Degree-one convection and the origin of Enceladus' dichotomy     

M. Grott  F. Sohl 《Icarus》2007,191(1):203-210

Recently, the Cassini spacecraft has detected ongoing geologic activity near the south pole of Saturn's moon Enceladus. In contrast, the satellite's north-polar region is heavily cratered and appears to have been geologically inactive for a long time. We propose that this hemispheric dichotomy is caused by interior dynamics with degree-one convection driving the south-polar activity. We investigate a number of core sizes and internal heating rates for which degree-one convection occurs. The numerical simulations imply that a core radius of less than 100±20 km and an energy input at a rate of 3.0 to 5.5 GW would be required for degree-one convection to prevail. This is within the range of the observed thermal power release near Enceladus' south pole. Provided that Enceladus is not fully differentiated, degree-one convection is found to be a viable mechanism to explain Enceladus' hemispheric dichotomy.  相似文献   

Iapetus' geophysics: Rotation rate, shape, and equatorial ridge   总被引：1，自引：0，他引：1  

J.C. Castillo-Rogez  D.L. Matson  T.V. Johnson  P.C. Thomas 《Icarus》2007,190(1):179-202

Iapetus has preserved evidence that constrains the modeling of its geophysical history from the time of its accretion until now. The evidence is (a) its present 79.33-day rotation or spin rate, (b) its shape that corresponds to the equilibrium figure for a hydrostatic body rotating with a period of ∼16 h, and (c) its high, equatorial ridge, which is unique in the Solar System. This paper reports the results of an investigation into the coupling between Iapetus' thermal and orbital evolution for a wide range of conditions including the spatial distributions with time of composition, porosity, short-lived radioactive isotopes (SLRI), and temperature. The thermal model uses conductive heat transfer with temperature-dependent conductivity. Only models with a thick lithosphere and an interior viscosity in the range of about the water ice melting point can explain the observed shape. Short-lived radioactive isotopes provide the heat needed to decrease porosity in Iapetus' early history. This increases thermal conductivity and allows the development of the strong lithosphere that is required to preserve the 16-h rotational shape and the high vertical relief of the topography. Long-lived radioactive isotopes and SLRI raise internal temperatures high enough that significant tidal dissipation can start, and despin Iapetus to synchronous rotation. This occurred several hundred million years after Iapetus formed. The models also constrain the time when Iapetus formed because the successful models are critically dependent upon having just the right amount of heat added by SLRI decay in this early period. The amount of heat available from short-lived radioactivity is not a free parameter but is fixed by the time when Iapetus accreted, by the canonical concentration of ²⁶Al, and, to a lesser extent, by the concentration of ⁶⁰Fe. The needed amount of heat is available only if Iapetus accreted between 2.5 and 5.0 Myr after the formation of the calcium aluminum inclusions as found in meteorites. Models with these features allow us to explain Iapetus' present synchronous rotation, its fossil 16-h shape, and the context within which the equatorial ridge arose.  相似文献   

Optimal dynamos in the cores of terrestrial exoplanets: Magnetic field generation and detectability     

Peter Driscoll  Peter Olson 《Icarus》2011,213(1):12-23

A potentially promising way to gain knowledge about the internal dynamics of extrasolar planets is by remote measurement of an intrinsic magnetic field. Strong planetary magnetic fields, maintained by internal dynamo action in an electrically conducting fluid layer, are helpful for shielding the upper atmosphere from stellar wind induced mass loss and retaining water over long (Gyr) time scales. Here we present a whole planet dynamo model that consists of three main components: an internal structure model with composition and layers similar to the Earth, an optimal mantle convection model that is designed to maximize the heat flow available to drive convective dynamo action in the core, and a scaling law to estimate the magnetic field intensity at the surface of a terrestrial exoplanet. We find that the magnetic field intensity at the core surface can be up to twice the present-day geomagnetic field intensity, while the magnetic moment varies by a factor of 20 over the models considered. Assuming electron cyclotron emission is produced from the interaction between the stellar wind and the exoplanet magnetic field we estimate the cyclotron frequencies around the ionospheric cutoff at 10 MHz with emission fluxes in the range 10⁻⁴-10⁻⁷ Jy, below the current detection threshold of radio telescopes. However, we propose that anomalous boosts and modulations to the magnetic field intensity and cyclotron emission may allow for their detection in the future.  相似文献   

Stability of methane clathrate hydrates under pressure: Influence on outgassing processes of methane on Titan     

