The Sequence of Magmatic-Tectonic Events and Orogenic Processes of the Yanshan Belt, North China   总被引：11，自引：0，他引：11  

DENG Jinfu  SU Shangguo  MO Xuanxue  ZHAO Guochun  XIAO Qinghiu  JI Guangyi  QIU Ruizhao  ZHAO Hailing  LUO Zhaohu  WANG Yang  LIU Cui China University of Geosciences  Beijing  and Key Laboratory of Lithospheric Tectonics  Lithoprobe Techniques  Ministry of Education of China 《《地质学报》英文版》2004,78(1):260-266

This paper emphasizes that the interactive constraints of geology and isotopic dating is the best approach to construct the geological event sequence, and has compiled 106 data of reasonable isotopic ages for the igneous rocks of the Yanshan belt. We propose a sequence of mgmatic-tectonic events in the Jurassic-Cretaceous Yanshan orogen of North China. Five orogenic episodes are divided, (1) pre-and initial orogenic episode (Early Jurassic); (2) early orogenic episode (Middle Jurassic); (3) peak orogenic episode (Late Jurassic); (4) late orogenic episode (early Early Cretaceous), and (5) post-orogenic episode. Each episode is a short cycle, all of the orogenic processes construct a longer cycle, and they, in general, followed a counter-clockwise (ccw) PTt path. Finally, it is suggested that the Yanshanian movement was so intensive that the magmatism and tectonic deformation had involved all the lithosphere thickness and the late-Achaean-formed cratonic lithosphere had been significantly reworked.  相似文献   

流体包裹体中微量气体组成及其成矿示踪体系研究新进展   总被引：2，自引：0，他引：2  

孙晓明  王敏  薛婷  孙凯 《地学前缘》2004,11(2):471-478

N2 Ar He体系可用以示踪成矿流体及温泉等与火山有关的水流体的来源 ,当体系中He含量低于检出限 ,N2 Ar He体系不能用时 ,CO2 /CH4 N2 /Ar体系可用于识别成矿流体中岩浆水、建造水和大气降水 ,CO2 CH4 H2 体系可以鉴别成矿流体是否发生过沸腾作用以及沸腾是在开放体系还是封闭体系中形成 ,一般开放体系中沸腾有利于成矿。CO2 CH4 C2 H6体系可用于判别岩浆作用是否直接影响成矿或对成矿流体的贡献 ,从而确定热液矿床的成因。CH4 C2 H6 C3 H8体系可用来示踪一些与干酪根热解有关的成矿流体长距离、大规模迁移过程。C2 H6 C3 H8 C6H6体系可用于判定成矿流体的大地构造环境 ,因岛弧与裂谷环境下C2 H6/C3 H8比值有明显差异。以广东长坑 (Au Ag)和嵩溪 (Ag Sb)矿床为例 ,概述了这些体系各自的应用  相似文献   

Photometric and spectral analysis of the distribution of crystalline and amorphous ices on Enceladus as seen by Cassini     

Sarah F. Newman  B.J. Buratti  R. Jaumann  T. Momary 《Icarus》2008,193(2):397-406

Photometric and spectral analysis of data from the Cassini Visual and Infrared Mapping Spectrometer (VIMS) has yielded significant results regarding the properties and composition of the surface of Saturn's satellite Enceladus. We have obtained spectral cubes of this satellite, containing both spatial and spectral information, with a wavelength distribution in the infrared far more extensive than from any previous observations and at much higher spatial resolution. Using a composite mosaic of the satellite, we map the distribution of crystalline and amorphous ices on the surface of Enceladus according to a “crystallinity factor” and also the depth of the temperature- and structure-dependent 1.65 micron water-ice band. These maps show the surface of Enceladus to be mostly crystalline, with a higher degree of crystallinity at the “tiger-stripe” cracks and a larger amorphous signature between these stripes. These results suggest recent geological activity at the “tiger stripe” cracks and an intriguing atmospheric environment over the south pole where amorphous ice is produced either through intense radiative bombardment, flash-freezing of cryovolcanic liquid, or rapid condensation of water vapor particles on icy microspherules or on the surface of Enceladus.  相似文献   

Textural and mineralogical biosignatures in an unusual microbialite from Death Valley, California     

Susanne Douglas  William Abbey  Randall Mielke  Pamela Conrad  Isik Kanik 《Icarus》2008,193(2):620-636

