TiO2/浮石复合材料降解有机污染物亚甲基蓝的实验研究

利用天然浮石的孔隙结构和小比重等特点,以浮石为原料、TiOSO4为TiO2前驱体,采用水热合成法,在200℃、15 h条件下,制备出可漂浮的TiO2/浮石复合材料.采用10×10-5mol/L亚甲基蓝水溶液,在紫外光下进行光催化实验.并用紫外可见分光光度计检测亚甲基蓝浓度变化.实验结果表明,TiO2/浮石复合材料能够降解亚甲基蓝.该材料的孔隙结构对亚甲基蓝有聚集作用,促进了负载的TiO2的光催化性能的发挥.因为成本低廉,性能优越,TiO2/浮石复合材料在有机污染物治理方面具有很大的应用潜力.     

Double funnelling in a mature coastal British Columbia forest: spatial patterns of stemflow after infiltration

Many studies have focused on the amount of stemflow in different forests and for different rainfall events, but few studies have focused on how stemflow intensity varies during events or the infiltration of stemflow into the soil. Stemflow may lead to higher water delivery rates at the base of the tree compared with throughfall over the same area and fast and deeper infiltration of this water along roots and other preferential flow pathways. In this study, stemflow amounts and intensities were measured and blue dye experiments were conducted in a mature coniferous forest in coastal British Columbia to examine double funnelling of stemflow. Stemflow accounted for only 1% of precipitation and increased linearly with event total precipitation. Funnelling ratios ranged from less than 1 to almost 20; smaller trees had larger funnelling ratios. Stemflow intensity generally was highest for periods with high‐intensity rainfall later in the event. The maximum stemflow intensities were higher than the maximum precipitation intensities. Dye tracer experiments showed that stemflow infiltrated primarily along roots and was found more frequently at depth than near the soil surface. Lateral flow of stemflow was observed above a dense clay layer for both the throughfall and stemflow experiments. Stemflow appeared to infiltrate deeper (122 cm) than throughfall (85 cm), but this difference was in part a result of site‐specific differences in maximum soil depth. However, the observed high stemflow intensities combined with preferential flow of stemflow may lead to enhanced subsurface stormflow. This suggests that even though stemflow is only a very minor component of the water balance, it may still significantly affect soil moisture, recharge, and runoff generation. Copyright © 2016 John Wiley & Sons, Ltd.     

基于水文模型的乌裕尔河流域水资源评价

基于水文模型的流域水资源评价可以为解决流域水资源短缺问题和改善水资源管理利用模式提供科学依据。针对传统水资源评价存在的问题,以乌裕尔河流域为例,利用研究区已建立的SWAT模型进行流域水资源评价,并分析了流域蓝水绿水资源量的时空分布规律。研究结果表明,绿水资源量在乌裕尔河流域水资源量中占得较大比重,对维持区域水安全、粮食安全和生态系统稳定具有重要作用。把绿水资源量评估纳入到传统水资源评估体系中,并对传统的水资源管理进行革新是一项势在必行的举措。     

广东省红树林土壤碳储量及固碳潜力研究

利用文献收集和数据整合的方法,对广东省不同红树林群落和地区的碳储量及碳埋藏速率进行了系统梳理。研究发现,广东省红树林的面积为9 106.21 hm²,土壤碳储量为1 542.02 GgC,土壤碳密度为0.23 GgC/hm²。广东省内红海榄(Rhizophora stylosa)和木榄(Bruguiera gymnorrhiza)群落的土壤碳密度最高,分别是0.27和0.23 GgC/hm²,而秋茄(Kandelia candel)群落土壤碳密度最低,仅为0.13 GgC/hm²。广东13个沿海地市的红树林土壤碳储量按大小顺序为湛江(894.5 GgC)>阳江(195.4 GgC)>江门(97.7 GgC)>珠海(91.0GgC)>茂名(59.6 GgC)>汕头(51.4 GgC)>中山(49.2 GgC)>惠州(36.1 GgC)>广州(35.1 GgC)>深圳(18.3 GgC)>汕尾(10.8 GgC)>东莞(2.8 GgC)&...     

