Radar-bright channels on Titan     

A. Le Gall  M.A. Janssen  R.D. Lorenz  the Cassini Radar Team 《Icarus》2010,207(2):948-958

During Cassini’s T44 flyby of Titan (May 28, 2008), the Cassini SAR (synthetic aperture radar) revealed sinuous channels in the Southwest of Xanadu. These channels feature very large radar cross-sections, up to 5 dB, whereas the angle of incidence was relatively high, ∼20°. This backscatter is larger than allowed by the coherent backscatter model considered to explain the unusual reflective and polarization properties of the icy satellites and only a few radar scattering mechanisms can be responsible for such high radar returns. The presence of rounded (icy) pebbles with size larger than the radar wavelength (2.18 cm) is proposed to explain the large radar cross-sections measured in these units. The radar-bright channels are thus interpreted as riverbeds, where debris, likely shaped and transported by fluvial activity, have been deposited. Similar debris were observed in the landing site of the Huygens probe. This work may point the way to an explanation for the enhanced brightness of other fluvial regions of Titan.  相似文献   

Dust aerosols above the south polar cap of Mars as seen by OMEGA     

M. Vincendon  Y. Langevin  F. Poulet  J.-P. Bibring  B. Gondet  D. Jouglet  OMEGA Team 《Icarus》2008,196(2):488-505

The time evolution of atmospheric dust at high southern latitudes on Mars has been determined using observations of the south seasonal cap acquired in the near infrared (1-2.65 μm) by OMEGA/Mars Express in 2005. Observations at different solar zenith angles and one EPF sequence demonstrate that the reflectance in the 2.64 μm saturated absorption band of the surface CO₂ ice is mainly due to the light scattered by aerosols above most places of the seasonal cap. We have mapped the total optical depth of dust aerosols in the near-IR above the south seasonal cap of Mars from mid-spring to early summer with a time resolution ranging from one day to one week and a spatial resolution of a few kilometers. The optical depth above the south perennial cap is determined on a longer time range covering southern spring and summer. A constant set of optical properties of dust aerosols is consistent with OMEGA observations during the analyzed period. Strong variations of the optical depth are observed over small horizontal and temporal scales, corresponding in part to moving dust clouds. The late summer peak in dust opacity observed by Opportunity in 2005 propagated to the south pole contrarily to that observed in mid spring. This may be linked to evidence for dust scavenging by water ice-rich clouds circulating at high southern latitudes at this season.  相似文献   

Gusev photometric variability as seen from orbit by HRSC/Mars-express     

A. Jehl  D. Baratoux  S. Chevrel  N. Manaud  C. Rosemberg  K. Gwinner  H. Hoffman  the HRSC Team 《Icarus》2008,197(2):403-428

Minnaert and two-term phase function Hapke models are used to describe the photometric properties of the martian surface using HRSC (High Resolution Stereo Camera) multi-angular observations acquired along the ongoing Mars-Express mission. These observations can be pieced together to derive integrated phase functions over a wide range of phase angles. The photometric diversity at 675 nm, as seen from orbit, of the martian surface properties across Gusev is depicted with seven units. Three photometric units widespread across the flanks of Apollinaris Patera flank and the floor of Gusev Crater are identified as having high single scattering albedo with rather forward scattering properties, low to intermediate macroscopic roughness and porous or not compacted powdered surface state as indicated by the opposition parameters. Another unit has the highest single scattering albedo, the smoothest surface in terms of macroscopic roughness, associated with an extremely forward scattering behavior. The opposition parameters are consistent with the presence of transparent particles in the surface powder layer. The distribution of this unit appears quite intermittent across the crater and does not seem to indicate any relationship with a given morphological structure. It may correspond to sparse areas where the structure of the surface dust layer is the most preserved. The most pronounced photometric changes are observed in three units associated with the low-albedo features corresponding to dark wind streaks. These units have a low single scattering albedo, are the most backscattering surfaces across Gusev, have a high surface roughness and present variable surface states as shown by the opposition parameters estimates, consistent with the occurrence of large grains organized in more or less packed layers. Clear differences are seen among these units in terms of opposition effect. While one exhibits typical characteristics for the opposition effect, another appears more unusual in terms of lobe width and the third suggests the occurrence of a packed/compressed/narrow size distribution powder surface. The opposition effect thus appears to play a significant role suggesting that the surface state optical properties across Gusev are strongly influenced by the porosity and packing characteristics or grain size distribution of the upper layer of the martian soil. The mapping aspect of the investigation is quite useful to get a better sense of the meaning of the observed photometric variations. Indeed, the Hapke modeling suggests that surface organization (surface roughness, packing state) is more important than the simple physical characterization of the intrinsic optical properties of the constitutive particles. Given the overall spatial patterns derived from the photometric analysis, the variations, at least for the western and central part of Gusev Crater, are likely partly driven by the prevailing wind regimes, considered to be oriented north-northwest/south-southeast and disturbing the very upper surface layer. The present photometric results agree with independent investigations based on thermal inertia, reflectance spectroscopy, in situ photometric and microscopic imaging and support the idea of a thin layer of fine-grained dust, being stripped off in the low albedo units to reveal a dark basaltic substrate comprising coarse-grained materials.  相似文献   

