合性学术季刊。每季末出版。主要刊登地震学方面具有创新性的研究成果,也登载一些与地震有关的地球物理、地震地质、地震工程等方面的学术论文及与地震科学有关的实验、观测、考察、问题讨论等方面的论文。     

A GRAPHIC METHOD TO AID SPECIFIC DETERMINATION OF FUSULINOIDS AND SOME RESULTS OF ITS APPLICATION TO THE FUSULIN?E FROM N. CHINA.——WITH 2 PLATES AND 20 TEXT-FIGURES.

本篇分为三节:第一节论研究(竹廷)蜗之方法及其各部分之名称;并猎取古生物学家迄今历史之结果而加以批评。第二节专述中国北部已发见之(竹廷)蜗。第三节讨论本篇所述各种(竹廷)蜗生存之时代及其棲息流徙之情形。     

中国大陆科学钻探工程主孔2000～3000米正、副片麻岩的地球化学性质及其成因机制

中国大陆科学钻探工程主孔(CCSD-MH)2000.0-3000.0米深度范围内出露的岩心以正、副片麻岩为主,夹有薄层榴辉岩和斜长角闪岩等。地球化学研究结果表明,主孔20000.0-3000.0米之间的正片麻岩SiO2含量普遍偏高,为73.26%～78.17%之间,平均值76.40%;Al2O3含量为11.30%-13.66%。TiO2、Fe2O3、FeO、MnO和MgO含量则明显偏低,其中Fe2O3总量为0.39%-1.71%,FeO=0.20%-1.49%,MgO=0.01%-0.06%。CaO含量为0.19-1.41%,Na2O和K2O含量分别为3.38%-5.35%和1.31%-4.87%。正片麻岩的稀土元素和微量元素配分模式可分为三种类型。第一类表现出较强的轻、重稀土元素分馏,具有中等的负Eu异常,Eu/Eu*=0.39-0.64;洋脊玄武岩(MORB)标准化蛛网图表现出强烈富集大离子亲石元素(K、Rb、Ba、Th)的特点,显示明显的正Ba异常,Ba/Ba*=1.09-2.34,高场强元素Ti、Nb和Ta呈明显的负异常。第二类正片麻岩具有明显的负Eu异常,Eu/Eu*=0.39-0.41,稀土元素配分曲线具有明显右倾斜的特点,轻稀土元素明显富集,而重稀土元素明显亏损;洋脊玄武岩(MORB)标准化蛛网图与第一类正片麻岩比较相似,但却具有中等的负Ba异常,Ba/Ba*=0.57-0.67。第三类正片麻岩主要为含磁铁矿二长花岗质片麻岩,稀土元素球粒陨石标准化曲线呈“V”字型特点,具有异常强烈的负Eu异常,Eu/Eu*普遍低于0.11;洋脊玄武岩(MORB)标准化蛛网图显示出强烈富集大离子亲石元素(K、Rb、Th)的特点,具有异常强烈的负Ba异常,Ba/Ba*=0.03-0.21。2000.0-3000.O米深度范围内的正片麻岩具有多成因的特点,部分正片麻岩具有A型花岗岩的地球化学特征,反映它们有可能形成于板内的构造环境;而另一部分的原岩则可能形成于陆缘火山弧的构造环境。主孔2000.0-31000.0米深度范围内副片麻岩SiO2含量明显低于正片麻岩,Al2O3、Fe2O3 FeO、MgO和CaO含量则明显偏高,而Na2O和K2O含量则与正片麻岩大体相当。其中SiO2含量为64.21%-74.12%;Al2O3含量为13.06%-15.38%,Fe2O3 FeO含量为1.61%-4.92%;CaO含量为1.10%～3.27%,Na2O和K2O含量分别为3.68%-5.39%和2.46%-5.85%。副片麻岩稀土元素配分模式和洋脊玄武岩(MORB)标准化蛛网图与正片麻岩也存在明显差异。其中稀土元素配分模式表现出一定程度的轻、重稀土元素分馏,大多数样品具负Eu异常,Eu/Eu*=0.56-0.93之间,但远不及正片麻岩的明显;洋脊玄武岩(MORB)标准化蛛网图则显示出富集大离子亲石元素(K、Rb、Ba、Th)的特点,具有异常明显的正Ba异常,且变化范围较大,Ba/Ba*=1.02-4.83之间,高场强元素如Ti、Nb和Ta呈现负异常的特点。副片麻岩的原岩可能是形成于被动大陆边缘的一套典型的沉积岩或变沉积岩。SHRIMPU-Pb定年结果表明,主孔副片麻岩锆石微区记录了十分复杂的年代学信息。继承性碎屑锆石核部的年龄(206Pb/238U的年龄)为313-659Ma,表明原岩继承性碎屑锆石来源的复杂性,以及部分碎屑锆石在超高压变质过程中发生不完全重结晶,导致年龄变新;在含柯石英锆石微区记录的超高压变质年龄(206Pb/238U的年龄)为220-236Ma,加权平均值为227±5Ma;而锆石晶体边部所记录的退变质年龄(206Pb/238U的年龄)为209-219Ma,加权平均值为214±6Ma,上述含柯石英锆石微区和锆石边部的SHRIMPU-Pb定年结果分别与主孔CCSD-MH中的正片麻岩锆石微区获得的超高压变质年龄(227±2Ma)和角闪岩相退变质年龄(209±3Ma)十分接近,这进一步证明了中国大陆科学钻探工程主孔中的正、副片麻岩的原岩曾一起发生深俯冲,并经历了新三叠纪的超高压变质作用。     

Cassini/VIMS hyperspectral observations of the HUYGENS landing site on Titan

Titan is one of the primary scientific objectives of the NASA–ESA–ASI Cassini–Huygens mission. Scattering by haze particles in Titan's atmosphere and numerous methane absorptions dramatically veil Titan's surface in the visible range, though it can be studied more easily in some narrow infrared windows. The Visual and Infrared Mapping Spectrometer (VIMS) instrument onboard the Cassini spacecraft successfully imaged its surface in the atmospheric windows, taking hyperspectral images in the range 0.4–5.2 μm. On 26 October (TA flyby) and 13 December 2004 (TB flyby), the Cassini–Huygens mission flew over Titan at an altitude lower than 1200 km at closest approach. We report here on the analysis of VIMS images of the Huygens landing site acquired at TA and TB, with a spatial resolution ranging from 16 to14.4 km/pixel. The pure atmospheric backscattering component is corrected by using both an empirical method and a first-order theoretical model. Both approaches provide consistent results. After the removal of scattering, ratio images reveal subtle surface heterogeneities. A particularly contrasted structure appears in ratio images involving the 1.59 and 2.03 μm images north of the Huygens landing site. Although pure water ice cannot be the only component exposed at Titan's surface, this area is consistent with a local enrichment in exposed water ice and seems to be consistent with DISR/Huygens images and spectra interpretations. The images show also a morphological structure that can be interpreted as a 150 km diameter impact crater with a central peak.