Collisions and close encounters involving massive main-sequence stars

We study close encounters involving massive main-sequence stars and the evolution of the exotic products of these encounters as common-envelope systems or possible hypernova progenitors. We show that parabolic encounters between low- and high-mass stars and between two high-mass stars with small periastrons result in mergers on time-scales of a few tens of stellar free-fall times (a few tens of hours). We show that such mergers of unevolved low-mass stars with evolved high-mass stars result in little mass-loss  (∼0.01 M_⊙)  and can deliver sufficient fresh hydrogen to the core of the collision product to allow the collision product to burn for several million years. We find that grazing encounters enter a common-envelope phase which may expel the envelope of the merger product. The deposition of energy in the envelopes of our merger products causes them to swell by factors of ∼100. If these remnants exist in very densely populated environments  ( n ≳ 10⁷ pc⁻³)  , they will suffer further collisions which may drive off their envelopes, leaving behind hard binaries. We show that the products of collisions have cores rotating sufficiently rapidly to make them candidate hypernova/gamma-ray burst progenitors and that ∼0.1 per cent of massive stars may suffer collisions, sufficient for such events to contribute significantly to the observed rates of hypernovae and gamma-ray bursts.     

Young star clusters in the Large Magellanic Cloud: NGC 1805 and 1818

We present colour–magnitude diagrams for two rich (≈10⁴ M_⊙) Large Magellanic Cloud star clusters with ages ≈10⁷ yr, constructed from optical and near-infrared data obtained with the Hubble Space Telescope . These data are part of an HST project to study LMC clusters with a range of ages. In this paper we investigate the massive star content of the young clusters, and determine the cluster ages and metallicities, paying particular attention to Be-star and blue-straggler populations and evidence of age spreads. We compare our data with detailed stellar-population simulations to investigate the turn-off structure of ≈25 Myr stellar systems, highlighting the complexity of the blue-straggler phenomenon.     

Multisite campaign on the open cluster M67 – I. Observations and photometric reductions

We report on an ambitious multisite campaign aimed at detecting stellar variability, particularly solar-like oscillations, in the red giant stars in the open cluster M67 (NGC 2682). During the six-week observing run, which comprised 164 telescope nights, we used nine 0.6-m to 2.1-m class telescopes located around the world to obtain uninterrupted time series photometry. We outline here the data acquisition and reduction, with emphasis on the optimization of the signal-to-noise ratio of the low-amplitude (50–500 μmag) solar-like oscillations. This includes a new and efficient method for obtaining the linearity profile of the CCD response at ultrahigh precision (∼10 parts per million). The noise in the final time series is 0.50 mmag per minute integration for the best site, while the noise in the Fourier spectrum of all sites combined is 20 μmag. In addition to the red giant stars, this data set proves to be very valuable for studying high-amplitude variable stars such as eclipsing binaries, W UMa systems and δ Scuti stars.     

Petrogenesis of the Palaeoproterozoic Xishankou pluton,northern Tarim block,northwest China: implications for assembly of the supercontinent Columbia

The Tarim block, one of the largest cratons in China, records an important part of the Proterozoic crustal evolution of the Earth. Many previous studies have focused on the Neoproterozoic magmatism and tectonic evolution of this block in relation to the break-up of Rodinia, although relatively little is known about its earlier tectono-magmatic history. In this article, we present detailed petrographic, geochronologic, whole-rock geochemical, and in situ zircon Hf isotope data for the pre-Neoproterozoic Xishankou granitoid pluton (XBP), one of several blue quartz-bearing granitoid intrusions well exposed in the Quruqtagh area, and discuss these intrusions in terms of their tectonic environment. Zircon LA-ICP-MS dating indicates that gneissic quartz diorite and granodiorite of the XBP crystallized at 1934 ± 13 and 1944 ± 19 Ma, respectively. Both underwent metamorphism essentially coeval with emplacement, a time that is compatible with the globally distributed 2.1–1.8 Ga crustal amalgamation during formation of the supercontinent Columbia. Petrographic and geochemical evidence suggest that the XBP is a continental-arc-type granite and may have been generated by the partial melting of Archaean thickened lower crust; this would suggest that the northern Tarim block was a continental-type arc at ca. 1940 Ma. Our new data, together with previous regional geological studies, indicate that a series of Palaeoproterozoic (ca. 2.0–1.8 Ga) tectono-magmatic events occurred in the northern Tarim attending the assembly of Columbia.