惠东—连县地学断面的地壳结构及性质研究

本文利用地球物理－地质球化学相结合的研究方法，分析了惠东－连县地学断面的地球物理特征及其速度密度模型，探讨了断面地壳的物质组成、结构和深部地壳的形成时代，认为该断面地壳的物质组成以长英质为主，低绿片岩相及沉积盖层组上地壳的三部分。     

基于语义的地球物理信息检索模型研究

针对网络上地球物理领域的信息资源复杂多样,而传统的信息检索方法在检索地球物理信息时结果比较片面这一问题,将本体技术与传统信息检索技术相结合,建立了一个基于语义的地球物理信息检索系统模型。研究了地球物理领域的本体特征,并设计建立了本体库;提出了计算地球物理领域本体的语义相似性方法,分析了地球物理爬虫的工作机制;最后编程实现了系统的主体功能,验证了系统模型设计的合理性、可行性。     

小波分析应用研究

本文介绍了小波分析的方法原理和Ｍａｌｌａｔ快速算法，探讨了小波分析在地球物理领域中的作用，结合我们的工作，给出了地球物理异常分解，信号的奇异性检测，物化探数据去噪和滤波以及数据压缩与信号重构等应用方面的理论分析和小波应用方法。     

高频渐近散射理论及其在地球物理场数值模拟与反演成像中的应用——研究历史与研究现状概述以及若干新进展

为了对高频渐近散射理论及其在地球物理场数值模拟与反演成像中的应用有一个提纲挈领的了解,对与之有关的研究历史和研究现状进行了概述,并对近5年内笔者在这个领域中所取得的一些进展做了介绍。针对目前文献中所存在的一些问题,首先,对散射理论中的一些基本概念和基本公式进行了回顾,并对这些概念和公式的数学物理内涵进行了重申和强调;其次,对高频渐近散射理论的研究历史和研究现状及其在地球物理场数值模拟与反演成像中的应用成效进行了概述;再次,对近5年内笔者所取得的一些研究进展进行了介绍,其中包括对面积分方程的拟解析近似、广义Beam-Born（Beam-Rytov）型近似以及弱散射近似所引入的误差等等;最后,对高频渐进散射理论的自身发展及其在地球物理场数值模拟与反演成像中的应用前景进行了展望。无论是在历史上还是在现阶段,高频渐近散射理论在地球物理场数值模拟与反演成像中一直占有不可替代的地位,尤其是在反射地震偏移成像和全波形反演研究中更是如此。高频渐近散射理论的进一步发展依赖于对高频渐近Green函数的研究。随着相应研究的不断深入,高频渐近散射理论今后将会在地球物理场数值模拟与反演成像领域中发挥更大的作用。     

多参数航空地球物理研究的计算机化技术

本文论述了俄联邦近来随着程控航空地球物理测量系统的研制成功和仪器组成的扩大和质量的提高，为了保证充分开发航空测量方法和仪器的潜力，提高航空地球物理测量的地质效果和经济效益而建立的较新的航空测量技术，并着重阐述了这种技术的最重要的要素，即在高效率现代个人计算机的基础上建立的全套自动计算机设备。使用这套设备能使地球物理研究的全过程完全自动化，完成多参数航测数据的加工处理和解释。采用这种新技术能使应用过     

预测铀矿靶区时航空地球物理资料及放射性地球化学参数处理的计算机操作

本文论述了通过应用γ的全能谱分析方法处理放射性测量数据，保证了最终获得资料的真实性和信息量；指出了现代航空地球物理综合测量系统的资料处理和解释的组成；总结出主要铀矿区的三方面的放射性地球化学特征。最后再次指出，航空地球物理资料的处理和解释方法在俄罗斯等国的矿床普查中取得了成功。实践证明，可以有效地用于预测和普查铀矿床。     

关于在《地球科学进展》杂志开辟“发展战略论坛”专栏的公告

2004年是我国制定中长期规划、“十一五”规划的关键一年，为了给我国制定地球科学和资源环境领域以及全球变化研究方面，提供有参考价值的文献，《地球科学进展》从2004年第4期起开辟“发展战略论坛”专栏，邀请各领域的专家学者，就我国学科发展方向发表自己的见解，主要刊登地球科学（包括地理学、地质学、地球化学、地球物理、空间物理、大气科学和海洋科学等分支学科）、地球系统科学.     

