Enceladus: Present internal structure and differentiation by early and long-term radiogenic heating

Pre-Cassini images of Saturn's small icy moon Enceladus provided the first indication that this satellite has undergone extensive resurfacing and tectonism. Data returned by the Cassini spacecraft have proven Enceladus to be one of the most geologically dynamic bodies in the Solar System. Given that the diameter of Enceladus is only about 500 km, this is a surprising discovery and has made Enceladus an object of much interest. Determining Enceladus' interior structure is key to understanding its current activity. Here we use the mean density of Enceladus (as determined by the Cassini mission to Saturn), Cassini observations of endogenic activity on Enceladus, and numerical simulations of Enceladus' thermal evolution to infer that this satellite is most likely a differentiated body with a large rock-metal core of radius about 150 to 170 km surrounded by a liquid water-ice shell. With a silicate mass fraction of 50% or more, long-term radiogenic heating alone might melt most of the ice in a homogeneous Enceladus after about 500 Myr assuming an initial accretion temperature of about 200 K, no subsolidus convection of the ice, and either a surface temperature higher than at present or a porous, insulating surface. Short-lived radioactivity, e.g., the decay of ²⁶Al, would melt all of the ice and differentiate Enceladus within a few million years of accretion assuming formation of Enceladus at a propitious time prior to the decay of ²⁶Al. Long-lived radioactivity facilitates tidal heating as a source of energy for differentiation by warming the ice in Enceladus so that tidal deformation can become effective. This could explain the difference between Enceladus and Mimas. Mimas, with only a small rock fraction, has experienced relatively little long-term radiogenic heating; it has remained cold and stiff and less susceptible to tidal heating despite its proximity to Saturn and larger eccentricity than Enceladus. It is shown that the shape of Enceladus is not that of a body in hydrostatic equilibrium at its present orbital location and rotation rate. The present shape could be an equilibrium shape corresponding to a time when Enceladus was closer to Saturn and spinning more rapidly, or more likely, to a time when Enceladus was spinning more rapidly at its present orbital location. A liquid water layer on Enceladus is a possible source for the plume in the south polar region assuming the survivability of such a layer to the present. These results could place Enceladus in a category similar to the large satellites of Jupiter, with the core having a rock-metal composition similar to Io, and with a deep overlying ice shell similar to Europa and Ganymede. Indeed, the moment of inertia factor of a differentiated Enceladus, C/MR², could be as small as that of Ganymede, about 0.31.     

On the origin of south polar folds on Enceladus

Recent high-resolution Cassini images of the south polar terrain of Enceladus reveal regions of short-wavelength deformation, inferred to be compressional folds between the Baghdad and Damascus tiger stripes (Spencer, J.R., Barr, A.C., Esposito, L.W., Helfenstein, P., Ingersoll, A.P., Jaumann, R., McKay, C.P., Nimmo, F., Waite, J.H. [2009a]. Enceladus: An active cryovolcanic satellite. In: Saturn after Cassini-Huygens. Springer, New York, pp. 683-722). Here, we use Fourier analysis of the bright/dark variations to show that the folds have a dominant wavelength of 1.1 ± 0.4 km. We use the simple model of lava flow folding from Fink (Fink, J. [1980]. Geology 8, 250-254) to show that the folds could form in an ice shell with an upper high-viscosity boundary layer of thickness <400 m, with a driving stress of 40-80 kPa, and strain rate between 10⁻¹⁴ s⁻¹ and 10⁻¹² s⁻¹. Such deformation rates imply resurfacing of the SPT in 0.05-5 Myr, consistent with its estimated surface age. Measurements of fold topography and more sophisticated numerical modeling can narrow down the conditions of fold formation and provide valuable constraints on the thermal structure of the ice shell on Enceladus.     

Dynamics of two satellites in the 2/1 Mean–Motion resonance: application to the case of Enceladus and Dione

The dynamics of a pair of satellites similar to Enceladus–Dione is investigated with a two-degrees-of-freedom model written in the domain of the planar general three-body problem. Using surfaces of section and spectral analysis methods, we study the phase space of the system in terms of several parameters, including the most recent data. A detailed study of the main possible regimes of motion is presented, and in particular we show that, besides the two separated resonances, the phase space is replete of secondary resonances.     

