贵州紫云剖面P/T界面附近碳氧同位素的变化及生物绝灭事件

:贵州南部紫云剖面由上二叠统长兴组的碳酸盐台地边缘沉积体系、下三叠统罗楼组的碳酸盐浅海陆棚沉积体系、以及下三叠统紫云组的半深海深海沉积体系组成。在前两种沉积体系中选取 18块样品进行碳、氧同位素测试。测试的结果表明 :上二叠统长兴组δ13 C平均值为 2 4 8‰ ,保持了较高的正值 ,δ18O平均值为 - 4 19‰ ;在P/T界面附近 ,δ13 C ,δ18O值都有显著的降低 ,δ13 C值由 2 71‰陡降至 - 0 90‰ ,变化幅度达 3 6 1‰ ,δ18O值由 - 5 0 3‰降为- 9 4 6‰ ,变化幅度可达 4 4 3‰ ;下三叠统罗楼组下部 ,δ13 C值为负值及低正值 ,出现明显的δ13 C值低异常 ,而δ18O值则比较稳定 ,介于 - 4 6 6‰和 - 5 6 2‰之间 ,平均值为 - 5 2 8‰。罗楼组上部 ,δ13 C值有回升的趋势。由于生物对轻碳具有重要的分馏作用 ,因此 ,P/T界面附近δ13 C值的显著变化反映了一次生物大量绝灭的过程。由δ18O值的变化反映出的生物绝灭的外因主要有温度和盐度两方面。从δ18O值可计算出在P/T界面处古温度有 4～ 5℃的升降 ,这势必影响到狭温生物的生存 ;从δ18O值计算出的Z值来看 ,古盐度也有小幅度的变化 ,加速了狭盐度生物的绝灭。事实上 ,生物的绝灭可能是海平面变化、火山事件、温度变化及盐度变化多种因素的综合     

干旱与灌溉处理对冬小麦冠层内光分布的影响

为探讨北方冬麦区节水灌溉的关键时期,借助干旱和灌溉对冬小麦冠层光分布,获取本地化参数,为华北农业干旱预报模型的修正提供依据。采用美国CID公司生产的CI-110型植物冠层分析仪,对干旱和灌溉条件下冬小麦冠层内光分布进行直接测定。结果表明,干旱和灌溉条件下,无论是高氮还是低氮、中氮,平均叶面倾角(MLA)都随生育期的延长呈现出先下降再上升的趋势。高氮和低氮时,随着生育期的延长,干旱处理和灌溉处理的冬小麦散射辐射透过系数(TCDP)都呈现先下降再上升的变化趋势;中氮时,干旱处理和灌溉处理的冬小麦TCDP在开花期和灌浆期都呈现一直上升的趋势。无论高氮还是中氮、低氮,冬小麦直接辐射透过系数(TCRP)的值都随着天顶角角度的增大而减小,冬小麦TCRP的值随着冬小麦生育期的推进,都呈现出先下降、后上升的变化趋势。高、中、低氮3种情况下,干旱和灌溉处理的冬小麦每个生育期均呈现随着天顶角角度的增加,消光系数K也增大;高氮时,多数情况下,冬小麦冠层的消光系数K干旱的大于灌溉的;中氮、低氮时,多数情况下,冬小麦冠层的消光系数K干旱的小于灌溉的。干旱和灌溉对冬小麦冠层光分布的影响:灌溉增加了冬小麦的平均叶面倾角(MLA);干旱和灌溉处理条件下冬小麦的TCDP差异较小,TCDP与MLA变化趋势相似,也都呈现出先下降、再上升的变化规律;干旱和灌溉处理冬小麦TCRP,无论高氮还是中氮、低氮,都随着天顶角角度的增大而减小,在7.5°、22.5°时干旱和灌溉对冬小麦TCRP的影响较大,而在37.5°、52.5°、67.5°时对冬小麦TCRP的值影响很小;每个生育期消光系数K均随着天顶角角度的增加而增大。     

The poor cluster of galaxies S639

We have studied the poor southern cluster of galaxies S639. Based on new Strömgren photometry of stars in the direction of the cluster, we confirm that the Galactic extinction affecting the cluster is large. We find the extinction in Johnson B to be A_B =0.75±0.03. We have obtained new photometry in Gunn r for E and S0 galaxies in the cluster. If the Fundamental Plane is used for determination of the relative distance and the peculiar velocity of the cluster, we find a distance, in velocity units, of (5706±350) km s⁻¹, and a substantial peculiar velocity, (839±350) km s⁻¹. However, the colours and the absorption line indices of the E and S0 galaxies indicate that the stellar populations in these galaxies are different from those in similar galaxies in the two rich clusters Coma and Hydra I. This difference may severely affect the distance determination and the derived peculiar velocity. The data are consistent with a non-significant peculiar velocity for S639 and the galaxies in the cluster being on average 0.2 dex younger than similar galaxies in Coma and Hydra I. The results for S639 caution that some large peculiar velocities may be spurious and caused by unusual stellar populations.     

