Composition of Titan''s surface from Cassini VIMS     

T.B. McCord  G.B. Hansen  B.J. Buratti  R.N. Clark  D.P. Cruikshank  E. D&#x;Aversa  C.A. Griffith  E.K.H. Baines  R.H. Brown  C.M. Dalle Ore  G. Filacchione  V. Formisano  C.A. Hibbitts  R. Jaumann  J.I. Lunine  R.M. Nelson  C. Sotin  the Cassini VIMS Team 《Planetary and Space Science》2006,54(15):1524-1539

Titan's bulk density along with Solar System formation models indicates considerable water as well as silicates as its major constituents. This satellite's dense atmosphere of nitrogen with methane is unique. Deposits or even oceans of organic compounds have been suggested to exist on Titan's solid surface due to UV-induced photochemistry in the atmosphere. Thus, the composition of the surface is a major piece of evidence needed to determine Titan's history. However, studies of the surface are hindered by the thick, absorbing, hazy and in some places cloudy atmosphere. Ground-based telescope investigations of the integral disk of Titan attempted to observe the surface albedo in spectral windows between methane absorptions by calculating and removing the haze effects. Their results were reported to be consistent with water ice on the surface that is contaminated with a small amount of dark material, perhaps organic material like tholin. We analyze here the recent Cassini Mission's visual and infrared mapping spectrometer (VIMS) observations that resolve regions on Titan. VIMS is able to see surface features and shows that there are spectral and therefore likely compositional units. By several methods, spectral albedo estimates within methane absorption windows between 0.75 and 5 μm were obtained for different surface units using VIMS image cubes from the Cassini-Huygens Titan T_a encounter. Of the spots studied, there appears to be two compositional classes present that are associated with the lower albedo and the higher albedo materials, with some variety among the brighter regions. These were compared with spectra of several different candidate materials. Our results show that the spectrum of water ice contaminated with a darker material matches the reflectance of the lower albedo Titan regions if the spectral slope from 2.71 to 2.79 μm in the poorly understood 2.8-μm methane window is ignored. The spectra for brighter regions are not matched by the spectrum of water ice or unoxidized tholin, in pure form or in mixtures with sufficient ice or tholin present to allow the water ice or tholin spectral features to be discerned. We find that the 2.8-μm methane absorption window is complex and seems to consist of two weak subwindows at 2.7 and 2.8 μm that have unknown opacities. A ratio image at these two wavelengths reveals an anomalous region on Titan that has a reflectance unlike any material so far identified, but it is unclear how much the reflectances in these two subwindows pertain to the surface.  相似文献   

青海省大柴旦镇红柳沟金矿床地质特征及其成因     

吴正寿  邓元良  苏生顺 《青海国土经略》2001,(1)

通过对红柳沟金矿床地质特征及围岩蚀变的研究,总结了金矿控矿因素及其富集规律,认为该矿床的成因为动力变质热液型。  相似文献   

Study of floods in West Bengal during September, 2000 using Indian Remote sensing satellite data     

S. K. Bhan  Flood Team 《Journal of the Indian Society of Remote Sensing》2001,29(1-2):1-2

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Cassini/VIMS hyperspectral observations of the HUYGENS landing site on Titan     

S. Rodriguez  S. Le Moulic  C. Sotin  H. Clnet  R.N. Clark  B. Buratti  R.H. Brown  T.B. McCord  P.D. Nicholson  K.H. Baines  the VIMS Science Team 《Planetary and Space Science》2006,54(15):1510-1523

Titan is one of the primary scientific objectives of the NASA–ESA–ASI Cassini–Huygens mission. Scattering by haze particles in Titan's atmosphere and numerous methane absorptions dramatically veil Titan's surface in the visible range, though it can be studied more easily in some narrow infrared windows. The Visual and Infrared Mapping Spectrometer (VIMS) instrument onboard the Cassini spacecraft successfully imaged its surface in the atmospheric windows, taking hyperspectral images in the range 0.4–5.2 μm. On 26 October (TA flyby) and 13 December 2004 (TB flyby), the Cassini–Huygens mission flew over Titan at an altitude lower than 1200 km at closest approach. We report here on the analysis of VIMS images of the Huygens landing site acquired at TA and TB, with a spatial resolution ranging from 16 to14.4 km/pixel. The pure atmospheric backscattering component is corrected by using both an empirical method and a first-order theoretical model. Both approaches provide consistent results. After the removal of scattering, ratio images reveal subtle surface heterogeneities. A particularly contrasted structure appears in ratio images involving the 1.59 and 2.03 μm images north of the Huygens landing site. Although pure water ice cannot be the only component exposed at Titan's surface, this area is consistent with a local enrichment in exposed water ice and seems to be consistent with DISR/Huygens images and spectra interpretations. The images show also a morphological structure that can be interpreted as a 150 km diameter impact crater with a central peak.  相似文献   

