龙门山彭县－灌县断裂的活动构造于地表破裂

2008年5月12日在龙门山发生了8.0级特大地震,彭县－灌县断裂亦发生了同震地表破裂。在前期对龙门山活动构造研究的基础上,汶川特大地震发生后,在灾区进行了多次的野外调查和国际合作考察,重点对汶川地震的地表破裂和地质灾害开展了详细的详细野外地质填图,利用全站仪和GPS对地表破裂进行了精确的测量,研究了的地表破裂地貌错位、构造组合和运动学,已实地测得地表破裂数据70余组(其中彭县－灌县断裂地表破裂数据20余组)。文章以彭县－灌县断裂地表破裂为切入点,在彭县－灌县断裂的关键部位开展了详细的野外地貌测量,主要测量了彭州磁峰、白鹿、绵竹金花和汉旺等地的地表破裂,标定了彭县－灌县断裂破裂带的垂向断距和水平断距,结果表明该地表破裂南西起于彭州磁峰,向北东延伸经白鹿、绵竹金花至绵竹汉旺,全长约 40～50km。地表破裂带沿彭县－灌县断裂带的走向断续分布,单个破裂长度在几米到500余米不等,破裂带切割了多种类型的地貌单元,包括山脉基岩、河流阶地、冲洪积扇、公路、桥梁等,同时也使道路发生拱曲、破坏和桥梁垮塌或移位。其以脆性破裂为特征,以逆冲－右旋走滑为特点,断面倾角较陡,北西盘为上升盘,南东盘为下降盘,垂直位错介于 0.39～2.70m之间,水平位错介于 0.20～0.70m,平均垂直位错为1.6m,平均水平位错为0.6m; 地表最大错动量的地点位于彭州白鹿镇,其中最大垂直断错为 2.7±0.2m,最大水平断错为 0.7±0.2m。垂直位错与水平位错量之间的比值为2 ∶1,表明该地震地表破裂带不仅存在逆冲运动分量和右旋走滑运动分量,而且逆冲运动分量大于右旋走滑运动分量,显示了彭县－灌县断裂破裂带具有以逆冲和缩短作用为主、右旋走滑作用为辅的破裂性质。其与映秀－北川断裂带的地表破裂相比较,该断裂的地表破裂程度远小于映秀－北川断裂带的地表破裂程度,主要表现在地表破裂的长度较短,垂直位错和水平位错也相对较小,而且为以逆冲作用为主。初步研究结果表明,彭县－灌县断裂与映秀－北川断裂地表破裂的平面组合样式显示为两条在平面上近于平行的北东向地表破裂带,其间由一条南北向的次级地表破裂带(小鱼洞断裂)将它们相连结,地下破裂面的剖面组合样式显示为叠瓦状,并在汶川地震震源附近或震源的上方相连的,是同“根”的。     

美国艾奥瓦州文尼希克Lagerst(a)tte及其沉积环境

Lagerstatte是指保存丰富或精美化石、因而具有特殊研究价值的化石层.这类地层所含的化石常具有经矿化的生物软体甚至未变实体,从而为古生物的分类学、组织学、形态学、解剖学、生态学、埋藏学等研究提供了极其难得的材料.近年来发现于美国艾奥瓦州的文尼希克化石层,以其特异保存的多门类不常见化石分子为特征,成为目前仅知的中奥陶世Lagerstatte.这一生物群的发现不仅填补了化石记录中的一些空白,也为中奥陶世的生物辐射事件研究领域打开了一个在赤道附近非正常海洋环境中生存的生物群面貌窗口.而且,其中所含的不同类别矿化生物残留,在有机物的分解、置换以及生物成岩作用等研究中具有重要意义.初步研究表明,文尼希克生物群的生活环境与化石保存,可能与陨石撞击事件有关,从而为奥陶纪生物辐射事件的起因町能与太空星体爆裂有关的理论研究,提供了新的验证材料.     

Glacier reconstruction of La Covacha Massif in Sierra de Gredos(central Spain) during the Last Glacial Maximum

A paleoglacier reconstruction during the Last Glacial Maximum(LGM) is presented for a high mountain area of La Covacha massif in Sierra de Gredos(Iberian Central System) in central Spain. The moraines that, according with the previous literature, had formed during the global LGM, were mapped through photo interpretation of digital aerial photographs and 3D images and detailed field surveys. The topography of the paleoglaciers was estimated using a simple steady-state model that assumed a perfectly plastic ice rheology, reconstructing the theoretical ice profiles and obtaining the ice thickness of the glaciers during the LGM. The reconstruction of the glaciers was carried out using automated and semi-automated physically-based models, obtaining more realistic results with semi-automated models. According to our study, the paleoglaciers in the study area covered an area of 34.79 km~2 during the global LGM, with a maximum ice thickness of 366 meters in La Vega gorge, a total volume of 34.25 × 108 m~3 and a mean paleoELA of 1932 meters. Most of the ice(～82%) was in paleoglaciers facing north, and the rest was in paleoglaciers with other orientations. This emphasizes the importance of orientation in relation to glacier dynamics and ice accumulation. The results obtained in the calculation of paleoELAs during the global LGM in Gredos are average compared to the Iberian mountains of the Northwest where the values were much lower, and with respect to those of the Southwest, much higher. This demonstrates the importance of the exposure of Mediterranean mountains to the humidity sources coming from the NW during the global LGM, as is the case at present.     