新疆阿合奇县布隆石英重晶石脉型金矿地质特征和硫、氦、氩同位素研究   总被引：8，自引：0，他引：8  

杨富全  王义天  毛景文  杜红星 《地质论评》2004,50(1):87-98

位于新疆西南天山阿合奇县的布隆金矿赋存于上泥盆统细碎屑岩中,金矿体受层间缓倾斜破碎带控制,矿区内发育重晶石脉、石英大脉、石英重晶石脉,但金矿体只产于石英重晶石脉中,为一种比较少见的石英重晶石脉型金矿床。矿石中黄铁矿的 δ~(34)S 值变化于14.6‰～19.2‰,重晶石的 δ~(34)S 值介于35.0‰～39.6‰,反映硫来自于地层。黄铁矿流体包裹体的~3He/~4He 比值为0.24～0.82 R/Ra,趋近于地壳特征值。~(40)Ar/~(36)Ar=338～471,略高于大气氩的同位素组成。~(40)Ar/~4He 比值0.015～0.412,平均为0.153,与地壳~(40)Ar/~4He 比值(0.156)一致。成矿流体的He、Ar 同位素组成特征反映了成矿流体主要来源于地壳。  相似文献   

INDEPTH-Ⅲ地震层析成像--藏北印度岩石圈俯冲断落的证据   总被引：9，自引：2，他引：7  

赵文津  薛光琦  赵逊  吴珍汉  史大年  刘葵  江万  熊嘉育  INDEPTH研究队 《地球学报》2004,25(1):1-10

德庆-龙尾错剖面层析速度结构剖面揭示了在高原地壳发生缩短与增厚后,高速的印度大陆地幔岩石圈分为两层以不同角度向北伸展到(美)塘盆地的中部(33°N～34°N之间).上层在拉萨地块岩石圈(速度为7.9～8.0 km/s)之下向北伸展过程中发生断裂,形成若T断块,并下沉;下层以较大角度向北俯冲下去,并在32°N之下进人软流圈;发现北部有一浅一深2条低速带,可能代表地幔内温度较高的热流体的流动通道,并产生强烈的各向异性.浅处低速带与深部低速带有联系;此低速带与东部Wittlinger发现的34.5°N深部的高温低速体没有直接联系,后者呈NV-SE走向.  相似文献   

大连上震旦统地震灾变事件研究   总被引：20，自引：4，他引：16  

彭阳  李黄志等 《地质学报》2001,75(2):221-227,T004

笔者在大连工作区的上震旦统南关岭组、甘井子组和营城子组碳酸盐岩地层中,识别出以震动液化脉、震动液化角砾岩、碳酸盐岩注积岩等震积岩为代表的古地震灾变事件层（工作区缺失上震旦统顶部的兴民村组震积岩）,这在工作区属首次发现,这一发现进一步提高了辽南震旦系的研究程度,证明了辽南地区晚震旦世存在4个地震活跃期,从而为区域地层对比提供了新的实际材料,新发现的甘井子组白云岩中的地震灾变事件层表现为白云石质的震动液化脉及液化卷曲变形,是对辽南震旦系研究程度的提高和丰富。  相似文献   

皖东南黄片麻岩的锆石U—Pb年龄   总被引：22，自引：2，他引：22  

涂荫玖杨晓勇  郑永飞李惠民 《岩石学报》2001,17(1):157-160

在皖东嘉山南黄地区新元古代张八岭岩群之下,隐伏一套角闪岩相的TTG质片麻岩类。单颗锆石U-Pb法年龄测定得到其不一致线上交点年龄为2493±19Ma,代表了片麻岩原岩的形成年龄。这是扬子陆块北东缘首次发现的新太古代基底,证实扬子陆块北缘存在较广泛的新太古代—古元古代基底。  相似文献   

