闽西北铅锌矿成矿特征及控矿条件浅析

闽北地区属华南褶皱系的一部分,其中铅、锌为区内优势矿种,广泛分布于前震旦纪变质岩系中,尤其以前震旦纪龙北溪组的黑云斜长变粒岩、云母片岩、石英片岩中最为多见。其成矿特征可分为热液型铅锌矿床、充填交代型铅锌矿床及沉积变质热液叠加型铅锌矿床。其形成受地层、岩浆、构造（以断裂构造为主）控制较为明显,前震旦系变质岩系中的绿片岩、压扭性断裂及前震旦系变质岩系与岩体的接触带及其附近应是本区铅锌矿床找矿的主要方向。     

基于洪峰模数的山洪灾害雨量预警指标研究

山洪灾害预警是防御山洪的重要非工程措施,雨量预警指标是山洪灾害预警的关键。目前的雨量预警指标计算方法对水文气象资料条件以及模型建模率定都有很高的要求,并不适用于基层防汛人员。因此,本文基于全国山洪灾害调查评价成果数据,提出了一种运用洪峰模数计算雨量预警指标的简便、易用的方法。该方法以小流域洪水计算推理公式为基础,将公式中流量与流域面积的比值用洪峰模数表示,得到基于洪峰模数的临界雨量估算公式,并考虑流域土壤含水量等因素,分析临界雨量变化阈值,最终得到雨量预警指标。本文以云南省绥江县双河小流域为例,计算结果显示不同时段（1 h、3 h、6 h）净雨量和预警时段呈线性关系。降雨损失计算中洼地蓄水和植被截留在不同时段相同,土壤下渗在不同的时段不相同。在此基础上,计算不同土壤含水量条件下,不同时段的雨量预警指标。最后,对临界流量、降雨损失和预警指标进行了合理性分析,结果显示预警指标和调查评价结果及实测降雨都比较接近,计算的预警指标合理。本研究为基层山洪灾害预警提供了一种快速、便捷的预警指标计算方法,为预警指标计算提供技术支持。     

毛乌素沙漠边缘地区春末夏初沙尘暴天气的物理量场结构

沙尘暴天气是毛乌素沙漠边缘内蒙古、甘肃、宁夏、陕西等地区春末夏初特有的一种灾害性天气。应用欧洲中心再分析资料的气压场和各种物理量场,选取了5个沙尘暴个例,分析了沙尘暴时期各层气压场的特征和物理量的空间结构。结果表明：蒙古高压是影响沙尘暴的主要天气系统。在沙尘暴发生时,蒙古高压前部整层都为宽广而强劲的西北气流,从地面可伸展到200 hPa附近,其物理属性是干、冷,其前部近乎于东北—西南向的区域,是锋区的密集带,也是各种物理量表现最为敏感的区域,垂直速度场为上升运动区,涡度场为正涡度区,高—低层散度差值场为正值,这些物理量都为沙尘暴的发生起到了推动和加强作用。     

Non-Gaussian distribution and clustering of hot and cold pixels in the five-year WMAP sky

We present measurements of the clustering of hot and cold patches in the microwave background sky as measured from the Wilkinson Microwave Anisotropy Probe 5-year data. These measurements are compared with theoretical predictions which assume that the cosmological signal obeys Gaussian statistics. We find significant differences from the simplest Gaussian-based prediction. However, the measurements are sensitive to the fact that the noise is spatially inhomogeneous (e.g. because different parts of the sky were observed for different lengths of time). We show how to account for this spatial inhomogeneity when making predictions. Differences from the Gaussian-based expectation remain even after this more careful accounting of the noise. In particular, we note that hot and cold pixels cluster differently within the same temperature thresholds at few-degree scales. While these findings may indicate primordial non-Gaussianity, we discuss other plausible explanations for these discrepancies. In addition, we find some deviations from Gaussianity at sub-degree scales, especially in the W band, whose origin may be associated with extragalactic dust emission.     

