推进古地磁研究的着力点

通过对当代古地磁研究现状的分析及今后前景的展望,本文着意深化古地磁研究在地球系统科学发展中可能继续发挥重要作用的正确认识,强化选用古地磁数据必须把握其可靠程度的科学意识。本文强调,对古地磁学及其物理化学基础的岩石磁学,急切需要在基础研究和实际应用等方面开展高水平的理论与实验工作。     

柴达木地块古地磁研究及其演化

根据柴达木地块获得的6个古地磁数据,结合已知的古地磁数据阐述了柴达木地块及与相邻板块间的演化模式.结果表明柴达木地块从震旦纪到石炭纪一直处于赤道附近和低纬度地区.石炭纪时,柴达木、杨子及走廊过渡带三地块均处在赤道附近,三者可能是连在一起的.而华北板块与上述三地块至少有10°左右的纬向差,因此,华北与柴达木、杨子和走廊过渡带当时还没有连在一起.     

北祁连山古生代和中生代岩石古地磁的初步研究

本文通过对北祁连山近90个上古生代和中生代岩石样品的热退磁、交变退磁和剩余磁性的初步测定,认为石炭纪、二叠纪和侏罗纪岩石的剩余磁化强度已被现代地磁重新磁化;而上泥盆纪和三叠纪的剩余磁性可能是原生的,说明这一时期北祁连山地体有较大的北向移动,但三叠纪时尚未达到目前的地理位置。     

河西走廊地块古生代地层古地磁初步研究

古地磁初步研究结果表明,早古生代阶段,河西走廊过渡带与阿拉善地块古纬度接近,且漂移过程中形影相随,说明其间并无洋盆相隔。志留纪末,河西走廊过渡带与阿拉善地块拼接,但二者磁极位置与古方位均有差异,可能表明走廊过渡带相对于阿拉善地块同时作了顺时针旋转。泥盆纪时,两地块古纬度一致,但古方位不同,可能反映在碰撞拼合后二者间仍有相对的旋转运动。二叠纪时,二块体的空间位置及其配置关系已与现状接近。     

最新的岩石圈磁场模型及中国磁异常特征的几点认识

介绍了最新的地球磁场模型,包括MF5,NGDC-720和WDMAM。模型MF5是由CHAMP卫星测量得来,它的球谐展开阶次为n=16~100,对应的波长段为400~2500km。模型NGDC-720和WDMAM是综合了卫星磁测、航空磁测、海洋磁测与地面磁测得到数据经过处理后得来,它们有不同的球谐阶次和分辨率。NGDC-720模型是由美国国家地球物理数据中心(The National Geophysical Data Center,NGDC)提供,它的球谐阶次从16阶到720阶,对应于由2500km到56km的波带。M.Purucker博士公布的WDMAM参考模型1是一张分辨率为3′,高度位于WGS84上方5km的磁异常图,它向上延拓后的结果与MF5中的岩石圈磁异常保持一致。作者根据国际上公布的CHAMP、NGDC-720与WDMAM Candidate1的最新数据,绘制了中国及毗邻地区的磁异常图,对中国及毗邻地区明显的大地构造,如造山带,盆地等地区的磁异常特征进行了描述和分析,塔里木、四川、松辽等盆地地区及华北平原部分地区模型中均表现为正异常,西藏高原、天山造山带等地区表现为负异常,而一些深大断裂表现为磁异常高梯度带。通过四川盆地和西藏高原地区三个模型的相互对比,我们发现模型阶次越高,它所反映的磁性体(尤其是浅部地质体)的情况越丰富,不同的是四川盆地的结果随着阶次的增高就越接近航磁结果,而西藏高原随着阶次的增高却和航磁结果差别越来越大。     