宁芜盆地边界断裂带及邻区玄武岩特征和意义     

赵玉琛 《岩石矿物学杂志》1992,11(3):225-238

宁芜火山岩盆地边缘主要由北东和北西向边界断裂构成。西界为长江破碎带,发育早,属张扭性,切割较浅;东界为方山—小丹阳断裂,属压扭性,切割较深;南、北边界均属扭性,发育最晚。新生代玄武岩喷发受边界断裂性质及其构造演化控制,分三期:早期始于早第三纪,沿长江破碎带分布,属高铝拉斑玄武岩,生成较浅;中期喷发于晚第三纪,主要沿方山—小丹阳断裂分布,先后为响碧玄岩—碱性橄榄玄武岩,多幔源二辉橄榄岩包体、捕虏晶及下伏岩层碎块,生成很深;晚期喷发属早更新世,以富钛响碧空岩为主,受北西及东西向断裂交叉点控制。经计算比较,本区玄武岩不具备找金刚石矿产的前景,但从一些岩筒中深部地层碎块看,盆缘地带仍可能是寻找宁芜盆地本身深部铁矿的目标区。  相似文献   

层间氧化带型砂岩铀矿床地浸过程的热力学研究：以伊犁盆地512铀矿床为例   总被引：4，自引：2，他引：2  

李德平  王保群等 《地质论评》2002,48(6):642-650

伊梨盆地512层间氧化带型砂岩铀矿床是中国第一个工业化规模开发的地浸铀矿床,作者简要地介绍了其地质特征和地浸开发工艺,并利用较新的Gibbs自由能和平衡常数数据,对该矿床地浸处理中铀的地球化学行为进行了定量研究。首先,通过标准电动势（E^o）,氧化-还原电位（Eh）的计算和分析,阐明了H2O2、硝酸盐、大气中自由氧都能提升溶液的Eh值,从而加速矿物相U^4 的氧化溶解,为了节约地浸氧化剂成本,对于U^4 /U^6 比值不太高的矿床来说,建议充分利用大气中自由氧化氧化剂,然后,通过化学平衡计算,推导出了地下水和硫酸浸出液中铀存在形式的计算公式,计算结果表明：（1）512铀矿床矿体所赋存的含矿层地下水中,铀主要以碳酸铀酰类络合物形式存在,并且以UO2（CO3)^4-3和UO2（CO3）^2-2形式为主,并随着pH从7.31升高到8.20,UO2CO3从3.80%降低到0.06%,UO2（CO3）^2-2从21.91%降低到3.12%,而UO2（CO3）^4-3则从74.28%升高到96.82%,（2）512铀矿床硫酸浸出液中,铀主要以硫酸铀酰类络合物形式存在,其中,UO2SO4占63.28%～ 63.86%,UO2(SO4)^2-2占16.55%～21.36%,UO^2 2占15.04%～19.62%,从推导出的计算公式可以看出,硫酸浸出液中铀的存在形式随溶液pH、总SO^2-4含量的变化而变化,并呈非线性关系,为了提高离子交换树脂的吸附性能,可利用文中推导出的公式进行计算,以使调节溶浸液的pH和总SO^2-4含量,从而达到浸出液中铀存在形式的最佳比例关系,最后,因热力学数据对化学反应平衡计算的影响呈指数关系,在进行热力学数据计算时,必须采用较新、较准确的数据。  相似文献   

电阻率层析成像和激电测深对栾川铅锌矿的联合勘探     

李清林  邢克元  张建志  秦建增 《CT理论与应用研究》2002,11(4):36-38

在栾川铅锌矿的物探工作中，采用了电阻率层析成像和激电测深两种方法，电阻率层析成像法采用温纳装置或偶极装置，电极数量和极距视情况而定，主要调查工作区内隐伏构造情况，激电测深采用对称四极测深法，最小AB／2距为3M，最大AB／2距为500M，主要研究激电测深参数的变化规律，对于含矿构造而言，激电参数呈异常高值反映，视极化率在15－40％，两种方法的联合应用，具有快速而准确的特点，在探矿工作中取得了良好的效果。  相似文献