流体包裹体中微量气体组成及其成矿示踪体系研究新进展

N2 Ar He体系可用以示踪成矿流体及温泉等与火山有关的水流体的来源 ,当体系中He含量低于检出限 ,N2 Ar He体系不能用时 ,CO2 /CH4 N2 /Ar体系可用于识别成矿流体中岩浆水、建造水和大气降水 ,CO2 CH4 H2 体系可以鉴别成矿流体是否发生过沸腾作用以及沸腾是在开放体系还是封闭体系中形成 ,一般开放体系中沸腾有利于成矿。CO2 CH4 C2 H6体系可用于判别岩浆作用是否直接影响成矿或对成矿流体的贡献 ,从而确定热液矿床的成因。CH4 C2 H6 C3 H8体系可用来示踪一些与干酪根热解有关的成矿流体长距离、大规模迁移过程。C2 H6 C3 H8 C6H6体系可用于判定成矿流体的大地构造环境 ,因岛弧与裂谷环境下C2 H6/C3 H8比值有明显差异。以广东长坑 (Au Ag)和嵩溪 (Ag Sb)矿床为例 ,概述了这些体系各自的应用     

长江口南汇边滩冲淤变化规律与机制

根据1842—2004年海图资料分析发现,南汇边滩存在近百年尺度的强烈冲刷—淤积旋回。长江主泓走南港或北港是造成冲刷期"北滩、东滩淤积,南滩、过渡带冲刷"或淤积期冲淤态势反相的主要原因;冲刷期内风暴强度和频数明显多于淤积期,造成冲刷期滩面叠置记忆的是暴风浪成因的"高滩冲刷、低滩淤积"的冲淤态势,而淤积期保存的是弱风浪成因的"高滩淤积、低滩冲刷"叠置增强的剖面特征。尽管三角洲整体冲淤态势的转变主要受流域来沙量的控制,但不同岸段受河口河势分水分沙作用、潮流和波浪等共同作用,明显存在此冲彼淤、冲淤动态调整等特征。已有的入海泥沙含量阈值研究以点代面或以局部代整体,这是造成阈值估算偏高的主要原因。2003年三峡水库开始蓄水后平均年输沙量154 Mt/a已低于低阈值184 Mt/a,但三角洲尚未如预测那样发生由净淤积向净侵蚀的转变。已有的河口水文观察资料显示,水体含沙量也未发生明显下降,这可能是潮控型三角洲潮流对泥沙在河口的再分配起主导作用,并可能由此延长三角洲冲淤转变对入海泥沙量减少的滞后。今后需进一步加强潮控型河口复杂过程的综合研究,提高对泥沙含量阈值估算和应对可能面临的海岸侵蚀及其相关的环境地质灾害的能力。     

A Modified Double-Moment Bulk Microphysics Scheme Geared toward the East Asian Monsoon Region

Representation of cloud microphysical processes is one of the key aspects of numerical models. An improved doublemoment bulk cloud microphysics scheme(named IMY) was created based on the standard Milbrandt-Yau(MY) scheme in the Weather Research and Forecasting(WRF) model for the East Asian monsoon region(EAMR). In the IMY scheme, the shape parameters of raindrops, snow particles, and cloud droplet size distributions are variables instead of fixed constants.Specifically, the shape parameters of r...     

俄罗斯阿尔丹地块西部穆龙斯克杂岩体中的碱性交代岩

含紫硅碱钙石、镁钠钙闪石（钠透闪石－石棉）及蓝色软透闪石的碱性交代岩的形成首先是由硅酸和碱（Ｎａ２Ｏ和Ｋ２Ｏ的不同作用）的隋性及ＦｅＯ,ＭｇＯ,ＣａＯ和Ａｌ２Ｏ３的强烈活性决定的。含蓝色软透闪石和镁钠钙闪石（钠透闪石－石棉）的交代岩是岩浆期后溶解演化的中期产物,而含紫硅碱钙石的交代岩却是其晚期的产物。     

帕米尔弧形构造带东北缘晚新生代构造活动的沉积与重矿物变化响应

帕米尔弧形构造带东北缘晚新生代沉积特征的研究对于理解帕米尔构造带弧形扩展机制具有重要意义.本文通过对帕米尔弧形构造带东北缘的晚新生代沉积地层的沉积特征对比研究和重矿物采样与组份分析,建立了帕米尔弧形构造带东北缘地区的晚新生代沉积联合柱状对比图和重矿物组份变化曲线.研究结果表明,晚新生代沉积与重矿物变化主要记录了帕米尔弧...     