Mathieu Choukroun  Olivier Grasset 《Icarus》2010,205(2):581-10437

We have conducted high-pressure experiments in the H₂O-CH₄ and H₂O-CH₄-NH₃ systems in order to investigate the stability of methane clathrate hydrates, with an optical sapphire-anvil cell coupled to a Raman spectrometer for sample characterization. The results obtained confirm that three factors determine the stability of methane clathrate hydrates: (1) the bulk methane content of the samples; (2) the presence of additional gas compounds such as nitrogen; (3) the concentration of ammonia in the aqueous solution. We show that ammonia has a strong effect on the stability of methane clathrates. For example, a 10 wt.% NH₃ solution decreases the dissociation temperature of methane clathrates by 14-25 K at pressures above 5 MPa. Then, we apply these new results to Titan’s conditions. Dissociation of methane clathrate hydrates and subsequent outgassing can only occur in Titan’s icy crust, in presence of locally large amounts of ammonia and in a warm context. We propose a model of cryomagma chamber within the crust that provides the required conditions for methane outgassing: emplacement of an ice plume triggers the melting (if solid) or heating (if liquid) of large ammonia-water pockets trapped at shallow depth, and the generated cryomagmas dissociate surrounding methane clathrate hydrates. We show that this model may allow for the outgassing of significant amounts of methane, which would be sufficient to maintain the presence of methane in Titan’s atmosphere for several tens of thousands of years after a large cryovolcanic event.  相似文献   

Temporal stability of apparent soil electrical conductivity measured by electromagnetic induction techniques     

LIAO Kai-hua  ZHU Qing  James DOOLITTLE 《山地科学学报》2014,11(1):98-109

Assessing and managing the spatial variability of hydropedological properties are important in environmental,agricultural,and geological sciences.The spatial variability of soil apparent electrical conductivity（ECa） measured by electromagnetic induction（EMI） techniques has been widely used to infer the spatial variability of hydrological and pedological properties.In this study,temporal stability analysis was conducted for measuring repeatedly soil ECa in an agricultural landscape in 2008.Such temporal stability was statistically compared with the soil moisture,terrain indices（slope,topographic wetness index（TWI）,and profile curvature）,and soil properties（particle size distribution,depth to bedrock,Mn mottle content,and soil type）.Locations with great and temporally unstable soil ECa were also associated with great and unstable soil moisture,respectively.Soil ECa were greater and more unstable in the areas with great TWI（TWI 〉 8）,gentle and concave slope（slope 〈 3%; profile curvature 〉 0.2）.Soil ECa exponentially increased with depth to bedrock,and soil profile silt and Mn mottle contents（R2= 0.57）,quadratically（R2 = 0.47）,and linearly（R 2 = 0.47）,respectively.Soil ECa was greater and more unstable in Gleysol and Nitosol soils,which were distributed in areas with low elevation（〈 380 m）,thick soil solum（〉 3 m）,and fluctuated water table（shallow in winter and spring but deep in summer and fall）.In contrast,Acrisol,Luvisol,and Cambisol soils,which are distributed in the upper slope areas,had lower and more stable soil ECa.Through these observations,we concluded that the temporal stability of soil ECa can be used to interpret the spatial and temporal variability of these hydropedological properties.  相似文献   

A lithological assessment of the resistivity data acquired during the airborne geophysical survey of Anglesey,North Wales     

James C. White  David Beamish 《Proceedings of the Geologists' Association. Geologists' Association》2014

A recent airborne geophysical survey has provided high resolution estimates of the electrical resistivity of the near-surface and deeper (bedrock) formations found across Anglesey and a portion of the coastal area of North Wales. This single small survey provides new geophysical information on both the complex configuration of the Neoproterozoic and Cambrian bedrock units and the shallow near-surface geology and glacial features.  相似文献   

A geophysical view of the Southeastern Brazilian margin at Santos Basin: Insights into rifting evolution     

《Journal of South American Earth Sciences》2014

This study investigates the rifting structures of Santos Basin at the Southeastern Brazilian margin, based on an integrated geophysical approach. Our aim is to constrain the crustal basement topography of central and northern Santos basin, the presence of magmatism and the role of inherited structures in space and time through the rifting processes. We present a new high resolution aeromagnetic dataset, which in correlation with gravity anomalies enables us to interpret the tectonic trends and crustal basement structures. We calculated the magnetic basement depth for the central and northern Santos Basin using power spectrum analysis. The obtained depths range between 2 and 9 kms, and are comparable with results from previous works. From our integrated study, three margin domains could be identified, which display distinct rifting structures and are characterized by important lateral variation along the margin. The proximal domain displays trends and magnetic basement blocks NE–SW oriented, i.e., parallel to inherited onshore crustal basement with an inflexion to E–W oriented trends; the necking domain is characterized by oblique magnetic basement highs and lows (E–W and NW–SE) and a structural trend change. The trends and magnetic basement highs are bounded by NW–SE negative anomalies, interpreted as transfer zones. Oceanwards at the distal domain, the lineaments and transfer zones show a progressive structural inflexion to ENE and E–W, sub-parallel to adjacent South Atlantic Fracture Zones. The observed crustal basement architecture and segmentation suggest the reactivation of pre-rift structures at the proximal margin and the obliquity of rifting relative to them. From the proximal domain oceanwards the structural pattern may reflect the passage from a “continental type” domain, where lithospheric inheritance controls the deformation, to a distal margin where this influence diminishes and “new” structural trends are formed. We propose that northern Santos Basin show evidences of an intensely deformed zone, where rift evolved under oblique extension, similar to that observed at transform margin segments.  相似文献   