For in situ astrobiological studies of Mars or other planets, we must employ strategies that will enable us to verify whether our approach and prototype instruments are actually capable of distinguishing life from non-life. This must be done against a background of rigorously conducted scientific characterization of the environment or sample types being considered for measurement by the instruments under development. In this study we show how a combination of mineralogical and textural features can be considered a biosignature in an early Mars analogue environment, Death Valley, California. We propose that it is a combination of features in context of the geologic matrix which allows determination of biogenicity to be made. Polymineralic microbialites (organosedimentary formations constructed by microorganisms) from a spring pool at Badwater, within Death Valley National Park, are composed of alternating biogenic and abiogenic minerals in a distinct triplet sequence related to wet and dry seasons. A microbial community, occurring as a black biofilm, produced paired layers of two different mineral types: manganese oxyhydroxides and calcite. These biogenic layers are separated from the next pair by a gypsum layer and appear to be laid down in the wet season, with the gypsum (a mineral positively identified on Mars) precipitating in the dry part of the year, abiogenically (i.e., not dependent on microbial metabolic activity for its deposition). In addition, textural features (smaller grain size and less geometric morphology) unique to the biogenic vs the abiogenic layers, were consistently observed so that texture served as a biosignature in this environment.  相似文献   

Transfer of mass from Io to Europa and beyond due to cometary impacts     

José Luis Alvarellos  Kevin J. Zahnle  Patrick Hamill 《Icarus》2008,194(2):636-646

We simulate the production and orbital evolution of escaping ejecta due to cometary impacts on Io. The model includes the four Galilean satellites, Amalthea, Thebe, Jupiter's gravitational moments, Saturn and the Sun. Five scenarios are examined: an impact at the apex, the sub-jovian point, the anti-jovian point, the antapex, and at the south pole of Io. We estimate that on average a cometary impact injects thrice its mass (in the form of Io surface material) into jovicentric orbit. The majority of the escaping debris comes back to Io, but a sizeable fraction (between 5.0 and 8.7%) manages to reach Europa, and a smaller fraction Ganymede (between 1.5 and 4.6%). Smaller fractions reached Amalthea Thebe, Callisto, and Jupiter itself. For million year time scales, the mass transfer to Europa is estimated as 1.8-3.1×¹⁰¹⁴ g/Myr. The median time for transfer of ejecta from Io to Europa is ∼56 years.  相似文献   

Higher-order neighbor analysis of the Tartarus Colles cone groups, Mars: The application of geographical indices to the understanding of cone pattern evolution     

Mark A. Bishop 《Icarus》2008,197(1):73-83

Cone fields of ambivalent origin exist in the Elysium, Amazonis, Cerberus, Isidis, Acidalia and Cydonia regions of Mars. Considerable interest exists in regard to their location and origin as their occurrence in many instances, is most likely associated with near surface ground ice; the presence of which has consequences for past and present climate, astrobiological activity, and future exploration. This research has outlined an understanding of both spatial and geomorphic processes of cone development for a region within the Tartarus Colles, Mars, as well as the manner in which spatial statistical indices can be affected by modification to the areal unit of study. This study found that cone groups for the region of the Tartarus Colles, are completely spatially random (CSR) across all distances extending to their sixth-order neighbor. However, significant statistical indices of aggregation were found for groups where post-emplacement erosional modification may have occurred by solifluction-like mechanisms or magmatic incursion into or over frozen ground. Such circumstances imply that R-indices reflect both the underlying spatial and geologic processes of cone formation, and also, an overprint of erosional modification of the cone-field within a glacial or periglacial setting, in this instance. The comparison of spatial indices can therefore offer a viewpoint from which geomorphic change can be recognized and quantitatively evaluated for cone fields.  相似文献   

Geomorphological evidence of water level changes in Nepenthes Mensae, Mars     

Miguel Ángel de Pablo  Andrea Pacifici 《Icarus》2008,196(2):667-671

In the western sector of Nepenthes Mensae, Mars, there are some geomorphological features that could be related to a standing water sheet in the area, such as fluvial terraces, deltas and shorelines. A detailed analysis of these features reveals two variations in water level, probably related to tectonic processes, as suggested by the existence of a fissural volcano at this site.  相似文献   