从古地磁研究看中国大陆形成与演化过程

古地磁学是进行大陆板块或微板块(地块)运动演化过程和古地理重建的最有效手段之一。近半个世纪以来,通过中外学者艰苦卓绝的努力,在中国大陆上积累了大量的古地磁数据,为中国大陆各主要块体的起源、构造演化和碰撞拼合过程等提供了定量约束。文中根据现代古地磁数据可靠性判别标准,对扬子、华北及塔里木地块显生宙古地磁数据进行了重新分析和筛选,结合拉萨和喜马拉雅地块的古地磁数据,对中国大陆的形成和演化提出了几点认识:(1)古生代中国大陆各主要块体基本位于赤道附近的低纬度地区;早古生代扬子、华北及塔里木地块与东冈瓦纳大陆关系密切;(2)中生代是中国大陆各主要块体发生碰撞和拼合的主要时期;(3)中国大陆主要块体间的碰撞和拼合具有局部首先碰撞、相互旋转、完全拼合、陆内挤压造山和伸展反弹的特点。     

闽粤晚白垩世古地磁学研究

在福建沙县至上杭、广东兴宁至河源上白垩统采集古地磁学定向样品３９０个（３９个采点）,进行了古地磁学研究,研究表明,闽粤两地的晚白垩世地磁学数据具有廊的重合性,福建：古地磁偏角１１．７°,地磁倾角４２．９°,地磁极位置北纬７９．４°,东径２１０．３°;广东;古地磁偏角１０．７°,古地磁倾角４４．０°,古地磁有位置北纬８０．１°,东径１９３．４°,该古寺磁学数据反映了中国华南地区自晚白垩世至今曾经厍过     

华北陆块早三叠世刘家沟组古地磁学新数据

在河北武安大淑村刘家沟组布采点１３个,采样９１个,进行了古地磁学研究,研究结果表明,华北陆块与陆块在早三叠世时尚未形成一体,自上三叠世至今,华北陆块以反时针,扬子陆块以顺时针,各自旋转了数十度。     

华南早三叠世的古地磁学与大地构造

从华南几个具代表性地点的下三叠统灰岩中,获得了有意义的古地磁学初步结果。这些结果支持华南存在分离板块的设想。根据新近获得的地质与古地磁学证据,推断华南存在4个岩石图板块。它们是扬子(D=232.4°,I=-11.8°,K=28.2,α₉₅=5.5°),湘桂(D=198.0°,I=32.2°,α₉₅=12.9°),华夏(D=88.0°,I=13.0°,K=20.1,α₉₅=9.1°)和海南(上二叠统D=338.2°,I=15.9°,K=10.2,α₉₅=14.3°)板块。4个板块的古地磁极位分散,纬度差明显,并存在碰撞后的局部与区域性的旋转作用,尤其是顺时针旋转。华南早中生代的大地构造可理解为4个来自古特提斯和冈瓦纳的岩石圈碎块与欧亚大陆聚合作用的产物。     

A Comparative Analysis of Evaporate Sediments on Earth and Mars：Implications for the Climate Change on Mars

The knowledge of Martian salts has gone through substantial changes during the past decades. In the 70th of last century, Viking landers have noticed the existence of salts on Mars. Several salt species have been suggested from then on, such as sulfates and chlorides. However, their origin was a mystery due to the lack of observations. The recent explorations and related studies at the beginning of this century revealed that the crustal composition of Mars is similar to that of Earth, and it was hypothesized that almost one third of Martian surface was covered by oceans and lakes in the early stage of Mars. The huge water bodies may have dissolved a large quantity of ions from Martian primary rocks during the whole Noachian and Hesperian epoch. After the enormous drought event happened during the late Hesperian and the early Amazonian, these dissolved ions have formed huge salts deposits and most of them were preserved on Mars until today. To date, carbonates, sulfates, chlorides have all been detected by orbital remote sensing and by landers and rovers. However, the salt mineral assemblages on Mars seems to have some differences from those on Earth, e.g., rich in sulfates and lack of massive carbonates. To explain this difference, we propose that most of the surface carbonates precipitated from the ancient oceans may have been dissolved by the later ubiquitous acidic fluids originated from the global volcanism in the Hesperian era, and formed the enormous sulfate deposits as detected, and this hypothesis seems to be supported by the evidence that most of the sulfate deposits distribute around the Tharsis volcanic province while the survived carbonates located far from it. This process can release most of the carbon on Mars to the atmosphere in the form of CO2 and then be erased by the late heavy bombardments, which might have profound influence on the climate change happened in the Hesperian age. The positive correlation between the GRS results of the potassium distributions and the distribution of chlorides on Mars, together with the high Br concentration measured from the evaporate sediments at two Mars exploration rover landing sites, indicate that the brines in the regions where the chlorides deposited may have reached the stage for potassium salts deposition, thus we propose for the first time that potassium salts deposits might be prevalent in these regions.     