塔里木和中亚造山带西段二叠纪大火成岩省的两类地幔源区

对塔里木和中亚造山带西段二叠纪玄武质岩石地质、年龄、元素地球化学、同位素组成的系统总结表明,二叠纪火成岩在分布面积、岩石类型(以玄武岩占绝对优势)、活动时间(以275Ma左右为峰期)等方面均与世界典型的大火成岩省一致,将其命名为巴楚大火成岩省(Bachu LIP)。元素和同位素地球化学特征表明,塔里木玄武岩来自长期富集的岩石圈地幔,来源深度为60~80km。塔里木基性岩墙和超镁铁-镁铁杂岩的原始岩浆可能来自软流圈地幔(OIB)部分熔融。中亚造山带西段的玄武岩、基性岩墙和超镁铁-镁铁杂岩主要来自被俯冲带熔体交代的强烈亏损的岩石圈地幔,其中部分地区可能有软流圈物质的加入,如东天山和阿勒泰南缘高Ti系列的玄武质岩石。根据元素和同位素地球化学资料,将巴楚大火成岩省分为2个地幔省(mantle domain),即塔里木省和中亚省。这2个不同地幔省的成矿系列也有显著的差异,塔里木省为钒-钛磁铁矿矿床,而中亚则以铜-镍-(铂族金属)硫化物矿床为主,成矿作用的差异和岩浆地幔源区的差异是完全对应的。综合地质、地球化学和成矿作用,认为巴楚大火成岩省的形成和二叠纪地幔柱密切相关。     

Intraplate geodynamics and magmatism in the evolution of the Central Asian Orogenic Belt

The Central Asian Orogenic Belt (CAOB) was produced as a consequence of the successive closure of the Paleoasian Ocean and the accretion of structures formed within it (island arcs, oceanic islands, and backarc basins) to the Siberian continent. The belt started developing in the latest Late Neoproterozoic, and this process terminated in the latest Permian in response to the collision of the Siberian and North China continents that resulted in closure of the Paleoasian ocean (Metcalfe, 2006; Li et al., 2014; Liu et al., 2009; Xiao et al., 2010; Didenko et al., 2010). Throughout the whole evolutionary history of this Orogenic Belt, a leading role in its evolution was played by convergent processes. Along with these processes, an important contribution to the evolution of the composition and structure of the crust in the belt was made by deep geodynamic processes related to the activity of mantle plumes.Indicator complexes of the activity of mantle plumes are identified, and their major distribution patterns in CAOB structures are determined. A number of epochs and areas of intraplate magmatism are distinguished, including the Neoproterozoic one (Rodinia breakup and the origin of alkaline rock belt in the marginal part of the Siberian craton); Neoproterozoic–Early Cambrian (origin of oceanic islands in the Paleoasian Ocean); Late Cambrian–Early Ordovician (origin of LIP within the region of Early Caledonian structures in CAOB); Middle Paleozoic (origin of LIP in the Altai–Sayan rift system); Late Paleozoic–Early Mesozoic (origin of the Tarim flood-basalt province, Central Asian rift system, and a number of related zonal magmatic areas); Late Mesozoic–Cenozoic (origin of continental volcanic areas in Central Asia).Geochemical and isotopic characteristics are determined for magmatic complexes that are indicator complexes for areas of intraplate magmatism of various age, and their major evolutionary trends are discussed. Available data indicate that mantle plumes practically did not cease to affect crustal growth and transformations in CAOB in relation to the migration of the Siberian continent throughout the whole time span when the belt was formed above a cluster of hotspots, which is compared with the African superplume.     