Mojave Mars simulant—Characterization of a new geologic Mars analog     

Gregory H. Peters  Gregory H. Bearman  J. Anthony Smith  Susanne Douglas 《Icarus》2008,197(2):470-479

We have identified and characterized a basaltic Mars simulant that is available as whole rocks, sand and dust. The source rock for the simulant is a basalt mined from the Tertiary Tropico Group in the western Mojave Desert. The Mojave Mars Simulant (MMS) was chosen for its inert hygroscopic characteristics, its availability in a variety of forms, and its physical and chemical characteristics. The MMS dust and MMS sand are produced by mechanically crushing basaltic boulders. This is a process that more closely resembles the weathering/comminution processes on Mars where impact events and aerodynamic interactions provide comminution in the (relative) absence of water and organics. MMS is among the suite of test rocks and soils that was used in the development of the 2007/8 Phoenix Scout and is being used in the 2009 Mars Science Laboratory (MSL) missions. The MMS development team is using the simulant for research that centers on sampling tool interactions in icy soils. Herein we describe the physical properties and chemical composition of this new Mars simulant.  相似文献   

Frosted granular flow: A new hypothesis for mass wasting in martian gullies     

Chris H. Hugenholtz 《Icarus》2008,197(1):65-72

Recent gully deposits on Mars have been attributed to both wet and dry mass wasting processes. In this paper frosted granular flow (FGF) is presented as a new hypothesis for recent mass wasting activity in martian gullies. FGF is a rare type of granular flow observed on a talus slope in the Province of Québec, Canada [Hétu, B., van Steijn, H., Vandelac, P., 1994. Géogr. Phys. Quat. 48, 3-22]. Frost reduces dynamic inter-particle friction, enabling flows to mobilize onto relatively low slope gradients (25-30°) compared to those involving dry granular flow of the same material (35-41°). Resulting erosional and depositional features include straight to sinuous channels, levees and digitate to branching arrangements of terminal deposits. Similar features are commonly found in association with geologically-young gully systems on Mars. Based on terrestrial observations of FGF processes the minimum criteria required for their occurrence on Mars include: (i) readily mobilized, unconsolidated sediment at the surface; (ii) an upper slope gradient at or near the angle of repose; (iii) frost accumulation at the surface; and (iv) triggering by rock fall. All four conditions appear to be met in many areas on present-day Mars though triggering mechanisms may vary. Compared to terrestrial FGFs, which are lubricated by thin liquid films at inter-particle contacts, those occurring on Mars are more likely lubricated by vaporization of CO₂ and small amounts of H₂O frost that becomes incorporated in the translating mass. Some recent mass wasting activity in martian gullies, therefore, could be interpreted as the product of FGF.  相似文献   

Experimental study on the impact fragmentation of core-mantle bodies: Implications for collisional disruption of rocky planetesimals with sintered core covered with porous mantle     

Chisato Okamoto  Masahiko Arakawa 《Icarus》2008,197(2):627-637

Impact experiments of inhomogeneous targets such as layered bodies consisting of a dense core and porous mantle were conducted to clarify the effect of the layered structure on impact strength. The layered structure of small bodies could be the result of the thermal evolution of planetesimals in the solar nebula. So, the impact disruption of thermally evolved bodies with core-mantle structure is important for the origin of small bodies such as asteroids. We investigated the impact strength of rocky-layered bodies with porous mantle-sintered cores, which could be formed at an initial stage of thermal evolution. Spherical targets composed of soda-lime glass or quartz core and porous gypsum mantle were prepared as an analog of small bodies with a core-mantle structure, and the internal structure was changed. A nylon projectile was impacted at the impact velocity from 1 to 5 km/s. The impact strength of the core-mantle targets decreases with the increase of the core/target mass ratio (RCM) in the specific energy range from 1×¹⁰³ to 4×¹⁰⁴ J/kg. We observed two distinct destruction modes characterized by the damage to the core: one shows a damaged core and fractured mantle, and the other shows an intact core and broken mantle. The former mode was usually observed with increasing RCM, and the boundary condition of the core destruction () was experimentally found to be , where is the specific energy required to disrupt a glass core. From this empirical equation, it might be possible to discuss the destruction conditions of a thermally evolved body with a porous mantle-sintered core structure. We speculate that the impact strength of the body could be significantly reduced with the progress of internal evolution at the initial stage of thermal evolution.  相似文献