The 825-1110 angstroms EUV spectrum of Venus

On 15 August 1994 we launched the EUVS sounding rocket payload to observe the 825-1110 angstrom region of Venus's far ultraviolet airglow spectrum. The EUVS telescope/spectrograph obtained good data at five times higher spectral resolution than was previously available in the far ultraviolet. We present these data and compare our results to those obtained by the Galileo UVS and Venera 11/12 UV spectrophotometers. We identify several new spectral emission features, including both singly ionized nitrogen and molecular nitrogen in Venus's spectrum. We also see evidence for electron-impact-induced emission from CO. Finally, the EUVS data indicate that the "Ar" emissions detected in Venus's far ultraviolet spectrum by Venera 11/12 spectrophotometers are in fact not due to argon, thus eliminating the discrepancy between in situ and remote sensing measurements.     

The infrared spectra of nitriles and related compounds frozen in Ar and H2O

We present the 2320-2050 cm-1 (4.31-4.88 micrometers) infrared spectra of 16 solid-state nitriles, isonitriles, and related compounds in order to facilitate the assignment of absorption features in a spectral region now becoming accessible to astronomers for the first time through the Infrared Space Observatory (ISO). This frequency range spans the positions of the strong C triple bond N stretching vibration of these compounds and is inaccessible from the ground due to absorption by CO2 in the terrestrial atmosphere. Band positions, profiles, and intrinsic strengths (A values) were measured for compounds frozen in Ar and H2O matrices at 12 K. The molecular species examined included acetonitrile, benzonitrile (phenylcyanide), 9-anthracenecarbonitrile, dimethylcyanamide, isopropylnitrile (isobutyronitrile), methylacrylonitrile, crotononitrile, acrylonitrile (vinyl cyanide), 3-aminocrotononitrile, pyruvonitrile, dicyandiamide, cyanamide, n-butylisocyanide, methylisocyanoacetate, diisopropylcarbodiimide, and hydrogen cyanide. The C triple bond N stretching bands of the majority of nitriles fall in the 2300-2200 cm-1 (4.35-4.55 micrometers) range and have similar positions in both Ar and H2O matrices, although the bands are generally considerably broader in the H2O matrices. In contrast, the isonitriles and a few exceptional nitriles and related species produce bands at lower frequencies spanning the 2200-2080 cm-1 (4.55-4.81 micrometers) range. These features also have similar positions in both Ar and H2O matrices, and the bands are broader in the H2O matrices. Three of the compounds (pyruvonitrile, dicyandiamide, and cyanamide) show unusually large shifts of their C triple bond N stretching frequencies when changing from Ar to H2O matrices. We attribute these shifts to the formation of H2O:nitrile complexes with these compounds. The implications of these results for the identification of the 2165 cm-1 (4.62 micrometers) "XCN" interstellar feature and the 4550 cm-1 (2.2 micrometers) feature of various objects in the solar system are discussed.     

通过地理信息系统评估地震破坏和损失

引言在评价地震对某一地区的社会经济影响时,评估地震造成的破坏和损失是头等重要的。除对减轻风险的工作和应急准备提供帮助以外,地震破坏和损失分析还用于鉴别高危险性的设施,也即那些为某一区域提供基本服务的建筑和生命线单元或     

中尺度对流系统和闪电

1.引言每年春夏时节美国包括大平原和东南地区在内的广大地区的总降水量与中尺度对流系统(Mesoscale Convective Systems,以下简称MCS)过境有关.MCS定义为持续时间至少几小时且在生命史内具有明显对流活动的大范围降水系统(水平尺度为100-500km).根据定义,MCS包括超级单体雷暴,伴有层状云降水区的飑线以及中尺度对流复合体(MCC).MCC是根据云顶最低温度和特定温度阈值的覆盖范围来定义的(Maddox,1980).MCC中的对流单体的分布较为     

西澳大利亚大规模的剪切带及其对太古代金矿化的意义

很多太古代后生的大型金矿床都与绿岩带中的区域性线构造有着广泛的空间上的联系,尽管详细地看来,它们是位于次级脆—韧性的断层构造中。来源于地球深处的热液在向地壳上部运移的过程中经过了一个复杂的通道,并与不同的岩石和变质溶液发生了一种重新均衡的过程。在角闪岩和绿色片岩带中或在其下面的温度和压力条件有利于次级脆—韧性和脆性构造的形成,这种构造是金矿最易形成的部位,大多数矿都位于这里。区域性韧性构造和较脆的次级构造之间的物理梯度使得热液在局部的范围内不稳定地流入较脆的次级构造之中,在这里较低的温度和具有高的Fe/(Fe+Mg)比值的合适的主岩有利于金矿的沉积。金矿的各种同位素和地球化学特征反映了金矿具有多种来源并与地壳中的岩石不断地发生过再平衡作用。     

根据海底地震仪观测资料确定克里特海岩石层S波的衰减

１９８７年在克里特海设置了５台海底地震仪。在９天的时间里记录到了４３０个地方震，测定了其中８５个微震的震中。根据海底地震仪和一些陆地上的希腊台站同时记录到的１４个地震的数据，发现了震级ＭＬ与海底地震仪记录上的地震持续时间之间的相关关系，给出了由海底地震仪记录到的ＭＬ＝２－４地震的震级－频度关系。绘制了描述克里特海岩石层体波振幅衰减的曲线图。通过对比实验和理论振幅曲线，对品质因素作了评估。计算出克里