东秦岭陕西聂家沟剖面二叠纪—三叠纪之交沉积特征及其古环境意义*

东秦岭陕西镇安聂家沟地区二叠纪—三叠纪之交发育一套海相碳酸盐岩沉积序列,较完整地记录了二叠纪末生物大灭绝事件前后浅海碳酸盐岩台地相生物群落演替及环境变化等信息,是研究二叠纪末生物大灭绝事件前后生态环境变化与沉积响应的理想区域。通过碳酸盐岩微相分析方法,对陕西镇安聂家沟剖面二叠系—三叠系界线附近的碳酸盐岩生物组合和微相类型进行了详细分析,共识别出11个微相类型: 斑点状凝块石、叠层石灰岩、鲕粒—纹层状叠层石灰岩、有孔虫颗粒灰岩、藻—海百合泥粒灰岩、含有被包壳和被磨蚀骨屑颗粒的粒泥灰岩、鲕粒颗粒灰岩、集合颗粒灰岩、含鲕粒的粒泥灰岩、泥晶灰岩和泥岩。根据碳酸盐岩微相特征及沉积相标志,在二叠系—三叠系界限附近划分出台地边缘、开阔台地和局限台地3种沉积相,其反映了二叠纪—三叠纪之交频繁的沉积相带变更的特点。该剖面碳酸盐岩微相反映的古生态和生物群落演替特征与中国华南同时期其他剖面具有较好的一致性,即二叠纪末生物大灭绝事件之后,早三叠世正常浅水碳酸盐岩台地生物类型和丰度极低,仅含有少量的双壳类、海百合等,灭绝事件界线附近以微生物碳酸盐岩等特殊微生物沉积构造占主导,之后微生物岩等消失,又出现了以双壳类为首的生物碎屑石灰岩。研究结果为了解二叠纪末生物大灭绝事件中生物和环境的协同演化提供了新的材料和认识。     

三叠纪末期全球生物大灭绝事件研究综述

三叠纪末期生物大灭绝是全球地质历史时期五大生物灭绝事件之一,它致使海洋生态系统中约53%的属和80%的种灭绝。显著灭绝的生物包括菊石类、牙形类、放射虫类和陆地四足动物,发生部分灭绝的生物包括腕足类、介形类、双壳类和珊瑚类等。中大西洋火成岩省（CAMP）的爆发与三叠纪末期生物大灭绝在时间上具有较高的一致性,其火山的高强度和大面积喷发被认为是导致此次灭绝事件发生的主要原因。CAMP爆发释放出大量的CO2、SO2和CH4等气体,一方面温室效应促使海平面升高,物种栖息地面积减少、海洋酸化和海洋缺氧等事件直接威胁着海洋和陆地生物的生存环境;另一方面温室效应亦会引发全球性森林火灾,造成陆地植物减少,大量植物碳屑注入海洋使其发生富营养化,又因伴随海洋酸化作用（碳酸化和硫酸化）,海洋古生产率发生崩溃。不同地质时期生物大灭绝的发生往往伴随着剧烈的环境变化,在三叠纪末生物大灭绝期,这些变化多表现为古大气成分和古气温动荡、古火灾频繁、海洋酸化、海平面升高和海水缺氧等,它们之间的综合作用最终导致三叠纪末期全球生态系统失稳。在全球多个三叠纪—侏罗纪之交（TJB）剖面均可以识别出3次明显的碳同位素负偏移,最显著的1次发生于瑞替期末,早于TJB。上述情况说明,三叠纪末期生物大灭绝虽然是全球性事件,但并不是1次发生的,具有分阶段性、非同步性、区域性和有选择性等特点。     