贵州五指山背斜纳雍枝铅锌矿地质特征及找矿前景分析     

吴先彪  朱尤清  廖树衡  锁瑞强 《地质与资源》2013,22(6):493-498

纳雍枝铅锌矿床位于五指山背斜北东部,是五指山矿集区的组成部分.区内铅锌矿体产于清虚洞组的白云岩中,自下而上共划分为9个矿体层,属沉积型铅锌矿床.矿石类型为碳酸盐岩型铅锌矿石.五指山地区位于紫云-垭都深大断裂的北东侧,南东侧有安顺-凯里深断裂,这些深断裂是纳雍枝矿床深部物质来源的前提,次一级的构造为矿床的形成提供了矿质流动的通道.五指山背斜Pb、Zn综合异常明显的部位,异常与区内构造较吻合,与矿床(点)展布方向一致.该矿床与典型密西西比河谷铅锌矿床具有较高的可比性.通过对纳雍枝铅锌矿床地质特征的总结及分析,认为五指山地区的找矿前景十分广阔.  相似文献   

The surficial nature of lunar swirls as revealed by the Mini-RF instrument     

C.D. Neish  D.T. Blewett  S.J. Lawrence  B.J. Thomson  The Mini-RF Team 《Icarus》2011,215(1):186-196

Lunar swirls are optically bright, sinuous albedo features found on the Moon. The Mini-RF synthetic aperture radar on the Lunar Reconnaissance Orbiter has provided a comprehensive set of X- and S-Band radar images of these enigmatic features, including the first radar observations of swirls on the farside of the Moon. A few general remarks can be made about the nature of the lunar swirls from this data set. First, the average radar properties of lunar swirls are identical to nearby non-swirl regions, in both total radar backscatter and circular polarization ratio (CPR). This implies that average centimeter-scale roughness and composition within the high-albedo portions of the swirls do not differ appreciably from the surroundings, and that the high optical reflectance of the swirls is related to a very thin surface phenomenon (less than several decimeters thick) not observable with X- or S-Band radar. Secondly, bright swirl material appears to be stratigraphically younger than a newly discovered impact melt flow at Gerasimovich D. This observation indicates that the swirls are capable of forming over timescales less than the age of the crater. The Mini-RF data set also provides clues to the origin of the lunar swirls. In at least one case, the presence of an enhanced crustal magnetic field appears to be responsible for the preservation of a high-albedo ejecta blanket around an otherwise degraded crater, Descartes C. The degree of degradation of Descartes C suggests it should not be optically bright, yet it is. This implies that the enhanced albedo is related to its location within a magnetic anomaly, and hence supports an origin hypothesis that invokes interaction between the solar wind and the magnetic anomaly.  相似文献   

西藏班戈地区雪如岩体的形成环境及成矿意义     

高顺宝  郑有业  谢名臣  张众  闫学欣  武斌  罗俊杰 《地球科学》2011,36(4):729-739

雪如岩体主要由中细粒二长花岗岩、中粗粒斑状二长花岗岩组成,在其与郎山组灰岩接触带附近发育有大量的矽卡岩型铜铁矿床或矿化点.岩石及锆石LA-ICP-MS U-Pb、XRF、ICP-AES等分析显示,雪如岩体富K₂O、SiO₂、LREE及Rb、Ba、Pb、Th等大离子亲石元素,而Nb、Ta、Sr、Ti等高场强元素含量相对较低,稀土元素配分曲线为明显的右倾曲线,具有中等的负Eu异常,属高钾钙碱性-钾玄岩岩石系列和后碰撞花岗岩类,成岩时代分别为79.25±0.97 Ma和79.72±0.51 Ma,形成于早白垩世末-晚白垩世初班公湖-怒江缝合带闭合后、羌塘地体与拉萨地体的后碰撞阶段.综合认为,雪如岩体岩浆源区为下地壳富含流体的石榴石角闪岩相-斜长角闪岩相的镁铁质岩石,是在后碰撞环境下经部分熔融形成的花岗岩类,对班戈地区铜铁多金属成矿非常有利;矽卡岩型铜铁成矿作用发生于80 Ma左右,该认识为区域找矿指明了方向.   相似文献   

Titan's surface from the Cassini RADAR radiometry data during SAR mode     

F. Paganelli  M.A. Janssen  E. Stofan  R.D. Lorenz  R.L. Kirk  C. Elachi  The Cassini Radar Team 《Planetary and Space Science》2008,56(1):100-108

