基于傅里叶变换质谱的烃源岩成熟度评价方法及地质意义

<正>伴随非常规油气资源的勘探开发,油气资源开采的广度和深度进一步扩大,一定程度上缓解了我国油气供需矛盾、保障了我国能源安全,同时有力推动了能源结构战略转型。但同时也对能源地质研究工作提出了新的挑战。有机质成熟度是油气评价的重要参数之一,不同成熟阶段的有机质会对应产出不同成因、不同性质、不同质量的油气,如何准确评价沉积有机质成熟度是当前油气资源勘探开发工作的关键问题之一。前人在科研实践工作中从光学、化学、谱学等角度提出了适用条件各异的成熟度评价方法,在部分地质环境中获得了良好的应用效果,但已有的成熟度指标多受测定方法原理的制约导致其适用性不同程度受限(肖贤明等,2020),制约了油气资源的高质量勘探开发。     

铜锡复合成矿研究进展与展望

铜与锡具有不同的地球化学性质,然而铜锡共生或复合成矿现象在世界主要铜、锡成矿带中比较常见,如中国的右江、南岭(湘南)、大兴安岭南段(内蒙东部)、葡萄牙伊比利亚、秘鲁安第斯、英格兰德文郡、德国厄尔士山、日本西南、俄罗斯远东、加拿大新不伦瑞克等成矿带均为铜锡复合矿床的集中产区。铜锡复合矿床主要为岩浆热液矿床,以矽卡岩型、脉状矿床为主,兼有火山热液沉积型、斑岩型及云英岩型等。铜矿体的主要矿石矿物为黄铜矿,兼有斑铜矿、黝铜矿、辉铜矿等;锡矿体的主要矿石矿物为锡石,兼有黝锡矿。铜锡复合矿床的成矿物质来源(尤其是铜、锡成矿元素的来源是否具有一致性)尚有不少争议,锡普遍被认为是岩浆来源,而铜的来源具有多样性。成矿流体演化过程中的氧化还原环境的改变及流体的混合是导致铜锡复合成矿的主要原因。目前对于铜锡复合成矿的研究,主要是从矿床的年代学、单矿物(黄铜矿、锡石)微量元素及传统同位素地球化学、流体包裹体等方面入手,但对厘定铜锡复合成矿过程的作用有限。铜锡复合矿床的成因及勘查模型的建立具有重要的理论价值及现实意义。本文提出未来研究可以从多种非传统稳定同位素(例如Cu、Sn、W、Zn同位素)的联合示踪探索、成...     

黄河流域湿地景观时空演变格局分析

湿地景观的时空演变及其驱动因素研究是湿地生态恢复与保护的重要参考,本文利用1980—2015年7期黄河流域土地利用数据构建黄河流域湿地矢量数据集,基于景观格局指数对黄河流域湿地的时空演变特征进行定量和定性分析;采用转移矩阵对每两个时期湿地资源的转移类型和数量进行计算与分析。研究结果表明,①1980—2015年,黄河流域湿地率为3.5%,其中自然湿地率约为2.0%,即黄河流域的湿地类型以自然湿地为主。②斑块面积结果显示,黄河流域湿地总面积减少了312.74km²,表现为人工湿地增加,自然湿地减少;自然湿地中沼泽湿地呈增加状态,主要是在2005—2010年增加了979.22km²,滩地呈减少状态,减少了1218.19km²,主要发生在1990—1995年和2005—2010年。斑块密度结果显示,随着河渠和滩地受人为活动影响程度的加大,两者的斑块破碎化程度逐渐加大。最大斑块指数结果显示,水田是黄河流域的主导湿地类型,沼泽和湖泊是自然湿地中的主导湿地类型。③黄河流域湿地类型与非湿地之间转换是黄河流域景观转换的主要组成部分,其中沼泽与滩地是面积发生变化的主要湿地类型。     

基于GIS的土地储备业务管理系统的研究与实现

土地是支撑城市社会经济发展和基础设施建设的空间基础,作为自然物的土地具有价值属性。土地储备涉及市土地开发中心前期部、征地部、出让部、工程部、合同部、计财部等内部职能部门,涉及测绘、规划、房管、农业、城市更新、发改、人民政府等外部单位,交互业务较多,因此土地的规划、审批、征收、出让、工程等流程复杂、管理困难。本文介绍了土地储备业务管理系统的实现思路,系统实现建立业务审批体系。规范资金使用和管理,达到海量数据高效处理、图属档一体化、实时信息在线共享、流程优化协同办理、短信督办提醒的目标,满足对土地储备情况的宏观监管和微观审批,形成完善的土地储备业务管理体系。     

江西德兴铜矿田成矿热液演化过程及其对铼差异性富集的制约

铜厂和富家坞矿床是德兴矿田中两个典型的斑岩铜矿床,二者成矿时代、成矿背景和致矿斑岩均较一致,但前者中辉钼矿的Re含量明显高于后者。为探究成矿流体演化过程对辉钼矿中Re含量差异的影响,本文对铜厂和富家坞不同成矿阶段的石英开展LA- ICP- MS微区原位分析以及流体包裹体测温研究。结果显示,二者流体均具有由高温向低温,中低盐度高盐度共存向低盐度演化的趋势,且温度下降、流体沸腾以及pH值的变化可能是导致Cu、Mo沉淀的主要原因;但就同一成矿阶段而言,铜厂比富家坞成矿温度更低,并且在主成矿阶段,铜厂具有更高的流体盐度;因此,推测温度和盐度可能是导致二者中辉钼矿Re含量差异的主导因素。     

