差分GPS在乌拉特后旗1:25万区域重力调查中的应用     

赵军  关云鹏  孙禹成 《西部资源》2011,(5):94-96

测地工作精度的高低直接影响着重力测量的精度,研究并采取行之有效的测地方法来配合重力测量工作是十分必要的。乌拉特后旗1:25万区域重力调查GPS测地工作采用1954年北京坐标系,重力测点平面位置、正常高采用差分GPS测量方法。结果表明,采用此方法既能满足技术要求,又达到了省时省力,且达到了重力测量的精度要求。  相似文献   

青南高原西部砂金成矿条件分析     

田耀亭  王志成 《青海国土经略》1994,(2)

青南高原西部,处于柴达木准地台与松潘—甘孜印支褶皱系衔接部位。属于青藏高原北部的可可西里地区,平均海拔4800—5000m,属高寒荒漠干旱气候区。由昆仑山大起伏高山区及江河源高海拔波状平原区组成二级地貌区。通过对该区近代砂金矿形成的物质来源、新构造运动、地貌、气候、水动力条件及供源条件进行分析,认为该区砂金矿床的规模以及砂金找矿的前景并非如人们估计的那样乐观。  相似文献   

Scaling relations of field spirals at intermediate redshift     

A. Böhm  B.L. Ziegler  K.J. Fricke  the FDF Team 《Astrophysics and Space Science》2003,284(2):689-692

In the last few years, galaxies at redshifts up to z ∼ 1 have become accessible for medium-resolved spectroscopy thanks to the new generation of 10 m-class telescopes. With kinematic and photometric information on spiral galaxies in this regime, well-known scaling relations like the Tully-Fisher relation (TFR) can be studied over half a Hubble time. By comparison to local samples, these studies facilitate simultaneous tests of the hierarchical merging scenario and stellar population models. Using the Very Large Telescope, we obtained spatially resolved rotation curves of 78 spiral galaxies in the FORS Deep Field (FDF), covering all Hubble types from Sa to Sm/Irr at redshifts 0.1 < z < 1.0. We find evidence for a B-band luminosity increase of up to 2 mag for low-mass spirals, whereas the most massive galaxies are of the same luminosity as their local counterparts. In effect, the TFR slope decreases significantly. This would explain the discrepant results of previous observational studies. We also present the velocity-size relation and compare it to the predictions of numerical simulations based on the hierarchical merging scenario. This revised version was published online in August 2006 with corrections to the Cover Date.  相似文献   

柴北缘铅石山榴辉岩地质特征     

田承盛 《青海国土经略》2001,(1)

根据对铅石山榴辉岩岩石学、岩石化学、地球化学元素、变质岩相及变质作用等特征,该类岩石形成时代可能为中元古代后期,并经历了四堡期、晋宁期、加里东期三次快速折返及相应的退变质作用叠加,进一步证实了柴北缘地区高压变质带的存在。  相似文献   

秦、祁、昆三大造山带的结合特征     

孙延贵  田琪 《青海国土经略》2001,(1)

秦、祁、昆三大造山带结合地区的物质组成及结构特征显示,其间存在不同时期发育起来的陆缘、陆内转换断层,受其制约,造山带内曾发生大规模侧向运动和由此引起的岩心活动及复杂的构造变形。据此,结合演化可分三阶段,并且秦、祁、昆三大造山带间并不存在东西向贯通的单一结合带,而是在转换断层作用下,分阶段逐步完成了转换结合的结合方式。  相似文献   

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   

东营凹陷东辛2-4井上新世至全新世天文地层研究     

YAO Yi-min )  XU Dao-yi )  ZHANG Hai-feng )  HAN Yan-ben )  ZHANG Shou-peng )  YIN Zhi-qiang )  HE Qing-fang )  BIAN Xue-mei ) ) Geological Scientific Research Institute of Shengli Oilfield Company  SINOPEC  Dongying    ) Institute of Geology  China Earthquake Administration  Beijing    ) National Astronomical Observatories  Chinese Academy of Sciences  Beijing 《地层学杂志》2007,(Z2)

东辛2-4井钻取岩芯0—530.1m,明化镇组上段的上亚段至平原组划分为18个层,其中,下更新统平原组一段(简称平一段)的底作为第四系下界;同时进行了古地磁研究,测定出布容、松山、高斯和吉尔伯特等4个极性时。由于天文地层研究的需要,对90年代古地磁的年龄与"国际地层表"(2004)对比,作了相应调整,确定井深242.5m处的年龄为781ka,274.5m处的为2581ka,452.0m处的为3596ka和529.5m处的为4493ka,井深242.5m和452.0m这两个界线的年龄值作为天文地层计时的标定。研究大致分为两步:①以磁化强度(MI)数值曲线的频谱和小波分析,选定平原组一段102.4m周期和明化镇组上段68.36m周期分别对应于天文偏心率404ka旋回,求出了堆积速率为0.1584mm/a和0.1692mm/a及其他各层位的年龄:井深274.5m处上新统明上(上)亚段顶界的年龄为2546ka,平一段底界的年龄是970ka,不整合的延续时间大约为1.6Myr。②推测明上(上)亚段顶2546—1806ka期间可能沉积了129m地层;而在1806—908ka期间,由于构造活动上升,把原沉积又剥蚀掉了,形成井深274.5m处的一个大的不整合面,对储层孔隙的扩张和压实有重要影响,成为最后二次烃源物质的卸载和封堵。  相似文献