Stratospheric Aerosol Extinction Profile Retrieval from SCIAMACHY Limb Measurements

Stratospheric aerosol extinction profiles are retrieved from Scanning Imaging Absorption Spectrome- ter for Atmospheric Cartography （SCIAMACHY） limb scatter measurements. In the process of retrieval, the SCIATRAN radiative transfer model is used to simulate the limb scattering radiation received by the SCIAMACHY instrument, and an optimal estimation algorithm is used to calculate the aerosol extinction profiles. Sensitivity analy- ses are performed to investigate the impact of the surface albedo on the accuracy of the retrieved aerosol extinction profiles in the northern midlatitudes. It is found that the errors resulting from the bias of the assumed surface albedo in the retrieval are generally below 6%. The retrieved SCIAMACHY aerosol extinction profiles are compared with corresponding Stratospheric Aerosol and Gas Experi- ment （SAGE） II measurements, and the results indicate that for the zonal mean profiles, the SCIAMACHY retrievals show good agreement with SAGE II measurements, with the absolute differences being less than 2.3 × 10-5 km-1 from 14-25 km, and less than 5.9×10-6 km-1 from 25-35 km; and the relative differences being within 20% over the lati- tude range of 14-35 km.     

湖北崇阳二叠纪—三叠纪之交生物灭绝和沉积微相演化

二叠纪—三叠纪之交,湖北崇阳地区处于浅水碳酸盐岩台地环境.二叠纪末的全球事件在该剖面的沉积微相和生物演化上均留下了清楚的记录.二叠纪末生物大灭绝之前,崇阳地区为典型的正常浅海台地环境,生物种类多样,数量丰富,主要生物化石有钙藻、有孔虫、腕足、棘皮类和海绵等.生物大灭绝之后,钙藻、(筳)类、棘皮类、海绵、绝大部分有孔虫开始消失,取而代之的是个体微小的腹足、介形虫和大量的蓝细菌化石.大灭绝界线之上,首先出现的是25 cm厚的纹层状的微生物岩,含较丰富的种类单调的有孔虫化石.之后逐渐相变为花斑状微生物岩和穹隆状微生物岩,厚度分别为6.4,2.3m.不同类型微生物岩在结构构造和生物组成上存在差别.微生物岩沉积结束之后,则相变为浅滩相鲕粒灰岩.共划分出3种沉积相,即开阔台地相、潮坪相和浅滩相.崇阳剖面的生物灭绝和沉积微相变化是二叠纪—三叠纪之交浅水台地环境生物与环境过程的典型代表,为认识二叠纪末浅海沉积相演化和全球事件提供了新材料.     

湖南桃源郝坪奥陶系五峰组顶部斑脱岩LA-ICP-MS锆石U-Pb年龄

为了认识奥陶纪-志留纪之交的火山活动及事件年龄,对湖南桃源郝坪剖面的斑脱岩进行了LA-ICP-MS锆石U-Pb定年.结果表明,五峰组顶部斑脱岩LA-ICP-MS锆石U-Pb年龄为442.2±8.1 Ma,该年龄反映了扬子地区奥陶纪-志留纪之交火山活动的时代,与国际地层委员会公布的奥陶系-志留系界线年龄(443.7±1.5Ma)相一致,同属晚奥陶世.奥陶纪-志留纪之交的火山活动对于探讨晚奥陶世生物绝灭、沉积环境变化与年代地层对比具有重要的意义.     

Hydrogen and Oxygen Isotopes of Fluid Inclusion in Halite,Northern Shaanxi Salt Basin China

正The Ordovician was an important transitional period for global climate and organic evolution,the global was in the flood and glacial,Onganism was extinction(Zhan,2007;Trotter et al.,2008;Axel et al.,2010).Under the influence     

不同场景下的交通能见度估算模型的应用

能见度监测是交通出行安全的重要保障,尤其对机场和高速公路的大范围低能见度的监测和预警更为重要.在传统人工目测方法的基础上,以激光透射能见度仪为代表的仪器测量方法更为准确,但存在探测范围小、维护成本高、全覆盖耗资大的局限性.为了克服以上缺陷,使交通能见度的估计更为灵活、高效,本文基于机场气象站点观测数据、机场大雾以及高速...     