The evolution of the z distribution of normal neutron stars in the Galaxy

Under the two initial 1‐D one parameter velocity distribution forms (one is normal, the other is exponential), the z direction scale height evolution of normal neutron stars in the Galaxy is studied by numerical simulation. We do statistics for the cases at different time segments, also do statistics for the cumulative cases made of each time segment. The results show in the cumulative cases the evolution curves of the scale heights are smoother than in the each time segment, i.e., the cumulation improve the signal‐to‐noise ratio. Certainly the evolution cases are different at different Galactic disk locations, which also have very large difference from the average cases in the whole disk. In the initial stages of z evolution of normal neutron stars, after the beginning transient states, the cumulative scale heights increase linearly with time, and the cumulative scale height increasing rates have linear relationship with the initial velocity distribution parameters, which have larger fluctuation in the vicinity of the Sun than in the whole disk. We utilize the linear relationship of the cumulative scale height increasing rates vs. the initial velocity distribution parameters in the vicinity of the Sun to make comparison with the observation near the Sun. The results show if there is no magnetic decay, then the deserved initial velocity parameters are obvious lower than the present well known results from some authors; whereas if introducing magnetic decay, for the 1‐D normal case we can make consistence among concerning results using magnetic decay time values which are supported by some authors, while for the 1‐D exponential case the results show the lackness of young pulsar samples in the larger z in the vicinity of the Sun (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Pulsations and planets: The asteroseismology‐extrasolar‐planet connection

The disciplines of asteroseismology and extrasolar planet science overlap methodically in the branch of high‐precision photometric time series observations. Light curves are, amongst others, useful to measure intrinsic stellar variability due to oscillations, as well as to discover and characterize those extrasolar planets that transit in front of their host stars, periodically causing shallow dips in the observed brightness. Both fields ultimately derive fundamental parameters of stellar and planetary objects, allowing to study for example the physics of various classes of pulsating stars, or the variety of planetary systems, in the overall context of stellar and planetary system formation and evolution. Both methods typically also require extensive spectroscopic follow‐up to fully explore the dynamic characteristics of the processes under investigation. In particularly interesting cases, a combination of observed pulsations and signatures of a planet allows to characterize a system's components to a very high degree of completeness by combining complementary information. The planning of the relevant space missions has consequently converged with respect to science cases, where at the outset there was primarily a coincidence in instrumentation and techniques. Whether space‐ or ground‐based, a specific type of stellar pulsations can themselves be used in an innovative way to search for extrasolar planets. Results from this additional method at the interface of stellar pulsation studies and exoplanet hunts in a beyond‐mainstream area are presented (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Microbial life in martian ice: A biotic origin of methane on Mars?

Despite the fact that microbial cells are unlikely to be found in the Martian soil in the near future, this paper is written on the assumption that some of the seasonally varying concentration of Martian methane is due to ongoing methanogenesis. It is first pointed out that life might have arisen on Mars first and been transported to Earth later. A case is made that an icy origin of life is more likely than a hot origin, especially if biomolecules take advantage of the high encounter rates and stability against hydrolysis, and that microorganisms feed on the ions that comprise eutectic solutions in ice. Although certain difficulties are avoided if RNA and DNA grow while adsorbed on clay grains, double strand-breaks of microbial DNA due to alpha radioactivity are a far greater threat to microbial survival on clay or other rock types than in ice. Developing a relation between the rate of microbial metabolism in ice and the experimentally determined rate of production of trapped gases of microbial origin, one can estimate the concentration of methanogens that could account for the methane production rate as a function of temperature of their habitat. The result, of order 1 cell cm⁻³ in the Martian subsurface, seems an attainable goal provided samples are taken from at least 1 or 2 m below the hostile surface of Mars. Instruments on NASA’s 2011 Mars Science Lab will measure stable isotopes for methane, water, and carbon dioxide, which on Earth served to distinguish abiotic, thermogenic, and microbial origins. Future measurements of chirality of biomolecules might also provide evidence for Martian life.     

Parametrization of single and binary stars

Stellar masses and ages are not directly observable parameters, and the methods used to determine them are based on the calibrating relations. In particular, the mass–luminosity relation, based on the masses of less than 200 well-studied binaries, is virtually the only way to estimate the mass of single stars. Thus, the development of methods for estimating stellar masses with accuracy comparable to direct methods is a problem of vital importance.
Here, we describe a method for estimating stellar masses and ages, which is based on the geometric similarity of evolutionary tracks for the stars at the same evolutionary stage in the Hertzsprung–Russell (HR) diagram. To examine the proposed approach, it has been applied to various test data sets. Application of the method, using synthetic stellar spectra Basel Stellar Library (of theoretical spectra; BaSeL), demonstrates that it allows determination of masses and ages of stars with a predictable distribution of uncertainties.
This statistical approach allows us to demonstrate the viability of the method using it on the set of double-lined eclipsing binaries with intermediate-mass and low-mass components which allows us to compare calculated characteristics with observational ones. As a result, the uncertainties of the stellar masses estimated with the proposed method are comparable with the accuracy of ones obtained from direct observations. This allows us to recommend the method for mass estimates of masses of single stars by the localization in the HR diagram.
As for the ages, the estimates for intermediate-mass stars are more reliable, while those obtained for low-mass stars are very uncertain, due both to slower movement of these stars in the HR diagram with age at stages close to the main sequence and to certain disagreements between theoretical models for this mass range.