地球物理技术在页岩气勘探开发中的应用和前景

我国页岩气勘探开发技术还处于探索阶段,对页岩气的研究主要集中在页岩气的成藏模式、地质特征等方面。针对地球物理技术在页岩气勘探和开发中所能发挥的作用及页岩气勘探和开发对地球物理方法提出的新要求,简述了我国页岩气资源分布及美国页岩气的勘探开发情况;从页岩气资源评价参数出发,系统地阐述了地球物理方法在页岩气勘探和开发中能解决的一些问题;提出了针对页岩气的地球物理方法的发展建议。      

地球深部物质科学在地球深部研究中的作用和意义

为解决地球深部探测过程中地球物理和地球化学两大系列研究成果无法联系和统一的难题，地球深部物质科学应运而生。该学科既要研究组成地球深部的一切物质实体的物理和化学的属性，又要从物质的角度去研究地球深部的结构和动力学过程。随着该学科的发展，将会为地球深部的观测结果和计算模拟结果赋予物质内容，从而促进对地球深部的物质组成、结构分层以及动力学形成统一认识，建立适合于各学科的地球深部模型。     

工程测量在地球物理探矿中准确性的方法研究

工程测量的准确度是地球物理勘探方法具有可信度得前提,通过分析工程测量方法在提高地球物理勘探准确性中所起的作用,分析提出提高工程测量准确性的的方法流程。使工程测量以及地球物理勘探成果在下一步的地质工作中更具指导性。     

动高压物理在地球与行星科学研究中的应用

综述了动高压物理应用于地球和行星科学研究中的一些最新进展,包括地球内部的物质组成与热力学状态,巨行星的物质组成模型,太阳系中的碰撞成坑与吸积相互作用等。依据铁的冲击波数据,结合其他热力学数据,可以得到一条统一的铁的熔化曲线,将动高压与静高压数据完全统一,初步解决了长期困扰高压界的动、静压关于铁的熔化温度存在系统偏差的诘难。外推到ICB处(330 GPa),铁的熔化温度(亦称锚定温度)约为(5 950±100) K。冲击Hugoniot 数据,结合地震学模型可以约束地幔与地核的物质组成。冲击压缩下钙钛矿型(Mg0 9,Fe0 1)SiO3的高压声速测量结果表明,1 770 km深度的不连续面不仅是一个相变界面而且是一个化学成分或矿物学分界面。低温可凝聚气体(H2、He)或冰(H2 O, CH4, CO2, NH3 和N2 )的冲击波数据,及Jeffrey 数等其他数据可以用来构建巨行星(如木星和土星)的物质组成模型。地球深部矿物的冲击温度测量可以用来研究它们的高压熔化行为,据此建立的高压相图可以为控制地幔对流的地幔物质的准静态蠕变提供约束条件。熔融硅酸盐在上地幔压力条件下的冲击压缩数据,可以约束地幔熔岩稳定存在的深度,在此深度地幔熔岩不会因固体围岩提供的浮力而向上运移到地表,从而在此深度形成稳定的低速带。冲击波数据在描写行?     