Layering stratigraphy of eastern Coprates and northern Capri Chasmata, Mars     

Ross A. Beyer  Alfred S. McEwen 《Icarus》2005,179(1):1-23

Distinct competent layers are observed in the slopes of eastern Coprates Chasma, part of the Valles Marineris system on Mars. Our observations indicate that the stratigraphy of Coprates Chasma consists of alternating thin strong layers and thicker sequences of relatively weak layers. The strong, competent layers maintain steeper slopes and play a major role in controlling the overall shape and geomorphology of the chasmata slopes. The topmost competent layer in this area is well preserved and easy to identify in outcrops on the northern rim of Coprates Chasma less than 100 m below the southern Ophir Planum surface. The volume of the topmost emplaced layer is at least 70 km³ and may be greater than 2100 km³ if the unit underlies most of Ophir Planum. The broad extent of this layer allows us to measure elevation offsets within the north rim of the chasma and in a freestanding massif within Coprates Chasma where the layer is also observed. Rim outcrop morphology and elevation differences between Ophir and Aurorae Plana may be indicative of the easternmost extent of the topmost competent layer. These observations allow an insight into the depositional processes that formed the stratigraphic stack into which this portion of the Valles Marineris is carved, and they present a picture of some of the last volcanic activity in this area. Furthermore, the elevation offsets within the layer are evidence of significant subsidence of the massif and surrounding material.  相似文献   

阿尔泰南缘地球物理场特征与矿床分布规律     

王隆平  温佩琳 《地球科学与环境学报》2001,23(3):46-49

通过对新疆阿尔泰南缘地球物理场特征-深部构造-已知大型矿床分布规律的系统研究,认为该地区不同属性的地质块体受3组基底构造控制,即EW向、NE向和NW向3组基底构造系,并认为该地区已知大型-超大型矿床同样受这3组深部构造系的控制.最后对阿尔泰地区进行了大型、超大型多金属矿床成矿预测.  相似文献   

中国蛇绿岩清理——兼论蛇绿岩研究的新思路     

张旗  任纪舜  赵磊  焦守涛  王跃  王振 《地质论评》2022,68(2):2022030013-2022030013

中国蛇绿岩研究取得了很大的成绩,也存在许多问题。文中简要评述了日喀则、三江、青海、北秦岭、中亚造山带、东北以及中国南方蛇绿岩的若干问题,指出中国划归入蛇绿岩的地质体（组合）太多了,把许多可能不是蛇绿岩的地质体（组合）也当成了蛇绿岩。当前需要做的是去伪存真,对中国蛇绿岩进行一次认真的清理。文中指出,地幔橄榄岩无疑是蛇绿岩最重要的成员,它来自洋壳下。世界上还有另一类来自陆壳下的地幔岩,被称为“造山橄榄岩”。因此,地幔橄榄岩并非蛇绿岩所独有。此外,有越来越多的数据表明,在许多不同的构造背景下都可以出现类似MORB（大洋中脊玄武岩）地球化学性质的玄武岩,例如洋岛、岛弧、大陆溢流玄武岩、板内玄武岩以及太古宙（拉斑玄武岩和科马提岩）等。因此,不能简单地认为一个地区只要有了地幔橄榄岩和MORB就是蛇绿岩了。文中回顾了蛇绿岩研究的两个发展阶段：前一个阶段以1972年的彭罗斯会议为标志,开启了蛇绿岩研究的新篇章,当时的学术界主要关注蛇绿岩的岩石学和地球化学问题,关心蛇绿岩的岩石组合。新的阶段是从20世纪后期逐渐发展起来的,于近期取得了突出的进展。笔者等强调指出,蛇绿岩（野外出露更多的是蛇绿混杂岩）即蛇绿岩套,它不仅包括一个特定的岩石组合,还包括深海沉积。文中肯定了中外学术界在蛇绿岩构造研究方面获得的许多新发现、新思路和新进展。此外,大数据和地球物理方法也是非常有意义的。蛇绿岩是一个复杂体系,不确定的问题相当多。它们的解决需要构造地质学家、地层学家、古生物学家、岩石学家、地球化学家、年代学家以及地球物理学家的共同努力。  相似文献