水华生消过程中巢湖水体和沉积物理化性质变化特征

湖泊水华存在复杂的生消过程,然而目前较多研究聚焦在水华持续阶段对湖泊生态系统的影响,却较少关注水华生消过程对湖泊水体和沉积物理化性质的影响.以巢湖为对象,根据历史资料确定水华区和非水华区,在相同位点分别于水华形成前期、形成期、持续期和消亡期采集水体和沉积物样品,分析水华生消过程对湖泊水体和沉积物理化指标及营养盐的影响.结果表明,巢湖研究区域水华形成期为5月中旬至6月中旬,持续期为6月中旬至9月上旬,之后进入水华消亡期.水体透明度、p H值和溶解氧在水华区与非水华区大部分时间存在显著差异,且随水华生消过程呈现不同的变化趋势,但水温、氧化还原电位和电导率在水华区和非水华区无显著差异,并随水华生消过程呈现相同的变化趋势.非水华区水体和沉积物中各形态氮、磷浓度明显低于水华区,且随时间变化幅度相对较小.在水华区,水体氮、磷浓度(总溶解性氮、硝态氮、氨氮、总氮、总溶解性磷、磷酸盐)在水华形成期和水华持续前期呈下降趋势,但在水华持续后期和水华消亡期呈增加趋势;沉积物氮、磷浓度(总氮、总磷)和总有机质含量显著高于非水华区,三者在水华区和非水华区随水华生消过程呈现不同的变化趋势.研究表明,水华生消过程对湖泊营养盐和水体及沉积物性质有不同的影响,这对湖泊富营养化治理和水华防治具有重要意义.     

物种特征在生物绝灭事件中的作用

本文从居群生态学的角度出发,结合生物演化的更替速率、成种速率及灭绝速率讨论了物种的生物学特征在生物绝灭事件中的可能影响。监管蜓类、菊石、珊瑚及腕足动物的资料表明,生物的“抗灾变能力和生物的地理分布范围成正比,和生物的演化速率成反比。同时,生物在绝灭事件中的命运也和它们当时所处的演化阶段有密切的关系。     

Formation of the salinity minimum in the Mixed Water Region between the Oyashio and Kuroshio Fronts

The salinity minimum frequently occurring in the Mixed Water Region between the Oyashio and Kuroshio Fronts seems to originate from the salinity minimum at the density of 26.8σ_θ called the North Pacific Intermediate Water. We examined water exchange of this region with the Oyashio and the Kuroshio Extension using mixing ratio R_K defined as (θ - θ_OY)/(θ_K - θ_OY) × 100, where θ_OY, θ_K, and θ represent potential temperature of the Oyashio and Kuroshio Waters and their mixture on the isopycnal surfaces, respectively. CTD data were obtained by repeated observation from January 1990 to May 1991. R_K increases southward from the Oyashio Front to the Kuroshio Front with the range of −20 to 120%. The gradient of R_K on the isopycnal surfaces is large around the Oyashio Front above the 26.8σ_θ surface, while it is large around the Kuroshio Front below it. This agrees with the average R_K in the Mixed Water Region decreasing greatly with the increase of density at densities less dense than 26.8σ_θ. We calculated thickness and volume transport of the Oyashio between the isopycnal surfaces near the coast of Hokkaido. They increase largely with density at densities less dense than 26.8σ_θ. It is supposed that the salinity minimum in the Mixed Water Region is the upper limit of the water largely influenced by the Oyashio Water. Its density could depend only on the density structure of the Oyashio.     

类星体SDSS J0916+2921的类银河系2175 ?尘埃消光特征

光谱观测显示类星体SDSS J091613.60+292106.1 (简称J0916+2921,系统红移zem=1.1418±0.0018)中有特殊的2175?尘埃消光特征,其强度显著大于银河系平均强度.光谱同时探测到与尘埃成协的丰富气体吸收线,确定吸收线系统红移为zabs=1.1413±0.0002,和类星体红移一致.气态金属离子柱密度相对太阳丰度的比例为[Al/Zn]=-1.68±0.10,[Cr/Zn]=-0.49±0.10,[Fe/Zn]=-0.81±0.18.尘埃耗散作用显著,说明该系统中尘埃十分丰富,与观测的强尘埃消光特征吻合.类银河系的2175?尘埃消光特征在类星体光谱中多见于中间插入吸收线系统,至今未明确认证内禀吸收线系统出现该特征,类星体SDSS J0916+2921是目前仅有的数个候选者之一.该类星体X射线辐射相较一般类星体更强,后续可用作研究2175?尘埃在强高能射线照射条件下的形成与离解平衡,以揭示2175?尘埃的化学成分、物理性质和起源.     

