Cosmic-ray positrons: are there primary sources?

Galactic cosmic rays consist of primary and secondary particles. Primary cosmic rays are thought to be energized by first order Fermi acceleration processes at supernova shock fronts within our Galaxy. The cosmic rays that eventually reach the Earth from this source are mainly protons and atomic nuclei, but also include electrons. Secondary cosmic rays are created in collisions of primary particles with the diffuse interstellar gas. They are relatively rare but carry important information on the Galactic propagation of the primary particles. The secondary component includes a small fraction of antimatter particles, positrons and antiprotons. In addition, positrons and antiprotons may also come from unusual sources and possibly provide insight into new physics. For instance, the annihilation of heavy supersymmetric dark matter particles within the Galactic halo could lead to positrons or antiprotons with distinctive energy signatures. With the High-Energy Antimatter Telescope (HEAT) balloon-borne instrument, we have measured the abundances of positrons and electrons at energies between 1 and 50 GeV. The data suggest that indeed a small additional antimatter component may be present that cannot be explained by a purely secondary production mechanism. Here we describe the signature of the effect and discuss its possible origin.     

Long-term simulations of thermal and hydraulic characteristics in a mountain massif: The Mont Blanc case study, French and Italian Alps

 The use of hydrothermal simulation models to improve the prediction of water inflows in underground works during drilling is tested in the Mont Blanc tunnel, French and Italian Alps. The negative thermal anomaly that was observed during the drilling of this tunnel in 1960 is reproduced by long-term, transient hydrothermal simulations. Sensitivity analysis shows the great inertia of thermal phenomena at the massif scale. At the time of tunnel drilling, the massif had not reached thermal equilibrium. Therefore, a set of simulation scenarios, beginning at the end of the last glacial period, was designed to explain the anomaly encountered in the tunnel in 1960. The continuous cooling of alpine massifs due to infiltration of waters from the surface has occurred for 12,000 years and is expected to continue for about 100,000 years. Comparisons of water-discharge rates simulated in the tunnel with those observed indicate that this hydrothermal method is a useful tool for predicting water inflows in underground works. Received, May 1998 · Revised, March 1999 · Accepted, April 1999     

Volatile element chemistry during accretion of the earth

We review some issues relevant to volatile element chemistry during accretion of the Earth with an emphasis on historical development of ideas during the past century and on issues we think are important. These ideas and issues include the following: (1) whether or not the Earth accreted hot and the geochemical evidence for high temperatures during its formation, (2) some chemical consequences of the Earth’s formation before dissipation of solar nebular gas, (3) the building blocks of the Earth, (4) the composition of the Earth and its lithophile volatility trend, (5) chemistry of silicate vapor and steam atmospheres during Earth’s formation, (6) vapor - melt partitioning and possible loss of volatile elements, (7) insights from hot rocky extrasolar planets. We include tabulated chemical kinetic data for high-temperature elementary reactions in silicate vapor and steam atmospheres. We finish with a summary of the known and unknown issues along with suggestions for future work.     

吉林省集安市马蹄沟晶质石墨矿地质特征及找矿标志

吉林省集安市马蹄沟晶质石墨矿位于吉林省集安市财源乡马蹄沟一带,文章对该矿床地层、构造、岩浆岩等地质特征及矿床成因进行研究,认为赋存于古元古界集安群荒岔沟组的晶质石墨与硼铁建造、含磷透辉石建造、铀-稀土建造等相应矿床均属于海底火山喷发沉积变质、岩浆热液作用的层控矿床,马蹄沟晶质石墨矿成因类型为沉积变质型晶质石墨矿床。总结该地区晶质石墨矿的找矿标志。     

Northward younging zircon fission‐track ages from 13 to 2 Ma in the eastern extension of the Kathmandu nappe and underlying Lesser Himalayan sediments distributed to the south of Mt. Everest

This study is concerned with the tectono‐thermal history of the Kathmandu nappe and the underlying Lesser Himalayan sediments (LHS) that are distributed in eastern Nepal. We carried out zircon fission‐track(ZFT) dating and obtained 16 ZFT ages from the eastern extension of the Kathmandu nappe, the Higher Himalayan Crystalline, Kuncha nappe, and the Main Central Thrust (MCT) zone. The ZFT ages of the frontal part of the Kathmandu nappe range from 13.0 ±0.8 Ma to 10.7 ±0.7 Ma and exhibit a northward‐younging tendency. These Middle Miocene ZFT ages indicate that the frontal part of the Kathmandu nappe remained at a temperature above 240 °C until the termination of its southward emplacement at 12–11 Ma. The ZFT ages of the LHS range from 11.1 ±0.9 Ma in the southern part of the Okhaldhunga Window to 2.4 ±0.3 Ma of the augen gneiss in the northern margin and also exhibit a northward‐younging age distribution. The ZFT ages show the northward‐younging linear distribution pattern (?0.16 Ma/km) along the across‐strikesection from the frontal part of the Kathmandu nappe to the root zone, without a significant age gap. This distribution pattern indicates that the Kathmandu nappe, the underlying MCT zone, and the Kuncha nappe cooled from the frontal zone to the root zone as a thermally united geologic body at a temperature below 240 °C. An older ZFT age (456.3 ±24.3 Ma), which was partially reset at the axial part of the Midland anticlinorium in the central part of the Okhaldhunga Window, was explained by downward heating from the “hot” Kathmandu nappe. The above evidence supported a model that southward emplacement of the hot Kathmandu nappe resulted in a thermal imprint on the upper part of the LHS; however, the lower part did not reach 240 °C.     