往复潮流作用下推移质粒径趋势形成模拟初探

粒径趋势分析是一种用于判断海洋环境中沉积物净输运方向的方法,但是至今粒径趋势形成的物理机制尚不够清楚,因而影响了粒径趋势分析适用条件的确定。针对这个问题,本文通过建立一维、推移质、往复流（近岸潮流）条件下的数值模型,采用正演方法模拟粒度参数在输运方向上的分布．以评价沉积动力过程的影响,初步探讨粒径趋势形成的物理机制。数值模型实验的初步结果显示,水动力条件的空间差异导致的沉积物粒度参数的空间分布符合粒径趋势分析的假设,粒径趋势分析中定义的两种粒径趋势可由沉积物输运强度的空间梯度而形成,并且在沉积物净输运方向上出现的频率最高。     

Time–space fractional governing equations of one‐dimensional unsteady open channel flow process: Numerical solution and exploration

Although fractional integration and differentiation have found many applications in various fields of science, such as physics, finance, bioengineering, continuum mechanics, and hydrology, their engineering applications, especially in the field of fluid flow processes, are rather limited. In this study, a finite difference numerical approach is proposed to solve the time–space fractional governing equations of 1‐dimensional unsteady/non‐uniform open channel flow process. By numerical simulations, results of the proposed fractional governing equations of the open channel flow process were compared with those of the standard Saint‐Venant equations. Numerical simulations showed that flow discharge and water depth can exhibit heavier tails in downstream locations as space and time fractional derivative powers decrease from 1. The fractional governing equations under consideration are generalizations of the well‐known Saint‐Venant equations, which are written in the integer differentiation framework. The new governing equations in the fractional‐order differentiation framework have the capability of modelling nonlocal flow processes both in time and in space by taking the global correlations into consideration. Furthermore, the generalized flow process may possibly shed light on understanding the theory of the anomalous transport processes and observed heavy‐tailed distributions of particle displacements in transport processes.     

A search for electron cyclotron maser emission from compact binaries

Unipolar induction (UI) is a fundamental physical process, which occurs when a conducting body transverses a magnetic field. It has been suggested that UI is operating in RX J0806+15 and RX J1914+24, which are believed to be ultracompact binaries with orbital periods of 5.4 and 9.6 min, respectively. The UI model predicts that those two sources may be electron cyclotron maser sources at radio wavelengths. Other systems in which UI has been predicted to occur are short period extrasolar terrestrial planets with conducting cores. If UI is present, circularly polarized radio emission is predicted to be emitted. We have searched for this predicted radio emission from short period binaries using the Very Large Array (VLA) and Australian Telescope Compact Array (ATCA). In one epoch, we find evidence for a radio source, coincident in position with the optical position of RX J0806+15. Although we cannot completely exclude that this is a chance alignment between the position of RX J0806+15 and an artefact in the data reduction process, the fact that it was detected at a significance level of 5.8σ and found to be transient suggests that it is more likely that RX J0806+15 is a transient radio source. We find an upper limit on the degree of circular polarization to be ∼50 per cent. The inferred brightness temperature exceeds 10¹⁸ K, which is too high for any known incoherent process, but is consistent with maser emission and UI being the driving mechanism. We did not detect radio emission from ES Cet, RX J1914+24 or Gliese 876.     

Thermal desorption of water ice in the interstellar medium

Water (H₂O) ice is an important solid constituent of many astrophysical environments. To comprehend the role of such ices in the chemistry and evolution of dense molecular clouds and comets, it is necessary to understand the freeze-out, potential surface reactivity and desorption mechanisms of such molecular systems. Consequently, there is a real need from within the astronomical modelling community for accurate empirical molecular data pertaining to these processes. Here we give the first results of a laboratory programme to provide such data. Measurements of the thermal desorption of H₂O ice, under interstellar conditions, are presented. For ice deposited under conditions that realistically mimic those in a dense molecular cloud, the thermal desorption of thin films (≪50 molecular layers) is found to occur with zeroth-order kinetics characterized by a surface binding energy, E _des, of 5773 ± 60 K, and a pre-exponential factor, A , of 10^30 ± 2 molecules cm⁻² s⁻¹. These results imply that, in the dense interstellar medium, thermal desorption of H₂O ice will occur at significantly higher temperatures than has previously been assumed.