We present initial results on the calibration and interpretation of the high-resolution radiometry data acquired during the Synthetic Aperture Radar (SAR) mode (SAR-radiometry) of the Cassini Radar Mapper during its first five flybys of Saturn's moon Titan.We construct maps of the brightness temperature at the 2-cm wavelength coincident with SAR swath imaging. A preliminary radiometry calibration shows that brightness temperature in these maps varies from 64 to 89 K. Surface features and physical properties derived from the SAR-radiometry maps and SAR imaging are strongly correlated; in general, we find that surface features with high radar reflectivity are associated with radiometrically cold regions, while surface features with low radar reflectivity correlate with radiometrically warm regions. We examined scatterplots of the normalized radar cross-section σ⁰ versus brightness temperature, outlining signatures that characterize various terrains and surface features. The results indicate that volume scattering is important in many areas of Titan's surface, particularly Xanadu, while other areas exhibit complex brightness temperature variations consistent with variable slopes or surface material and compositional properties.  相似文献   

Stratigraphic analysis of the northern polar layered deposits of Mars: Implications for recent climate history     

Sarah M. Milkovich  James W. Head III  The HRSC Co-Investigator Team 《Planetary and Space Science》2008,56(2):266-288

We examine the stratigraphy of the polar layered deposits (PLD) within the north polar cap of Mars to assess its layer continuity, correlations, cyclicity and structure and implications for the recent climate record. PLD sequences characterized using Fourier analysis and curve shape matching algorithms show that layers correlate throughout the upper part of the PLD. We tested for cyclicity and found that the uppermost ∼300 m contain a dominant wavelength layer packet of ∼30 m, interpreted to be a climate signal related to the 51 kyr precession cycle. Directly below this region we document a section of polar layered deposits ∼100 m thick without a dominant periodic signal; this is interpreted to represent a phase of low net accumulation and lag deposits formed during the last ice age, about 0.5-2 Ma ago. We further analyzed layer structure by combining these results with three-dimensional determinations of layer orientation (strike and dip) to assess the internal stratigraphy of the PLD and its implications for polar history. We show that individual layers within the PLD stratigraphy are not horizontal (no dip) but rather show broad variation in elevation with distance. Correlations suggest that the layer strikes and dips broadly follow present cap surface topography. Local variations in layer orientations in the vicinity of the troughs suggest that (1) trough structures were present at the time of layer accumulation and (2) dips may have been influenced by ice flow and/or static ice accumulation in the presence of preexisting troughs. This new information favors models in which the troughs are long-term structures of the PLD rather than (1) recently eroded into the PLD, or (2) very active and laterally migrating around the PLD. Our results strongly support the hypothesis that significant volumes of polar volatiles are mobilized and transported equator-ward during periods of increased obliquity. Our results predict that the upper ∼300 m of the north polar PLD accumulated in the last 500 ka, yielding net accumulation rates of ∼0.06 cm/yr. The presence and albedo of the no periodic signal zone suggest that polar net accumulation rates are very low and that dust rich lag deposits form during periods of sustained high obliquity. Layer sequences in the south polar and equatorial regions are examined and compared to those in the north; rhythmic sequences are observed in both regions but no direct correlations to the dominant signals of the north polar deposits have yet been found. These new techniques and observations provide a paradigm for further analysis of recent polar history (the upper kilometer of the record) and a basis for extending assessments to the lower part of the polar deposits and to other cyclic deposits in the geological record of Mars.  相似文献   

Fluvial channels on Titan: Initial Cassini RADAR observations     

Ralph D. Lorenz  Rosaly M. Lopes  Jonathan I. Lunine  Karl L. Mitchell  Ellen R. Stofan  Melissa Myers  Jani Radebaugh  Stephen D. Wall  the Cassini RADAR Team 《Planetary and Space Science》2008,56(8):1132-1144

Cassini radar images show a variety of fluvial channels on Titan's surface, often several hundreds of kilometers in length. Some (predominantly at low- and mid-latitude) are radar-bright and braided, resembling desert washes where fines have been removed by energetic surface liquid flow, presumably from methane rainstorms. Others (predominantly at high latitudes) are radar-dark and meandering and drain into or connect polar lakes, suggesting slower-moving flow depositing fine-grained sediments. A third type, seen predominantly at mid- and high latitudes, have radar brightness patterns indicating topographic incision, with valley widths of up to 3 km across and depth of several hundred meters. These observations show that fluvial activity occurs at least occasionally at all latitudes, not only at the Huygens landing site, and can produce channels much larger in scale than those observed there. The areas in which channels are prominent so far amount to about 1% of Titan's surface, of which only a fraction is actually occupied by channels. The corresponding global sediment volume inferred is not enough to account for the extensive sand seas. Channels observed so far have a consistent large-scale flow pattern, tending to flow polewards and eastwards.  相似文献