尘埃消光对伽玛射线暴余辉的影响

为了研究尘埃消光对伽玛射线暴余辉的影响,基于严格的Mie理论和最新的星际尘埃光学性质,进行了高精度的数值计算,并分析具有不同物理参数的尘埃所产生的消光曲线.结果表明,介质密度和金属丰度是决定消光总量的主要物理参数,而尘埃颗粒大小的分布则是产生不同消光曲线轮廓的重要物理参数.如果尘埃颗粒相互聚集形成导致尺度增大,将产生较平或者较灰的消光曲线,同时绝对总量将减少;相反,如果尘埃颗粒由于某种原因发生离解导致尺度变小,将产生较陡的消光曲线,同时消光总量将增加.这些结果将对理解光学暗暴的形成机制提供重要的启示.     

GRB‐selected galaxies

We describe the current status and recent results from our Swift/VLT legacy survey, a VLT Large Programme aimed at characterizing the host galaxies of a homogeneously selected sub‐sample of Swift gamma‐ray bursts (GRBs). The immediate goals are to determine the host luminosity function, study the effects of reddening, determine the fraction of Lyα emitters in the hosts, and obtain redshifts for targets without a reported one. We have defined a very carefully selected sample, obeying strict and well‐defined criteria: 68 targets in total. Among the preliminary results is a large optical detection rate, the lack of extremely red objects (only one possible case in the sample), and 10 new GRB redshifts with the mean redshift of the host sample assessed to be 〈z 〉 ≳ 2 (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

湖南慈利礁相二叠系-三叠系界线地层及其对大灭绝事件的启示

湖南慈利康家坪长兴组礁相地层上直接覆以大冶组"错时相"钙质微生物岩、鲕状灰岩、蠕虫状灰岩等沉积物。岩相、生物地层和碳同位素演变表明大灭绝事件处地层连续;剖面上长兴期末的化石分布呈现一种单幕式灭绝型式和过程;占据大灭绝后浅水碳酸盐相的是一种以微生物主导的"异常生态系"。     

The 2200 Å bump and the interstellar extinction curve

The 2200 Å bump is a major figure of interstellar extinction. However, extinction curves with no bump exist and are, with no exception, linear from the near‐infrared down to 2500 Å at least, often over all the visible‐UV spectrum. The duality linear versus bump‐like extinction curves can be used to re‐investigate the relationship between the bump and the continuum of interstellar extinction, and answer questions as why do we observe two different kinds of extinction (linear or with a bump) in interstellar clouds? How are they related? How does the existence of two different extinction laws fits with the requirement that extinction curves depend exclusively on the reddening E (B – V) and on a single additional parameter? What is this free parameter? It will be found that (1) interstellar dust models, which suppose the existence of three different types of particles, each contributing to the extinction in a specific wavelength range, fail to account for the observations; (2) the 2200 Å bump is very unlikely to be absorption by some yet unidentified molecule; (3) the true law of interstellar extinction must be linear from the visible to the far‐UV, and is the same for all directions including other galaxies (as the Magellanic Clouds). In extinction curves with a bump the excess of starlight (or the lack of extinction) observed at wavelengths less than λ = 4000 Å arises from a large contribution of light scattered by hydrogen on the line of sight. Although counter‐intuitive this contribution is predicted by theory. The free parameter of interstellar extinction is related to distances between the observer, the cloud on the line of sight, and the star behind it (the parameter is likely to be the ratio of the distances from the cloud to the star and to the observer). The continuum of the extinction curve and the bump contain no information on the chemical composition of interstellar clouds. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Instellar extinction curves originated in single clouds

In der Arbeit wird gezeigt, daß zwischen den Extinktionskurven heller, relativ gering entfernter Sterne große Unterschiede bestehen, die mögficherweise dadurch verursacht werden, daß nur eine interstellare Wolke mit spezifischen Eigenschaften die Extinction verursacht. Die Unterschiede betreffen sowohl den Verlauf der Extinktionskurve als auch den R-Wen. Die Unterschiede in den Extinktionskurven sind korreliert mit den Inten-sitatsverhaltnissen der diffusen interstellaren Banden bei 578 nm und 579,7 nm. Es wird geschlußfolgert, daß sich die physikalischen Eigenschaften einzelner interstellarer Wolken stark voneinander unterscheiden und die aus den Spektren stark verfärbter Sterne gewonnenen Extinktionskurven nur einen schlecht spezifizierbaren Mittelwert der Verhältnisse in den Einzelwolken darstellen. Die abgeleiteten individuellen Extinktionskurven sollten mit theoretischen oder aus Laborexperimenten abgeleiteten Kurven verglichen werden.