Tracing the 850-Ma continental flood basalts from a piece of subducted continental crust in the North Qaidam UHPM belt,NW China

A Paleozoic ultrahigh-pressure metamorphic (UHPM) belt extends along the northern margin of the Qaidam Basin, North Tibetan Plateau. Eclogites in the Yuka eclogite terrane, northwest part of this UHPM belt, occur as blocks or layers of varying size intercalated with granitic and pelitic gneisses. These eclogites have protoliths geochemically similar to enriched-type mid-ocean ridge basalts (E-MORB) and oceanic island basalts (OIB). On the basis of Ti/Y ratios, they can be divided into low-Ti and high-Ti groups. The low-Ti group (LTG) eclogites exhibit relatively low TiO₂ (most <2.5 wt%) and Ti/Y (<500) but comparatively high Mg# (48–55), whereas the high-Ti group (HTG) eclogites have high TiO₂ (most >2.5 wt%) and Ti/Y (>500) but lower Mg# (46–52). Zircons from two eclogite samples gave a magmatic crystallization (protolith) age of ∼850 Ma and a UHPM age of ∼433 Ma. The occurrence, geochemical features and age data of the Yuka eclogites suggest that their protoliths are segments of continental flood basalts (CFBs) with a mantle plume origin, similar to most typical CFBs. Our observation, together with the tectonic history and regional geologic context, lend support for the large scale onset of mantle plume within the Rodinia supercontinent at ∼850 Ma. The Qaidam block is probably one of the fragments of the Rodinia supercontinent with a volcanic-rifted passive margin. The latter may have been dragged to mantle depths by its subducting leading edge of the oceanic lithosphere in the Early Paleozoic.     

Isotope provinces, mechanisms of generation and sources of the continental crust in the Central Asian mobile belt: geological and isotopic evidence

The available geological, geochronological and isotopic data on the felsic magmatic and related rocks from South Siberia, Transbaikalia and Mongolia are summarized to improve our understanding of the mechanisms and processes of the Phanerozoic crustal growth in the Central Asian mobile belt (CAMB). The following isotope provinces have been recognised: ‘Precambrian’ (T_DM=3.3–2.9 and 2.5–0.9 Ga) at the microcontinental blocks, ‘Caledonian’ (T_DM=1.1–0.55 Ga), ‘Hercynian’ (T_DM=0.8–0.5 Ma) and ‘Indosinian’ (T_DM=0.3 Ga) that coincide with coeval tectonic zones and formed at 570–475, 420–320 and 310–220 Ma. Continental crust of the microcontinents is underlain by, or intermixed with, ‘juvenile’ crust as evidenced by its isotopic heterogeneity. The continental crust of the Caledonian, Hercynian and Indosinian provinces is isotopically homogeneous and was produced from respective juvenile sources with addition of old crustal material in the island arcs or active continental margin environments. The crustal growth in the CAMB had episodic character and important crust-forming events took place in the Phanerozoic. Formation of the CAMB was connected with break up of the Rodinia supercontinent in consequence of creation of the South-Pacific hot superplume. Intraplate magmatism preceding and accompanying permanently other magmatic activity in the CAMB was caused by influence of the long-term South-Pacific plume or the Asian plume damping since the Devonian.     

阿尔金造山带中、新生代的演化

塔里木盆地东缘的阿尔金造山带中、新生代经历了一个复杂的大地构造演化历程:中生代早期(T)为隆升夷平,中生代中后期(J-K)为裂陷沉积阶段;自古新世-中新世因塔里木盆地向东挤压使得阿尔金造山带东南缘出现了右行走滑仰冲,柴达木壳体向阿尔金造山带之下俯冲,阿尔金造山带隆起.塔里木盆地相对柴达木盆地向北移动,最大距离可达400~500 km,使得原来统一的塔里木-敦煌-柴达木联合盆地裂解.由于逆冲走滑使阿尔金造山带内部发育了一系列小型的走滑盆地,形成了复杂的盆地沉积建造,并伴有动力变质及火山作用;中新世末,东西向挤压转变为不对称的南北向力隅作用,使得阿尔金造山带发生构造反转,右行转变为左行,统一的塔里木-敦煌盆地裂解.塔里木盆地向南漂移,距离达400多公里.塔里木盆地的向东俯冲使阿尔金造山带急骤隆起,同样,在阿尔金造山带内部发育了一系列小型盆地,形成了相应的复杂沉积建造.     

利用地质成果优化3010皮带上山设计

3010皮带上 山 建成 后将 担 负着 范各 庄 矿三 水平 、四 水平 的 煤炭 运输 任 务,服务 年 限要 求 至 少 30a。 此 皮 带上山 位于 岩 溶陷 落柱 较 发育 的井 口 区域 ,范 各庄 矿 发现 的 12个 陷落 柱 全部 位于 此 区域 。由 于 陷落 柱直 接 导通 下部 奥 灰水 ,一 旦揭 露 将有 淹没 整 个矿 井的 危 险。为 保 证矿 井安 全 ,在 工程 施工 前 ,利用 地 质手 段对 设 计区 域进 行 了探 查,发现皮 带上 山 的中 上部 发 育有 岩溶 陷 落柱 ,两 次对 设 计进 行了 修 改,为 施 工提 供了 安 全保 障。     

The Relationship between Tectono-metamorphic Evolution and Argon Isotope Records in White Mica: Constraints from in situ 40Ar-39Ar Laser Analysis of the Variscan Basement of Sardinia