The split fate of the early Earth,Mars, Venus,and Moon

Plate tectonics shaped the Earth, whereas the Moon is a dry and inactive desert, Mars probably came to rest within the first billion years of its history, and Venus, although internally very active, has a dry inferno for its surface. Here we review the parameters that determined the fates of each of these planets and their geochemical expressions. The strong gravity field of a large planet allows for an enormous amount of gravitational energy to be released, causing the outer part of the planetary body to melt (magma ocean), helps retain water on the planet, and increases the pressure gradient. The weak gravity field and anhydrous conditions prevailing on the Moon stabilized, on top of its magma ocean, a thick buoyant plagioclase lithosphere, which insulated the molten interior. On Earth, the buoyant hydrous phases (serpentines) produced by reactions between the terrestrial magma ocean and the wet impactors received from the outer solar system isolated the magma and kept it molten for some few tens of million years. The planets from the inner solar system accreted dry: foundering of wet surface material softened the terrestrial mantle and set the scene for the onset of plate tectonics. This very same process also may have removed all the water from the surface of Venus and added enough water to its mantle to make its internal dynamics very strong and keep the surface very young. Because of a radius smaller than that of the Earth, not enough water could be drawn into the Martian mantle before it was lost to space and Martian plate tectonics never began. The radius of a planet is therefore the key parameter controlling most of its evolutional features.     

Earth and Mars – Distinct inner solar system products

Composition of terrestrial planets records planetary accretion, core–mantle and crust–mantle differentiation, and surface processes. Here we compare the compositional models of Earth and Mars to reveal their characteristics and formation processes. Earth and Mars are equally enriched in refractory elements (1.9 × CI), although Earth is more volatile-depleted and less oxidized than Mars. Their chemical compositions were established by nebular fractionation, with negligible contributions from post-accretionary losses of moderately volatile elements. The degree of planetary volatile element depletion might correlate with the abundances of chondrules in the accreted materials, planetary size, and their accretion timescale, which provides insights into composition and origin of Mercury, Venus, the Moon-forming giant impactor, and the proto-Earth. During its formation before and after the nebular disk's lifetime, the Earth likely accreted more chondrules and less matrix-like materials than Mars and chondritic asteroids, establishing its marked volatile depletion. A giant impact of an oxidized, differentiated Mars-like (i.e., composition and mass) body into a volatile-depleted, reduced proto-Earth produced a Moon-forming debris ring with mostly a proto-Earth's mantle composition. Chalcophile and some siderophile elements in the silicate Earth added by the Mars-like impactor were extracted into the core by a sulfide melt (∼0.5% of the mass of the Earth's mantle). In contrast, the composition of Mars indicates its rapid accretion of lesser amounts of chondrules under nearly uniform oxidizing conditions. Mars’ rapid cooling and early loss of its dynamo likely led to the absence of plate tectonics and surface water, and the present-day low surface heat flux. These similarities and differences between the Earth and Mars made the former habitable and the other inhospitable to uninhabitable.     

试论地球演化历史中水的总体行为

在地球不均匀吸积模型的基础上，根据比较行星学所获得的行星演化理论、大陆进化的历史、板块运动的特点以及高温高压实验研究结果，对地球演化历史中水的总体行为进行了分析和推论。从而对地球原始壳的特点、地球上液态水成因、地球表面缺失最初８亿年历史的原因、水的总体运移趋势等有了一些新的认识     

Experimental Test of Possible Formation of Diamond under the Differentiation of the Earth

The first results are presented for the synthesis of diamond at 6.5 GPa and 1600°C during migration of molten iron through a silicate matrix, which is composed of olivine crystals with interstitial graphite. The experiment shows that diamonds in the Earth’s mantle and the terrestrial planets could have formed during differentiation. Diamond crystals, which were formed during iron segregation of the Earth’s differentiation, could be centers for further crystallization of mantle diamonds.

     

科学大洋钻探：成就与展望

在回顾ODP学术目标的发展历史的基础上，按照地球环境动力学和地球内部动力学两大科学主题，对ODP在地球环境变化、作为环境变化营力的沉积物、流体和细菌、地球内部物质和能量的传递、岩石圈变形和地震作用等前沿领域所取得的主要科学成就进行了简单的介绍。IODP将以地球系统科学的思想为指导，利用多个钻探平台，以更为广泛的钻探领域和更深的钻探深度，对全球海底进行学术目标更为庞大、系统的科学钻探，并进一步加强与石油工业以及其它国际地学研究计划的合作。     

On the implications of the coupled evolution of the deep planetary interior and the presence of surface ocean water in hydrous mantle convection