超级喷发(超级侵入)后成矿作用

本文仿照超级喷发的概念定义了超级侵入,并将超级火山对应于大型岩基.文章聚焦于这样一个科学问题:为什么大规模成矿作用发生在紧接着超级喷发和超级侵入之后？为此,首先探讨了峨嵋山地幔柱系统的活动规律.尽管少数学者对玄武质岩浆大规模喷出之前的千米级地壳隆升提出了质疑,峨嵋山火山岩系第一旋回底部玄武岩直接覆盖在喀斯特之上的新观察支持千米级隆升的认识.这表明,峨嵋山地幔柱快速上涌之初期,岩石圈子系统在相当长一段时间没有作出伸展响应,尽管局部已经发生了地壳岩石的部分熔融.因此,岩浆通道形成之后,首先喷出了巨厚层玄武岩,并且后者裹挟了部分长英质岩浆.此后,岩浆喷发的规模振荡性减小,直至消失和地表沉降.斜长石巨斑玄武岩和苦橄岩中橄榄石斑晶与基质间的不平衡表明这些晶体属于循环晶,暗示岩浆曾经在深部岩浆房滞留了相当长的时间,这将导致岩石圈受热膨胀和再次隆升以及岩浆的冻结.因此,下一阶段岩浆活动的开始要求有一个冻结岩浆房的活化机制.依据野外地质学和岩相学观察,文章详细描述了流体活化机制,并强调了提出这种机制的必要性.虽然多数作者偏好升温活化机制,流体活化机制对长英质和镁铁质岩浆成矿系统都是必需的.进而,结合地幔名义无水矿物的H₂O丰度及其对岩浆产生过程的贡献,提出岩浆产量与减压速率正相关而与流体产量反相关的观点.尽管水流体可以有效降低地幔橄榄岩的固相线温度从而有可能提高岩浆产量,新生代玄武岩中橄榄岩包体依然含有未分解的角闪石和云母且名义无水矿物依然含有较多的H₂O,表明快速减压条件下含水暗色矿物的分解反应和名义无水矿物的脱水作用都是低效的.将这种认识与峨嵋山地幔柱系统的振荡性运动结合在一起,结合成矿作用的基本解是成矿金属从流体中析出的认识,可以得出超大型矿床必然形成于超级喷发和超级侵入之后.攀枝花式铁矿的观察表明,两类代表性矿床都具有铁矿浆侵位发生在成矿系统演化最后阶段的特点.因此得出结论:超大型矿床的形成取决于岩浆通道向流体通道的转换.如果岩浆通道在尚未完全封闭之前被含矿流体所利用,大规模流体快速上升将产生超大型矿床.含矿流体透过残留于通道中的熔体上升,不仅冲刷通道中的残留熔体并使其聚集在火山岩系之下或侵位于其下部形成含矿小岩体,而且持续注入于小岩浆体中的含矿流体可以导致岩浆强烈分异形成层状岩体.当通道中残留熔体被消耗殆尽,沿着通道上升的只有含矿流体.这些含矿流体充填在自生长裂隙中并强烈排气,最终可形成矿浆型富矿体.考虑到通道的规模与关闭速率的关系,推测超级喷发/侵入发生时的岩浆主通道更容易转换为含矿流体通道,因而是圈定找矿靶区的首选目标.该模型似乎与观察结果相吻合,并可与岩浆成矿系统的复杂性、小岩体成大矿理论、透岩浆流体成矿理论和通道成矿假说有机地结合在一起,较合理解释了超级喷发/侵入后成矿作用的地球动力学背景和成矿过程.由于长英质和镁铁质岩浆系统中均可见岩基,我们建议将这类成矿作用统称为岩基后成矿作用.     

新元古代地幔柱事件在Rodinia超大陆西缘的响应:来自马达加斯加的初步证据

对于Rodinia超大陆西缘在裂解过程中是否发育巨长安第斯型陆弧存在较大争议.马达加斯加即位于古地理再造Rodinia的西缘位置,其太古宙结晶基底中出露有大量新元古代侵入体,是澄清这一争议的理想研究区.由于基性岩浆岩组分识别不足等原因,前人曾认为这些侵入岩形成于俯冲带陆弧环境.但笔者在中北部Alaotra湖地区野外考察期间发现了大量辉长质岩石,对其中典型岩体的LA-ICP-MS锆石U-Pb测年表明其结晶于798~778Ma之间(最大误差估计).因此,这些辉长岩体事实上与岛内其他新元古代侵入体构成了双峰式侵入岩套,暗示了可能的陆内伸展环境.在此基础上,笔者重新审视了前人已发表的地球化学数据,发现该双峰式侵入岩套的基性组分显示富钾特征和拉斑演化趋势,局部甚至发育了强烈地钒钛磁铁矿化;酸性组分则显示富铁、偏铝-过铝质和碱钙-钙碱性特征,并具有相对较高的K₂O/Na₂O和Ga/Al比值以及高场强元素含量,属于A型花岗岩(铁质花岗岩).这些特征进一步表明该双峰式侵入岩套形成于陆内伸展环境而非陆弧环境.结合本文的初步研究结果和区域地质演化历史,笔者认为马达加斯加这一双峰式侵入岩套很可能是新元古代地幔柱事件在Rodinia超大陆西缘的响应.     