三叠纪末期全球生物大灭绝事件研究综述

三叠纪末期生物大灭绝是全球地质历史时期5大生物灭绝事件之一,它致使海洋生态系统中约53%的属和80%的种灭绝。显著灭绝的生物包括菊石亚纲、牙形类、放射虫目和陆地四足动物,发生部分灭绝的生物包括腕足动物门、介形亚纲、双壳纲和珊瑚纲等。中大西洋火成岩省(CAMP)的爆发与三叠纪末期生物大灭绝在时间上具有较高的一致性,其火山的高强度和大面积喷发被认为是导致此次灭绝事件发生的主要原因。CAMP爆发释放出大量的CO₂、SO₂和CH₄等气体,一方面温室效应促使海平面升高,物种栖息地面积减少、海洋酸化和海洋缺氧等事件直接威胁着海洋和陆地生物的生存环境;另一方面温室效应亦会引发全球性森林火灾,造成陆地植物减少,大量植物碳屑注入海洋使其发生富营养化,又因伴随海洋酸化作用(碳酸化和硫酸化),海洋古生产率发生崩溃。不同地质时期生物大灭绝的发生往往伴随着剧烈的环境变化,在三叠纪末生物大灭绝期,这些变化多表现为古大气成分和古气温动荡、古火灾频繁、海洋酸化、海平面升高和海水缺氧等,它们之间的综合作用最终导致三叠纪末期全球生态系统失稳。在全球多个三叠...     

Biodiversity changes of the Ordovician trilobites in the middle Yangtze region of South China

The biodiversity changes of trilobites in the middle Yangtze region of South China in the Great Ordovician Biodiversification Event and the end-Ordovician mass extinction have been analysed. The Ordovician trilobites in this region originated in the early Tremadocian and radiated from the late Floian to the early Katian. Two peaks of diversity appeared in the late Dapingian to the early Darriwilian and the early Katian. The extinction occurred in the late Katian, followed by a survival period in the Hirnantian. The Whiterock fauna began to surpass the Ibex fauna during the early Katian and were dominant by the late Katian to the Hirnantian, indicating that Cambrian Evolutionary Fauna was gradually replaced. The study once again confirms the view that the effects of factors such as sea level, climate, oxygen content, nutrient supply, and tectogenesis differ temporally and to different degrees in different regions, resulting in differences in the vertical sequence and horizontal combination of ecosystems, which is the reason for the different evolution patterns of Ordovician trilobites in different regions.     

平面光极的制备及水母消亡对沉积物-海水界面溶解氧影响的模拟观测

制备了基于八乙基卟啉铂和香豆素的光强比率测量传感膜,结合3CCD相机构建了基于比率测量法的两维溶解氧观测系统,通过实验验证了该系统在沉积物-水界面微结构的溶解氧的时空动态变化监测的可行性。基于实验室模拟观测装置对海蜇消亡过程中沉积物-海水溶解氧的变化特征进行了观测。观测结果表明在置入水母组织的第16h后,水母分解使得沉积物-水界面的溶解氧开始下降,在2~3d内会导致沉积物-水界面空间的海水溶解氧发生剧烈变化,在沉积物-海水界面附近海水形成严重缺氧区。第1天内,沉积物-海水界面的溶解氧消耗速率为0.2mg·L-1·h-1,第2天溶解氧的消耗速率为0.04mg·L-1·h-1。在近海底的水体空间内,第1天的溶解氧消耗速率为0.28mg·L-1·h-1,第2天为0.14mg·L-1·h-1,第3天为0.13mg·L-1·h-1,表明水母消亡过程中的溶解氧消耗呈动态分布。实验证明水母在消亡过程中的3~4d内可在沉积物-海水界面附近形成一个贫氧区,水母消亡过程改变了海底区域的溶解氧分布体系,将对海底生态环境产生较大影响。     