We investigate the influence of the deep mantle water cycle incorporating dehydration reactions with subduction fluxes and degassing events on the thermal evolution of the Earth as a consequence of core–mantle thermal coupling. Since, in our numerical modeling, the mantle can have ocean masses ∼12 times larger than the present-day surface ocean, it seems that more than 13 ocean masses of water are at the maximum required within the planetary system overall to partition one ocean mass at the surface of the present-day Earth. This is caused by effects of water-dependent viscosity, which works at cooling down the mantle temperature significantly so that the water can be absorbed into the mantle transition zone and the uppermost lower mantle. This is a result similar to that without the effects of the thermal evolution of the Earth's core (Nakagawa et al., 2018). For the core's evolution, it seems to be expected for a partially molten state in the deep mantle over 2 billion years. Hence, the metal–silicate partitioning of hydrogen might have occurred at least 2 billion years ago. This suggests that the hydrogen generated from the phase transformation of hydrous-silicate-hosted water may have contributed to the partitioning of hydrogen into the metallic core, but it is still quite uncertain because the partitioning mechanism of hydrogen in metal–silicate partitioning is still controversial. In spite of many uncertainties for water circulation in the deep mantle, through this modeling investigation, it is possible to integrate the co-evolution of the deep planetary interior within that of the surface environment.     

软流层的地球膨胀成因及其形成时间

地球的软流层(圈)堪称全球构造、岩浆与成矿作用动力之源。以往人们虽然认识到软流层的重要作用,但其形成机制的定量研究还不够。最近20多年来,对地球半径变化的检验研究结果表明,地球膨胀已经有了较多的直接证据。而且,即使按照地球膨胀晚期0.1 mm/a的半径增长率计算,所产生的地球膨胀构造动力事件,也将是一个全球性超级构造动力事件。根据地球的非线性有限膨胀演化,所提出的软流层成因是:源于原始地球深部的膨胀内压,推挤原始地幔顶部物质做功并转化为原始岩石圈球壳围限下的地幔顶部物质的压缩能A,当压缩能的积累超过原始地幔顶部物质局部熔融所需要的热能Ω时,地幔顶部物质便开始熔融并逐渐形成地球的原始软流层。据此,按照地球非线性膨胀演化初期的半径增长率1.08 mm/a、原始地幔顶部物质以15%的局部熔融和绝热等压过程估算,地球开始膨胀后仅19.2 Ma,地球的原始软流层(圈)便可形成。     

Solubility of hydrogen and carbon in reduced magmas of the early Earth’s mantle

The solubility of volatile compounds in magmas and the redox state of their mantle source are the main factors that control the transfer of volatile components from the planet’s interior to its surface. In theories of the formation of the Earth, the composition of gases extracted by primary planetary magmas is accounted for by the large-scale melting of the early mantle in the presence of the metallic Fe phase [1, 2]. The fused metallic Fe phase and the melted silicate material experienced gravitational migration that exerted influence upon the formation of the metallic core of the planet. The large-scale melting of the early Earth should have been accompanied by the formation of volatile compounds, whose composition was controlled by the interaction of H and C with silicate and metallic melts, a process that remains largely unknown as of yet.     

An approach to the geologic history of the Earth’s mantle geospheres

The geospheres that make up the Earth’s mantle, i.e., the upper, middle, and lower mantle, as well as dividing zones of discontinuity, are autonomous geological bodies whose geologic history is poorly known. The data on evolution of planetary magmatism and mineral transformations along the Earth’s radius, thermobaric information on the Earth’s interior, and new geodynamic reconstructions are used to outline the geologic history of deep geospheres. In broad terms, we suggest that layer D″, the lower mantle, and the Eoarchean basic protocrust were the first to be formed after differentiation of the protoplanetary material. The sialic crust appeared in the Paleoarchean. The system that comprised layer D″ the lower mantle, and discontinuity II was formed later, ～2.6 Ga ago, while the upper mantle and discontinuity I originated ca. 1.6–1.7 Ga ago. Thus, the within-mantle geospheres were formed in their present-day appearance over a long period of time.