计算机随机样品模拟

本文介绍了利用计算机产生给定误差分布的模拟随机样品的一种方法。     

南巴伦支海磁场异常及其与海底地质结构的对比(英文)

对1986—2001年间巴伦支海南部海洋磁力测量的数据处理结果进行了研究。南巴伦支海底的地磁测量揭示出其复杂多期的地质构造结构,其中以两期分离型的构造为主导:(1)具NW走向的里菲-文德期继承性裂谷构造;(2)NE向转换叠加断层正交系统。晚泥盆世碱性侵入体及其相关的金属矿化作用恰位于这些构造系统的交点上。     

VLBI总体条纹拟合方法的应用及其效果

用总体条纹拟合求解各天线的延迟量和条纹率参数,可以提高与小天线相关基线的灵敏度。本文以射电致密陡谱源(CSS)3C43为例,就如何提高数据的信噪比,尽可能多地保留有效数据方面做了成功的尝试.从而十分有效地使用了总体条纹拟合方法.我们认为:对源结构的预知,配以恰当的处理技巧,能获取更多射电源结构信息,改善成图质量.     

Logs and snags in a shola forest of Kerala, India

Introduction Dead wood is an important structural and functional component of a forest ecosystem(Fridman and Welheim 2000). Recent studies also indicate that dead wood is important for maintaining both plant and animal diversity in different forest ecosystems (Grove 2001) as it serve as an energy source (Bray and Gorham 1964) and habitat for an array of organisms. Dead wood can also help reduce erosion, increase soil organic matters (McFee and Stone 1966), and suitable conditions for seedli…     

A photochemical model of the martian atmosphere

The factors governing the amounts of CO, O2, and O3 in the martian atmosphere are investigated using a minimally constrained, one-dimensional photochemical model. We find that the incorporation of temperature-dependent CO2 absorption cross sections leads to an enhancement in the water photolysis rate, increasing the abundance of OH radicals to the point where the model CO abundance is smaller than observed. Good agreement between models and observations of CO, O2, O3, and the escape flux of atomic hydrogen can be achieved, using only gas-phase chemistry, by varying the recommended rate constants for the reactions CO + OH and OH + HO2 within their specified uncertainties. Similar revisions have been suggested to resolve discrepancies between models and observations of the terrestrial mesosphere. The oxygen escape flux plays a key role in the oxygen budget on Mars; as inferred from the observed atomic hydrogen escape, it is much larger than recent calculations of the exospheric escape rate for oxygen. Weathering of the surface may account for the imbalance. Quantification of the escape rates of oxygen and hydrogen from Mars is a worthwhile objective for an upcoming martian upper atmospheric mission. We also consider the possibility that HOx radicals may be catalytically destroyed on dust grains suspended in the atmosphere. Good agreement with the observed CO mixing ratio can be achieved via this mechanism, but the resulting ozone column is much higher than the observed quantity. We feel that there is no need at this time to invoke heterogeneous processes to reconcile models and observations.     

Near-infrared spectroscopy of dark asteroids

Near-infrared (J, H and K bands) spectra of nine dark asteroids (chosen among a sample of supposed primitive objects between C and D classes) have been obtained at the Mauna Kea Observatory (Hawaii) with the 2.2-m telescope using KSPEC as spectrograph. The aim of this work was to search for evidence of the presence of organic materials in these objects as found in other planetary bodies as 5145 Pholus, and in some cometary nuclei. A careful analysis of the data has revealed flat or slightly redder spectra than the solar one for all observed asteroids. No evidence of distinct absorption features was found.     

Nitrogen sulfide in quiescent dark clouds

We report the first detection of interstellar nitrogen sulfide (NS) in cold dark clouds. Several components of the 2 pi 1/2, J = 3/2 --> 1/2 and J = 5/2 --> 3/2 transitions were observed in TMC-1 and L134N. The inferred column density for TMC-1 is NNS approximately 8 x 10(12)cm-2 toward the NH3 peak in that cloud, and in L134N is NNS approximately 3 x 10(12)cm-2 toward the position of peak NH3 emission. These values correspond to fractional abundances relative to molecular hydrogen of fNS approximately 8 x 10(-10) for TMC-1, and fNS approximately 6 x 10(-10) for L134N. The NS emission is extended along the TMC-1 ridge and is also extended in L134N. The measured abundances are significantly higher than those predicted by some recent gas phase ion-molecule models.