High spatial resolution Galactic 3D extinction mapping with IPHAS

We present an algorithm (MEAD, for 'Mapping Extinction Against Distance') which will determine intrinsic  ( r '− i ')  colour, extinction, and distance for early-A to K4 stars extracted from the IPHAS   r '/ i '/Hα  photometric data base. These data can be binned up to map extinction in three dimensions across the northern Galactic plane. The large size of the IPHAS data base (∼200 million unique objects), the accuracy of the digital photometry it contains and its faint limiting magnitude  ( r '∼ 20)  allow extinction to be mapped with fine angular (∼10 arcmin) and distance (∼ 0.1 kpc) resolution to distances of up to 10 kpc, outside the solar circle. High reddening within the solar circle on occasion brings this range down to ∼2 kpc. The resolution achieved, both in angle and depth, greatly exceeds that of previous empirical 3D extinction maps, enabling the structure of the Galactic Plane to be studied in increased detail. MEAD accounts for the effect of the survey magnitude limits, photometric errors, unresolved interstellar medium (ISM) substructure and binarity. The impact of metallicity variations, within the range typical of the Galactic disc is small. The accuracy and reliability of MEAD are tested through the use of simulated photometry created with Monte Carlo sampling techniques. The success of this algorithm is demonstrated on a selection of fields and the results are compared to the literature.     

Effects of scattering and dust grain size on the temperature structure of protoplanetary discs: a three-layer approach

The temperature in the optically thick interior of protoplanetary discs is essential for the interpretation of millimetre observations of the discs, for the vertical structure of the discs, for models of the disc evolution and the planet formation, and for the chemistry in the discs. Since large icy grains have a large albedo even in the infrared, the effect of scattering of the diffuse radiation in the discs on the interior temperature should be examined. We have performed a series of numerical radiation transfer simulations, including isotropic scattering by grains with various typical sizes for the diffuse radiation as well as for the incident stellar radiation. We also have developed an analytic model including isotropic scattering to understand the physics concealed in the numerical results. With the analytic model, we have shown that the standard two-layer approach is valid only for grey opacity (i.e. grain size ≳10 μm) even without scattering. A three-layer interpretation is required for grain size ≲10 μm. When the grain size is 0.1–10 μm, the numerical simulations show that the isotropic scattering reduces the temperature of the disc interior. This reduction is nicely explained by the analytic three-layer model as a result of the energy loss by scatterings of the incident stellar radiation and of the warm diffuse radiation in the disc atmosphere. For grain size ≳10 μm (i.e. grey scattering), the numerical simulations show that the isotropic scattering does not affect the interior temperature. This is nicely explained by the analytic two-layer model; the energy loss by scattering in the disc atmosphere is exactly offset by the 'green-house effect' due to the scattering of the cold diffuse radiation in the interior.     

Joint formation of QSOs and spheroids: QSOs as clocks of star formation in spheroids

Direct and indirect observational evidence leads to the conclusion that high-redshift QSOs did shine in the core of early-type protogalaxies during their main episode of star formation. Exploiting this fact, we derive the rate of formation of this kind of stellar system at high redshift by using the QSO luminosity function. The elemental proportions in elliptical galaxies, the descendants of the QSO hosts, suggest that the star formation was more rapid in more massive objects. We show that this is expected to occur in dark matter haloes, when the processes of cooling and heating are considered. This is also confirmed by comparing the observed submm counts with those derived by coupling the formation rate and the star formation rate of the spheroidal galaxies with a detailed model for their SED evolution. In this scenario SCUBA galaxies and Lyman-break galaxies are early-type protogalaxies forming the bulk of their stars before the onset of QSO activity.     

Dust attenuation in starburst galaxies determined by measuring the dependence of the optical color indices on galaxy inclination

We use optical color indices (colors) from the SDSS database to study the effect of dust in starburst galaxies by mea‐suring the dependence of colors on galaxy inclination. Starburst galaxies with ongoing star formation, are rich with metals/dust and are, therefore, an excellent objects for studying the effect of dust in galaxies. They are selected using the [O III ]λ 5007/Hα vs. [N II ]λ 6584/Hβ diagram, that is, the BPT‐diagram. We use Kauffmann's empirical demarcation line in the BPT‐diagram to exclude galaxies with active galactic nuclei (AGN) from the sample because they have different physical and dust properties from normal galaxies. The sample is divided into bins according to galaxy stellar mass and 4000 Å break (which is a coarse measure of a galaxy star formation history; SFH) and the reddening with inclination is studied as a function of these two physical parameters. Assuming that the dust effect is negligible in the SDSS z ‐band, we derive the attenuation curves for these galaxies. We fit the attenuation curves with a simple power law and use power law index to interpret the relative distribution of dust and stars in the starburst galaxies (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)