A SCUBA survey of L1689 – the dog that didn't bark

We present submillimetre data for the L1689 cloud in the ρ Ophiuchi molecular cloud complex. We detect a number of starless and pre-stellar cores and protostellar envelopes. We also detect a number of filaments for the first time in the submillimetre continuum that are parallel both to each other, and to filaments observed in the neighbouring L1688 cloud. These filaments are also seen in the ¹³CO observations of L1689. The filaments contain all of the star-formation activity in the cloud. L1689 lies next to the well-studied L1688 cloud that contains the ρ Oph-A core. L1688 has a much more active star-formation history than L1689 despite their apparent similarity in ¹³CO data. Hence, we label L1689 as the dog that didn't bark. We endeavour to explain this apparent anomaly by comparing the total mass of each cloud that is currently in the form of dense material such as pre-stellar cores. We note firstly that L1688 is more massive than L1689, but we also find that when normalized to the total mass of each cloud, the L1689 cloud has a much lower percentage of mass in dense cores than L1688. We attribute this to the hypothesis of Loren that the star formation in the ρ Ophiuchi complex is being affected and probably dominated by the external influence of the nearby Upper Scorpius OB association and predominantly by σ Sco. L1689 is further from σ Sco and is therefore less active. The influence of σ Sco appears none the less to have created the filaments that we observe in L1689.     

Endolithic fungi: A possible killer for the mass extinction of Cretaceous dinosaurs

Mycelium-like structures found under ESEM within radial sections of fragmental dinosaur eggshells would be the endolithic fungi coexistent with dinosaur eggs in the upper part of the Late Cretaceous Hugang Formation from the Wenjiaping section of Wenxian, Danjiangkou, northwestern Hubei, Central China. The endolithic fungi selectively occurred in the bad biomineral zone within the columnar layer of the eggshells, where the crowded endolithic fungi penetrated the columnar layer at near-vertical or near-horizontal angles. The endolithic fungi are needle-like, ribbon-like and silk-like, and 5-18 μm long, 0.3-0.5 μm wide at their base, with pointed tip, and are unbranched. The hyphae are mainly composed of oxygen, carbon and calcium, and are with minor sodium, potassium, chlorine and sulfur. The en-dolithic fungi and host have the same characters in lithification, fracture and main chemical composi-tion. We suggested that the episode endolithic fungi invading dinosaur eggs may have taken place in the interval between after formation of dinosaur eggshells and before their petrifaction and that dino-saur eggs invaded by endolithic fungi would not be normally incubated or would only be incubated into venerable and pathologic baby dinosaurs to be easily to aborted and contributed to the mass extinction of the dinosaurs at the end of Cretaceous.     

Optical emission at 5800 Å in the Red Rectangle and the 5797-Å diffuse interstellar band

An analysis of the intensity and spatial distribution of the discrete 5800-Å emission band in the spectrum of the Red Rectangle has been used to constrain the abundance and physical properties of the carrier of this emission. An origin in a large (>30 C atom) molecule is indicated. This molecule is formed in situ in the Red Rectangle, but is also a component of the diffuse interstellar medium. The UV photodissociation probability for this molecule is ≲10⁻⁵ per absorbed photon, and the luminescence efficiency is in the range 10⁻²–10⁻³. This molecule may be a product of the dissociation of carbonaceous dust.     