胶莱盆地东缘早白垩世莱阳群沉积序列及岩相古地理

胶莱盆地东缘早白垩世早期莱阳群沉积体现了湖盆由开始形成—鼎盛—萎缩消亡的全过程,发育由冲洪积相—湖相—三角洲相—河流相沉积的完整序列,且由东至西,由湖相到河流相逐渐过渡;古水流方向显示莱阳期盆地中心位于朱吴断裂、海阳断裂带之间,以断裂带为界,以西水流方向大致为由NW至SE向,以东水流方向则为由SE至NW向;早白垩世早期莱阳期盆地的形成与演化明显受区域性牟(平)-即(墨)断裂带活动所控制。     

济南东部埠村超单元及其就位机制

分布于济南东部六山圈—大有一带的侵入岩,为燕山早期同一岩浆热事件多次侵入形成的杂岩体,依其形成顺序可划分为山张庄、西杜、大有、赵家鹊山四个单元,归并为埠村超单元。该超单元的形成与幔源基性岩浆上侵及同源岩浆分异产生的中偏基性—中性岩浆多次侵入有关,属热气球式膨胀与火山口塌陷复合就位机制。     

Early development of Chondrus ocellatus Holm （Gigartinaceae, Rhodophyta）

1 INTRODUCTION Red algae C. ocellatus lives in temperate zone of coastal area, and inhabits at substrates from high tide to low tide regions. Its life history is composed of three phases: tetrasporophyte, gametophyte and carposporophyte. Chondrus is one o…     

基于非对称传感器的地震预警与烈度速报综合用烈度仪

对典型的地震预警与烈度速报方法进行分析,提出了基于非对称传感器的地震预警与烈度速报综合用烈度仪,其由非对称结构的三分量传感器和基于ARM嵌入式系统的专用数据采集器组成。经过测试,该地震烈度仪的专用数据采集器具有大于107 dB的动态范围;其非对称三分量传感器结构中,所选的单分量B类传感器的加速度误差小于0.8%,动态范围大于105 dB,而所选的三分量C类传感器的加速度误差小于5%,动态范围大于61 dB。该地震烈度仪的各项指标均满足地震预警与烈度速报综合应用的各项技术要求,且功耗低、成本低,适合于高密度布设。     

基于危险度区划的县级区域降雨引发滑坡的风险预警方法——以四川省米易县降雨滑坡为例

降雨滑坡预警在世界上开展广泛,但对小区域的降雨滑坡风险进行预警尚不多见。以通用的风险定义为基础,首先对目标区域——四川省米易县的地质灾害进行调查,以典型滑坡进行反演,获得灾害的本底因素,按贡献率权重叠加法进行危险度分区;通过对承灾体的调查确定承灾对象,并将各承灾对象按密度由行政界限向1km×1km的网格单元转化后叠加形成易损度分区。二者相乘完成风险分区。对研究区域近5年逐日降雨数据与172条地质灾害记录进行分析,按前期日降雨量模型得到降雨阈值,根据滑坡空间概率和降雨引发滑坡的时间概率叠加的结果,得到研究区域的降雨滑坡概率,对照风险分区,完成风险预警。     

3. Solar System Formation and Early Evolution: the First 100 Million Years

The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is its relation with the circumstellar disks that are ubiquitous around young low-mass stars today? Is it possible to define a “time zero” (t ₀), the epoch of the formation of the solar system? Is the solar system exceptional or common? This astronomical chapter focuses on the early stages, which determine in large part the subsequent evolution of the proto-solar system. This evolution is logarithmic, being very fast initially, then gradually slowing down. The chapter is thus divided in three parts: (1) The first million years: the stellar era. The dominant phase is the formation of the Sun in a stellar cluster, via accretion of material from a circumstellar disk, itself fed by a progressively vanishing circumstellar envelope. (2) The first 10 million years: the disk era. The dominant phase is the evolution and progressive disappearance of circumstellar disks around evolved young stars; planets will start to form at this stage. Important constraints on the solar nebula and on planet formation are drawn from the most primitive objects in the solar system, i.e., meteorites. (3) The first 100 million years: the “telluric” era. This phase is dominated by terrestrial (rocky) planet formation and differentiation, and the appearance of oceans and atmospheres.