Evidence for a simple pathway to maghemite in Earth and Mars soils

Soil magnetism is greatly influenced by maghemite (γ-Fe₂O₃), the presence of which is usually attributed to the following: (1) heating of goethite in the presence of organic matter; (2) oxidation of magnetite (Fe₃O₄); or (3) dehydroxylation of lepidocrocite (γ-FeOOH). Formation of the latter two minerals in turn requires the presence of Fe(II) in the system. No laboratory experiment or soil study to date has shown whether maghemite can form from ferrihydrite, a poorly crystalline Fe(III) oxide [∼Fe_4.5(O,OH,H₂O)_13.5], below 250°C. However, ferrihydrite is the usual precursor of goethite (α-FeOOH) and hematite (α-Fe₂O₃), the most frequently occurring crystalline Fe(III) oxides in soils. Here is presented in vitro evidence that ferryhidrite can partly transform into maghemite at 150°C. This transformation occurs upon aging of ferrihydrite precipitated in the presence of phosphate or other ligands capable of ligand exchange with Fe-OH surface groups. This maghemite coexists with hematite and is a transient phase in the transformation of ferrihydrite to hematite, which is apparently stabilized by the adsorbed ligands. Its particle size is small (10 to 30 nm), and its X-ray diffraction pattern exhibits superstructure reflections. The possible formation of maghemite in Mars and in different Earth soils can partly be explained in the light of this pathway with minimal ad hoc assumptions.     

Saltation threshold on Earth, Mars and Venus

New formulations valid for wide ranges of particle diameter and density and gas density are presented for prediction of saltation threshold speed for small particles. A low-air-density wind tunnel was used to extend the range of previous investigations and to separate the effects of Reynolds number and interparticle forces of cohesion. The new formulations are used to predict saltation threshold for atmospheric conditions on the surface of the Earth, Mars, and Venus.     

The contribution of sulphur dioxide from ablating micrometeorites to the atmospheres of Earth and Mars

Atmospheric composition is a key control on climate and the habitability of planetary surfaces. Ablation of infalling micrometeorites has been recognised as one way in which atmospheric chemistry can be changed, especially at times in solar system history when the infall rates of exogenous material were high. Despite its potential to influence climate and habitability, extraterrestrial sulphur dioxide is currently an unquantified contribution to the atmospheres of the terrestrial planets. We have used flash pyrolysis to simulate the atmospheric entry of micrometeorites and Fourier-transform infrared spectroscopy to identify and quantify the sulphur dioxide produced from the carbonaceous meteorites Orgueil (CI1), ALH 88045 (CM1), Cold Bokkeveld (CM2), Murchison (CM2) and Mokoia (CV3). We have used this approach to understand the introduction of sulphur dioxide to the atmospheres of Earth and Mars from infalling micrometeorites. Sulphates, present in carbonaceous chondrites at a few wt.%, are resistant to thermal decomposition, limiting the yields of sulphur dioxide from unmelted micrometeorites. Infalling micrometeorites are a minor source of present-day sulphur dioxide on Earth and Mars, calculated to be up to around 2400 tonnes and about 350 tonnes, respectively. During the Late Heavy Bombardment (LHB), the much greater infall rates of micrometeoritic dust are calculated to be associated with average production rates of sulphur dioxide of around 20 Mt yr⁻¹ for the early Earth and 0.5 Mt yr⁻¹ for early Mars, for a LHB of 100 Myr. These rates of delivery of sulphur dioxide at high altitudes would have reduced the solar energy reaching the surfaces of these planets, via scattering of sunlight by stratospheric sulphate aerosols, and may have had detrimental effects on developing biospheres by promoting cooler climates and reducing the probability of liquid water on planetary surfaces.     