生态因子在黄海绿潮生消过程中的作用

2008–2017年南黄海海域连续10 a发生绿潮,影响周边沿海城市养殖、旅游和航运安全等。研究绿潮生消过程及其影响因素对于理解黄海绿潮分布特征,开展绿潮灾害的预防与治理有重要意义。本文主要采用MODIS L1B数据,通过归一化植被指数提取绿潮信息。根据逐年绿潮覆盖面积的变化特征,将绿潮生消过程分为3个阶段:触发阶段、快速发展阶段、消衰阶段,分析了海表温度、降水和光照在绿潮生消过程中的作用。结果表明:在触发阶段,温度达到15°C后,有效降水可以刺激绿潮的触发,在降水后的半个月内可以通过MODIS影像发现绿潮。在快速发展阶段,绿潮所在位置海表面温度为16～21°C,适宜绿潮的快速生长;太阳短波辐射集中在250～280 W/m2范围内;降水量是影响绿潮生长规模的一个重要因素,降水量少时绿潮覆盖面积峰值明显较小,而出现绿潮覆盖面积最大值的2016年降水量也极高。在消衰阶段,海表温度上升至22～26°C,绿潮在卫星影像中消失时,平均海表温度超过26°C,最高温度可达27.48°C,较高的海表面温度是导致绿潮消亡的主要原因之一;太阳短波辐射集中在240～260 W/m2,略低于快速发展阶段光照范围;降水量在该阶段相对充足不再影响绿潮的生长。     

Intensifying aeolian activity following the end-Permian mass extinction: Evidence from the Late Permian–Early Triassic terrestrial sedimentary record of the Ordos Basin,North China

Sedimentary successions provide direct evidence of climate and tectonics, and these give clues about the causes of the mass extinction around the Permian–Triassic boundary. Terrestrial Permian–Triassic boundary strata in the eastern Ordos Basin, North China, include the Late Permian Sunjiagou, Early Triassic Liujiagou and late Early Triassic Heshanggou formations in ascending order. The Sunjiagou Formation comprises cross-bedded sandstones overlaid by mudstones, indicating meandering rivers with channel, point bar and floodplain deposits. The Liujiagou Formation was formed in braided rivers of arid sand bars interacting with some aeolian dune deposits, distinguished by abundant sandstones where diverse trough and planar cross-bedding and aeolian structures (for example, inverse climbing-ripple, translatent-ripple lamination, grainfall and grainflow laminations) interchange vertically and laterally. The Heshanggou Formation is a rhythmic succession of mudstones interbedded with thin medium-grained sandstones mainly deposited in a shallow lacustrine environment. Overall, the sharp meandering to braided to shallow lake sedimentary transition documents palaeoenvironmental changes from semi-arid to arid and then to semi-humid conditions across the Permian–Triassic boundary. The die-off of tetrapods and plants, decreased bioturbation levels in the uppermost Sunjiagou Formation, and the bloom of microbially-induced sedimentary structures in the Liujiagou Formation marks the mass extinction around the Permian–Triassic boundary. The disappearance of microbially-induced sedimentary structures, increasingly intense bioturbation from bottom to top and the reoccurrence of reptile footprints in the Heshanggou Formation reveal gradual recovery of the ecosystem after the Permian–Triassic boundary extinction. This study is the first to identify the intensification of aeolian activity following the end-Permian mass extinction in North China. Moreover, while northern North China continued to be uplifted tectonically from the Late Palaeozoic to Late Mesozoic, the switch of sedimentary patterns across the Permian–Triassic boundary in Shanxi is largely linked to the development of an arid and subsequently semi-humid climate condition, which probably directly affected the collapse and delayed recovery in palaeoecosystems.     

病毒与细菌等微生物在地球生物演化史上的作用

病毒与细菌统称为微生物。病毒与细菌之害是生物生存遭遇到的最大的灾害,不仅在人类社会历史上留下了深重灾难,而且在地球生物演化史上也是大灭绝的重要推手。虽然病毒和细菌难以形成实体化石,但却以一种特殊的分子化石成为了侦探地质时期生物大灭绝的神针。本文以地球微生物学为指导,以蓝细菌和绿硫细菌分子化石为例,综合有关研究成果,解读了微生物学、病毒和细菌以及微生物岩的有关知识,帮助人们认识地球生物演化史上二次重要的大灭绝事件。本文还从人类演化过程中的农业革命,阐明了人菌共生关系及带来的启示。     

Photometric survey near the main Galactic meridian: 2.2. Finding charts and photoelectric UBVR stellar magnitudes in 26 fields

Finding charts and photoelectric magnitudes of stars in the UBVR system in 26 fields of the MEGA programme are presented. This part of the photometric survey near the Main Galactic Meridian includes the fields with right ascentions 8^h < α < 16^h30^m and declinations −2° < δ < 58°. Together with the finding charts of 2.5° × 2.5° the equatorial coordinates of the stars are given for epoch and equinox 1950. Photometric properties of the night sky at the Mount Terskol observatory near Mount Elbrus are derived from the photoelectric observations.     

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)