The basement of Sardinia represents a nearly complete sectionof a segment of the Variscan belt that experienced a polyphasetectono-metamorphic evolution and Barrovian metamorphism. Thisbasement is well suited to investigate the relationship betweentectono-metamorphic evolution and argon isotope records in whitemica. Micaschists from the garnet zone (maximum T of up to 520–560°C)contain two texturally and chemically resolvable generationsof white mica: (1) deformed celadonite-rich flakes, defininga relict S₁ foliation preserved within the main S₂ foliationor enclosed in rotated albite porphyroblasts; (2) celadonite-poorwhite micas aligned along the main S₂ foliation. The S₁ foliationdeveloped earlier and at a deeper crustal level with respectto that at which the thermal peak was reached. From the staurolitezone (T of up to 590–625°C) to the sillimanite + K-feldsparzone, white mica is nearly uniform in composition (muscovite)and is predominantly aligned along the S₂ foliation or is oflater crystallization. In situ ⁴⁰Ar–³⁹Ar laser analysesof white mica yielded ages of     

Exhumation rates and age of metamorphism in the Sanbagawa belt: new constraints from zircon fission track analysis

Zircon fission track dating and track length analysis in the high‐grade part of the Asemigawa region of the Sanbagawa belt demonstrates a simple cooling history passing through the partial annealing zone at 63.2 ± 5.8 (2 σ) Ma. Combining this age with previous results of phengite and amphibole K–Ar and ⁴⁰Ar/³⁹Ar dating gives a cooling rate of between 6 and 13 °C Myr^?1, which can be converted to a maximum exhumation rate of 0.7 mm year^?1 using the known shape of the P–T path. This is an order of magnitude lower than the early part of the exhumation history. In contrast, zircon fission track analyses in the low‐grade Oboke region show that this area has undergone a complex thermal history probably related to post‐orogenic secondary reheating younger than c. 30 Ma. This event may correlate with the widespread igneous activity in south‐west Japan around 15 Ma. The age of subduction‐related metamorphism in the Oboke area is probably considerably older than the generally accepted range of 77–70 Ma.     

造山带与岩石圈演化动力学研究述评

本文综述指出：深部过程，可能导致放射性元素在地幔或下地壳的某些部位聚结而产生强烈的核反应，致使下地壳加热和上地壳的快速抬升和伸展垮塌，产生地震、火山作用、岩浆作用，形成山脉。通过对来自地球内部的α─粒子辐射监测，有可能对毁灭性地震作出预报。     

东昆仑大干沟火山岩SHRIMP锆石U-Pb测年及其地质意义

东昆仑大干沟以北地区造山后形成的牦牛山组磨拉石建造不整合覆盖于前泥盆系之上,其形成时代对限定柴达木盆地加里东造山作用的结束时间及晚古生代裂解作用的开始时间具有重要意义。应用单颗粒锆石离子探针质谱仪(SHRIMP)方法,对牦牛山组上部火山岩段的样品进行精确的锆石U-Pb测年。结果表明,牦牛山组上段火山岩样品DG01和DG02中的岩浆锆石206Pb/238U平均年龄分别为403.6±5.1Ma和409±3.4Ma。综合前人研究认为,造山后牦牛山组伸展型磨拉石的形成时代为晚志留世-早泥盆世,限定了晚古生代裂解的开始时间,也意味着早古生代加里东造山运动在晚志留世-早泥盆世之前已经结束。     

3. Solar System Formation and Early Evolution: the First 100 Million Years

The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is its relation with the circumstellar disks that are ubiquitous around young low-mass stars today? Is it possible to define a “time zero” (t ₀), the epoch of the formation of the solar system? Is the solar system exceptional or common? This astronomical chapter focuses on the early stages, which determine in large part the subsequent evolution of the proto-solar system. This evolution is logarithmic, being very fast initially, then gradually slowing down. The chapter is thus divided in three parts: (1) The first million years: the stellar era. The dominant phase is the formation of the Sun in a stellar cluster, via accretion of material from a circumstellar disk, itself fed by a progressively vanishing circumstellar envelope. (2) The first 10 million years: the disk era. The dominant phase is the evolution and progressive disappearance of circumstellar disks around evolved young stars; planets will start to form at this stage. Important constraints on the solar nebula and on planet formation are drawn from the most primitive objects in the solar system, i.e., meteorites. (3) The first 100 million years: the “telluric” era. This phase is dominated by terrestrial (rocky) planet formation and differentiation, and the appearance of oceans and atmospheres.     

帕米尔-兴都库什地区地震空间分布特征及应力场特征

本文研究了兴都库什及帕米尔地区地震的空间分布.发现h<70km的地震分布广泛,h≥100km的地震形成-S形的倾斜中源地震带.在71.5°E以西,中源地震带倾向接近正北,倾角随深度变化,在深部接近垂直,且倾角自西向东逐渐变陡,在71.5°E以东,倾向逐渐由东南变为正南. 分析了121个m_b≥5.0地震的机制解.浅源地震机制解的P轴大多位于NS和NNW-SSE方向,且多近水平,反映此区受到NS或NNW-SSE方向挤压.各剖面应力轴分布规律性强,在150km以下,总的趋势是机制解的T轴接近于倾斜的中源地震带的下倾方向,而P轴倾角较小且垂直于倾斜的中源地震带的走向.