从"全球冰川"到"雪球假说"——关于新元古代冰川事件的最新研究

新元古代冰期地层不同于显生宙冰期地层，近年来，一些学者提出了雪球假说，掀起了关于新元古代冰期环境特征与因演化的研究热潮，成为当前地学前沿的一个热门课题。本轮研究的一个突出特点，是它的高度综合性，涉及岩石圈，水圈，大气圈和生物圈，此外还牵攫到天体运行等学科。研究重点有新元古代冰川作用的低纬和低海拔特征。与Rodinia超大陆裂解的关系，冰室效应和温室效应的矛盾运动，海洋封冻的探索，碳酸盐岩岩帽的成因，碳，硫，锶等同位素的峰谷变化的环境含义，冰期地层中铁矿的成因，新元古代冰期的次数争议，雪球理论的数值模拟和冰期环境特征及其变化与生物演化，特别是与早寒武世生物大辐射的关系等。我国南方已成为研究新元古代冰期地层及其与寒武系生物大辐射关系的重要地区之一。     

Loess and dust on Earth and Mars: particle generation by impact mechanisms

Impact between windblown quartz grains as a source of desert dust is consistent with laboratory abrasion experiments and has received some field confirmation in the Negev. The suggestion is that an important process on Mars now gains support from laboratory studies; even though their geochemical interpretation is controversial, they show that dust generation by impact is tenable even for quartz. A simple mechanism for small dust production from sand seas is proposed; internal stresses can be mobilized by impact energy. A speculative mechanism (the andesite scenario) is proposed for fine particle production by particle impact on Mars. The internal stress range in terrestrial sand grains may vary, depending on the nature of the source rock, and this may influence particle production by impact processes.     

地球同火星蒸发岩沉积的对比

迄今为止,人类已经通过火星轨道探测器、火星着陆器及火星漫游车在火星上发现了碳酸盐、硫酸盐及氯化物等一 系列的盐类矿物,尽管整体上火星盐类矿物组合与地球上基本一致,但在许多细节方面还是和地球上有所不同。文中首先 对于火星盐类认知的现状作了简要综述;基于地球火星蒸发盐沉积及成盐作用规律的对比,预测火星表面及次表面可能存 在着广泛分布的钾盐;此外,发现火星轨道伽玛光谱仪所获的火星表面 K 的分布与火星表面已探测到的氯化物的分布有比 较强的相关性,喻示火星表面氯化物沉积地区的卤水浓度已经接近或达到钾盐形成的条件,同时指出这些地区存在钾盐的 可能性很大。     

From Paleogeographic maps to Evolving Deep-time Digital Earth models

正Major advances in computational power,as well as community modelling workflows and an improvement in data availability,has revolutionized Earth sciences over the last decade.Geological data has been synthesized into flexible and open access plate tectonic and paleogeographic reconstructions using the open-source and cross-platform GPlates (www.gplates.org)software since 2008 (Muller et al.,2018;Muller et al.,2008).These digital plate     

A Comparative Analysis of Evaporite Deposition on Earth and Mars

<正>In this paper,the authors give a brief review of recent observations and studies on Martian salts.On the basis of the comparison of salt sediments on Earth and Mars,the authors propose that potassium salts might be widespread on Martian surface and subsurface.Besides,the authors found a positive correlation between the GRS results of the po-