二叠纪-三叠纪之交双壳类的灭绝与复苏过程

为了建立早-中三叠世双壳类的残存-复苏模式及深入探讨双壳类迟缓复苏的原因,对全球范围内该时期双壳类属的 时限分布进行了统计.总体来看,3个亚纲(Pteriomorphia、Palaeotaxodont和Heteroconchia亚纲)和5种生活方式(外栖活动 类、外栖固着类、半内栖类、内栖浅掘穴类和内栖深掘穴类)的双壳类均展示出了一致的规律,属级分异度直到中三叠世Anisian 期才恢复到晚二叠世末生物大灭绝之前的水平.二叠纪残存类型在早-中三叠世双壳类中所占的比例逐步降低,从占过 渡层的77.3%降低到了中三叠世Anisian期的33.7%,指示双壳类的缓慢复苏过程.而在整个早三叠世的漫长复苏期中,双壳 类仅遭受背景灭绝,表明双壳类的迟缓复苏受限于长时期的高压环境,随着海洋环境的逐步好转,才逐渐出现新的类型.      

Infrared photometry of AGB stars

The goal of this article is to show that, if one avoids star forming regions, mass-losing AGB stars can generally be selected from the data that will be provided by the near-infrared surveys which are presently considered. Also, if IRAS data are available, the separation between carbon-rich and oxygen-rich stars can be operated by their positions in infrared colour diagrams. In extragalactic systems, red supergiants can be discriminated from AGB stars by their luminosities.based on observations obtained with the ESO 1-m telescope     

降水现象对大气消光系数和能见度的影响

大气中各种粒子对大气消光系数和能见度有不同程度影响,除气溶胶粒子外,降水粒子对能见度影响也不可忽视。为了解降水粒子对能见度的影响,确定能见度变化与降水现象之间的关系,该文在分析降水粒子的大小、速度、形状、谱分布、光学特性等特征的基础上,忽略气溶胶粒子的影响,建立基于实测谱分布的降水与能见度的理论模型,讨论不同类型降雨、降雪对大气消光系数和能见度的影响。同时选取Parsivel降水粒子谱仪在南京地区的降雨和降雪观测记录,利用实测数据来对比验证本文所建立的降水-能见度理论模型。结果表明:能见度随着降水强度的增大呈指数降低;受降水粒子特性和天气条件等多种因素影响,能见度与降水强度之间的关系并不是唯一对应的;降雨和降雪对能见度的影响各不相同,相比而言,降雨对能见度的影响比较容易确定,而降雪对能见度的影响比较复杂,主要因为雪花或冰晶的类型复杂多变,对大气消光系数有不同程度的影响。结合理论分析和实测数据对比验证,降水现象对能见度的影响得到了证实。     

大气气溶胶光学厚度的宽带消光遥感方法及其应用

该文发展了遥感气溶胶光学厚度的一个宽带消光遥感方法 ,它应用地面上太阳直射表探测的宽波段太阳直射信息反演 0 75 μm大气柱光学厚度。这方法的主要误差因子是气溶胶谱的不确定性。数值试验表明 ,气溶胶谱分布的误差所引起光学厚度解的误差一般小于 5 %。 1995年 1— 10月进行的 12 6 7组对比实验表明 ,由本方法探测的气溶胶光学厚度与光度计探测的气溶胶光学厚度的标准差为 10 5 % ,两者平均结果的偏差只有 0 7%。该文还应用这个方法 ,从气象台站辐射观测资料反演得到北京、沈阳等 10个地方 1980— 1994年间晴天气溶胶光学厚度资料 ,并分析其变化规律     

古—中生代之交的全球变化与生物效应

古—中生代之交是显生宙以来最大的一次生物绝灭期 ,其形成机制一直是地学界长期探讨的热点课题之一。地史重大转折期是地球内、外各圈层长期作用下 ,各种量变达到阀值 ,加之可能的外因激化 ,在短时间内以连锁反应形式相继质变 ,形成了全球变化 (包括生物绝灭 )的地球突变期。文中从可能的外因 (外星体撞击事件 )及内因 (岩石圈的变化 ,地球表层的变化和生物圈的变化 )两个方面探讨了古—中生代之交的全球变化与生物效应     

Towards a free–free template for CMB foregrounds

A full-sky template map of the Galactic free–free foreground emission component is increasingly important for high-sensitivity cosmic microwave background (CMB) experiments. We use the recently published Hα data of both the northern and southern skies as the basis for such a template.
The first step is to correct the Hα maps for dust absorption using the 100-μm dust maps of Schlegel, Finkbeiner & Davis. We show that for a range of longitudes, the Galactic latitude distribution of absorption suggests that it is 33 per cent of the full extragalactic absorption. A reliable absorption-corrected Hα map can be produced for ∼95 per cent of the sky; the area for which a template cannot be recovered is the Galactic plane area  | b | < 5°, l = 260°–0°–160°  and some isolated dense dust clouds at intermediate latitudes.
The second step is to convert the dust-corrected Hα data into a predicted radio surface brightness. The free–free emission formula is revised to give an accurate expression (1 per cent) for the radio emission covering the frequency range 100 MHz–100 GHz and the electron temperature range 3000–20 000 K. The main uncertainty when applying this expression is the variation of electron temperature across the sky. The emission formula is verified in several extended H  ii regions using data in the range 408–2326 MHz.
A full-sky free–free template map is presented at 30 GHz; the scaling to other frequencies is given. The Haslam et al. all-sky 408-MHz map of the sky can be corrected for this free–free component, which amounts to a  ≈6  per cent correction at intermediate and high latitudes, to provide a pure synchrotron all-sky template. The implications for CMB experiments are discussed.