直流弧光放电等离子体CVD金刚石薄膜中的晶体类型与特征

采用自主研制的直流弧光放电等离子体CVD设备,以甲烷和氢气为气源,在YG6硬质合金基体上制备出主显晶面为（100）、（111）以及纳米晶粒的金刚石薄膜涂层。SEM观测其晶体类型主要为立方体、八面体、立方八面体,其中以立方八面体为主。随着碳源气体浓度的增加,金刚石晶体的形态会呈现从八面体一立方八面体一立方体顺序转变的趋势;而薄膜的表面形貌呈现从主显（111）晶面-（111）与（100）晶面混杂-主显（100）晶面顺序转变的特征。此外,CVD金刚石薄膜中还存在有许多类似接触孪晶、贯穿孪晶、复合孪晶,以及球形或聚晶晶粒形态的晶体,并且多数孪晶属于类似（111）复合孪晶结构。     

Insights into the formation of rock varnish in prevailing dusty regions

The characteristics of rock varnish from the Campo de Piedra Pomez (CPP, Andes Argentina) provides new insights into the development of rock varnish under severe dusty conditions. The CPP varnish has been analysed using SEM‐EDAX and Raman techniques. The rock coating is tens of microns in thickness and under the microscope shows a micro to cryptocrystalline appearance and a general granular texture. Silica (quartz, cristobalite and amorphous silica) is the main phase forming these coverings followed by Al, K and Na compounds. Minor Fe oxides and Mn oxides are the source for the orange (Fe) and brown (Fe and Mn) hues of the coating. The results obtained for the CPP coating show that desert varnish developed under dusty circumstances does not have the appearance of typical rock varnish. Textural characteristics include high crystallinity and granular arrangement of the components. Moreover the absence of typical microlaminations is related to the presence of aeolian mineral grains which inhibit their development. The main mechanism of formation of rock varnish under such environmental circumstances is the direct incorporation of aeolian mineral grains into the varnish. However, other physicochemical processes are also required to explain the formation of varnish components such as amorphous silica or iron oxides phases. Although the development of the desert varnish may act as a protector of the underlying pyroclastic rock, the extreme and persistent windy conditions in the CPP field are high enough to weather and erode not only the rock coating but also the original ignimbrite. As other warm desert sites on Earth, the CPP area can also be considered as possible terrestrial analogue to Mars. Some environmental attributes might be similar to those expected on the Martian surface and thus, textural similarities between the CPP varnish and the rock varnish‐like coating of Mars are likely. Copyright © 2014 John Wiley & Sons, Ltd.     

辽东湾北部近海大型水母数量分布和温度盐度特征

通过2009-2011年5月下旬-7月下旬辽东湾北部近海10m等深线内的大型水母调查数据,分析了辽东湾北部近海近三年中大型水母资源状况,并探讨了辽东湾大型水母的生态类型。结果显示:辽东湾北部近海大型水母种类主要有海蜇(Rhopilema esculentum)、沙蜇(Nemopilema nomurai)、白色霞水母(Cyanea nozakii)、海月水母(Aurelia sp.1),海蜇和沙蜇是优势种。海蜇幼水母阶段主要集中分布在5m等深线以内的近岸河口水域,随着个体增大有略向深水或密度较小的水域扩散的趋势,仍主要分布在5m等深线两侧水域,属于高温低盐种类。6月份调查海区中发现大量的沙蜇幼水母,随着沙蜇个体增大,7月份调查海区中沙蜇数量大幅度减少。辽东湾海月水母在南部海域出现较多,2010、2011年在北部近海部分海域出现。白色霞水母近几年来辽东湾出现较少,栖息在盐度较高的水域。辽东湾各种大型水母中,沙蜇的生长速度最快。辽东湾海蜇幼水母、沙蜇幼水母的海区出现时间要晚于黄、东海。     

高喜马拉雅中段基性捕虏体的变质作用及其构造意义

西藏南部聂拉木—樟木剖面出露的高喜马拉雅变质带主要由副变质片麻岩和花岗质片麻岩组成,其次为伟晶岩和淡色花岗侵入体,区域变质程度为角闪岩相。我们对其中的变质基性捕虏体进行详细的变质作用研究,内容包括变质矿物组合,矿物变质反应结构和变质作用的温度—压力条件分析。基性捕虏体中的石榴子石角闪片麻岩和斜长角闪片麻岩均保存了两期变质矿物组合。温度与压力计算结果表明,石榴子石角闪片麻岩早期变质阶段(M1)温度约为829 ℃,压力为7.3 kbar; 晚期(M2)变质温度为625 ℃,压力为4.3 kbar。斜长角闪片麻岩所经历的早期变质阶段(M1)温度约为776 ℃、压力约为10.6 kbar; 晚期(M2)变质温度超过692 ℃,压力为7.4 kbar。石榴子石角闪片麻岩和斜长角闪片麻岩捕虏体均记录了典型的顺时针P-T轨迹,表明高喜马拉雅变质带曾向北俯冲到下地壳深度,之后被抬升到地表剥蚀出露。变质基性捕虏体的研究说明高喜马拉雅结晶岩系经历过较高温度—压力的变质作用,支持了其沿着藏南拆离系和主中央逆冲断裂系向南挤出的大地构造模型。     

四川米仓山地区扬子地台结晶基底的时代归属

主要叙述了米仓山地区太古代地体的构造岩石单元的划分，各单元的岩石组合特征，岩石化学成分，原岩恢复，变质作用，变质相以及主要单元的同位素年龄，证明后河群属太古代地体．