Late Olenekian Radiolarians from Bedded Chert of Ashio Terrane, Northeast Japan,and Faunal Turnovers in Western Panthalassa during Early Triassic

Late Olenekian assemblages in the western Panthalassa have been recovered from bedded radiolarian chert sequences of an accretionary complex, the Ashio belt. These faunas are documented and considered in terms of radiolarian diversity and faunal turnover during the latest Permian to Middle Triassic time. The fauna includes 30 radiolarians belonging to Spumellaria or Entactinaria, with two relicts from the Late Permian. This late Olenekian fauna is markedly different from Permian and Asisian faunas, respectively, and is herein named the Minowa fauna. Study of the literaure indicates that radiolarian provinces were significantly disconnected between the western Panthalassa and eastern Tethys during late Olenekian time. Furthermore, 121 of 143 species disappeared during late Olenekian time, and in turn 118 new species appeared in the western Panthalassa around the Olenekian-Anisian boundary. It is concluded that faunal turnover occurred at least three times between the latest Permian and Middle Triassic.The first turnover is the Poalaozoie-type radiolarian extinction at the Permain-Triassic boundary,the second is the diversification of spheroidal Spumellaria and Entactinaria between early and late Olenekian time, and the third is a faunal turnover from the Minowa fauna to the true Mesozoic-type radiolarian famas that are characterized by mulit0segmented Nassellaria.     

Devonian Frasnian-Famennian transitional event deposits of Guangxi, South China and their possible tsunami origin

A suite of event deposits, isochronous and interrelated in origin, occurs widely near the Frasnian- Famennian boundary in Guangxi, South China. It is mainly distributed in the facies areas of the platform-margin slope and inter-platform rift-trough. The rudstone or calcirudite occur in the Liujing section of Hengxian and Luoxiu and Baqi sections of Xiangzhou in the facies area of platform-margin slope. The turbidites are observed in the sections of Yangdi and Baisha of Guilin, Du'an of Debao, Nandong and Sanli of Wuxuan, Xiangtian, Ma'anshan of Xiangzhou, Nayi of Chongzuo, Yunpan of Shanglin in the facies area of inter-platform rift-trough. The massive homogenites occur in sections of Mangchang, Luofu and Road from Nandan to Tian'e and Ma'anshan etc in the facies area of inter-platform rift-trough. Herein event deposits can be correlated in stratohorizon to the turbidite in the bottom of the Lower triangularis Zone in Hony railroad cut of Belgium, Devils Gate of Nevada, USA, Atrous of Morocco, South Urals and Fore-Kolyma of northeastern Siberia of Russia, and erosional discontinuities and brecciation in the Frasnian-Famennian boundary in South Polish-Moravian shelf. The event deposits could be caused by a violent tsunami related to bolide impacts into ocean.     

年轻星体(YSO)红外氢谱线流量特征及其应用

在年轻星体星周致密HII区非局部热动平衡模型基础上，本文主要计算了年轻星体红外氢谱线流量及流量比．计算发现在Pfγ／Brα与Brγ／Brα之间，Pa7／Brα与Brγ／Brα之间有很好的线性相关性，这一关系与星周物理参数基本无关．利用这一理论关系可以估计YSOs的前景消光．另外，我们认为只要合理地选择中央星及星风的物理参数，例如质量损失率及星风速度等，年轻恒星的谱线过量问题就可以得到合理的解释．文中给出了部分红外源的分析结果．     

The far-infrared–submillimetre spectral energy distribution of high-redshift quasars

We combine photometric observations of high-redshift     quasars, obtained at submillimetre to millimetre wavelengths, to obtain a mean far-infrared (rest-frame) spectral energy distribution (SED) of the thermal emission from dust, parametrized by a single temperature ( T ) and power-law emissivity index ( β ). The best-fitting values are     and     . Our method exploits the redshift spread of this set of quasars, which allows us to sample the SED at a larger number of rest wavelengths than is possible for a single object: the wavelength range extends down to ∼60 μm, and therefore samples the turnover in the greybody curve for these temperatures. This parametrization is of use to any studies that extrapolate from a flux at a single wavelength, for example to infer dust masses and far-infrared luminosities.
We interpret the cool, submillimetre component as arising from dust heated by star formation in the host galaxy of the quasar, although we do not exclude the presence of dust heated directly by the active galactic nucleus (AGN). Applying the mean SED to the data, we derive consistent star formation rates ∼1000 M_⊙ yr⁻¹ and dust masses ∼10⁹ M_⊙, and investigate a simple scheme of AGN and host galaxy co-evolution to account for these quantities. The time-scale for formation of the host galaxy is     , and the luminous quasar phase occurs towards the end of this period, just before the reservoir of cold gas is depleted. Given the youth of the Universe at     (1.6 Gyr), the coexistence of a massive black hole and a luminous starburst at high redshifts is a powerful constraint on models of quasar host galaxy formation.