区域土地利用影响地表CO2浓度异质性特征的动力学机制

本文综合应用高斯方程和拉姆齐模型,针对京津冀地区2000年以来10 km×10 km栅格尺度的地表CO₂浓度开展研究,分析了区域土地利用影响地表CO₂浓度异质性特征的动力学机制。研究发现：① 地表CO₂浓度与土地利用类型密切相关。2000—2018年京津冀地区CO₂浓度的高值区主要集中于经济较发达的快速城镇化地区;② 土地利用强度及土地利用效率上的时空分异为地表CO₂扩散提供了潜在的势能。京津冀地区地表CO₂排放及扩散存在明显的空间异质性,距离CO₂排放高值区越近,其相应的CO₂浓度越高并随时间推移及空间拓展呈逐步减小的态势;③ 京津冀地区在土地利用结构调整、格局优化及效率提升后,CO₂排放强度增幅明显减弱,其区域间的增幅差异也逐渐缩小。产业转型发展、土地利用格局优化、土地利用效率提高有效地抑制了京津冀地区地表CO₂排放强度的提升并促进了该区域的内涵式增长与高质量发展。     

川南早三叠世砂页岩型铜矿床沉积环境、成矿模式及对峨眉山地幔柱成矿系统的补充

峨眉山地幔柱一直以来是国内外学者的研究热点之一,近年来对峨眉山地幔柱的成矿效应的关注度持续升高,但对提供成矿物源的矿床类型研究较少,特别是对砂页岩型铜矿的研究极少,砂页岩型铜矿稳定分布在沐川西部及西南部的飞仙关组底部,以往开展了大量的勘查工作,取得了较好的找矿成果,但其成矿物质来源还有较大争议。为厘清沐川地区飞仙关组底部砂页岩型铜矿床的富集规律、沉积环境和成因机制,本研究开展了野外实地调查、矿物学、岩相古地理与岩石地球化学等系统性研究,探讨其物源、富集规律、沉积环境,建立了成矿模式。研究结果表明,沐川地区砂页岩型铜矿体产出于早三叠世飞仙关组底部的一套灰绿色细碎屑岩中,主要矿石类型有粉砂质条带黏土岩型铜矿、泥质条带粉砂岩型铜矿、粉砂岩型铜矿和细砂岩型铜矿,矿石矿物以黄铜矿、斑铜矿、辉铜矿为主;沐川地区飞仙关组底部的沉积相属于有障壁型海岸相潮坪亚相,可识别出潮上泥坪微相、潮间混合坪微相、潮下砂坪微相和潮渠微相4种微相,Cu元素主要富集于粉砂质条带黏土岩和泥质条带粉砂岩等水动力条件较弱的潮间混合坪微相中,铜的富集严格受岩相古地理及沉积相的控制; Cu元素主要来源于峨眉山高钛玄武岩,西部的康滇古陆是主要的物源区;沐川地区飞仙关组底部砂页岩型铜矿属同生沉积型矿床,其成矿模式可分为峨眉山玄武岩喷溢（矿源层形成）阶段、风化剥蚀搬运阶段、沉积富集阶段和成岩保存阶段。上述成果,对西南地区进一步实现战略性矿产找矿突破和补充完善峨眉山地幔柱成矿系统具有重要意义。     

The Permian mafic intrusive events in the northwestern margin of the Tarim Basin and their tectonic significanceSCIEI北大核心CSCD

塔里木大火成岩省是我国境内发现的两个重要的二叠纪大火成省之一,不仅有大规模的溢流相玄武岩喷发,还有复杂多样的侵入岩及其组合。以往的研究主要集中在二叠系等显生宙地层发育区,对于前寒武系等古老层系中是否存在二叠纪岩浆侵入未引起重视。本文通过野外地质调查,在阿克苏地区前寒武系中识别出数条侵入南华系的基性岩墙和较大规模侵入震旦系的基性岩床。岩墙、岩床与围岩之间均显示出典型的侵入接触关系,包括岩体内部结晶粗、边部结晶细的淬冷边结构、岩床顶底面显著的切层现象以及包裹围岩团块等;显微镜下观察表明,辉绿岩具有典型的辉绿结构和嵌晶含长结构。锆石U-Pb年代学结果表明,侵入下震旦统的辉绿岩岩床和侵入南华系的辉绿岩岩墙的侵位时代在误差范围内基本一致,约为290Ma。岩石地球化学特征表明,辉绿岩岩床具有与洋岛玄武岩(OIB)相似的稀土及微量元素配分模式,结合Sr-Nb-Pb同位素测试结果,认为它们来源于碳酸盐化的富集型岩石圈地幔部分熔融,而辉绿岩岩墙具有Nb、Ta、Zr、Hf等负异常的地球化学特征,可能来自曾被俯冲相关流体/熔体交代的岩石圈地幔源区。本文的早二叠世辉绿岩岩床和岩墙的形成时代、岩浆源区和岩浆演化...