青海南部地区煤炭资源勘查思路

青海南部及其毗邻地区,是青海省乃至全国工业基础最薄弱、社会经济最落后的地区。煤炭资源紧缺,是制约其经济发展的重要因素之一。查明煤炭资源赋存状况,探讨聚煤规律,指出进一步找煤勘探的方向,科学、合理地开发煤炭资源,以带动其它资源开发,使该区尽快脱贫致富,意义重大。     

Reconstruction of RHESSI Solar Flare Images with a Forward Fitting Method

We describe a forward-fitting method that has been developed to reconstruct hard X-ray images of solar flares from the Ramaty High-Energy Solar Spectroscopic Imager (RHESSI), a Fourier imager with rotation-modulated collimators that was launched on 5 February 2002. The forward-fitting method is based on geometric models that represent a spatial map by a superposition of multiple source structures, which are quantified by circular gaussians (4 parameters per source), elliptical gaussians (6 parameters), or curved ellipticals (7 parameters), designed to characterize real solar flare hard X-ray maps with a minimum number of geometric elements. We describe and demonstrate the use of the forward-fitting algorithm. We perform some 500 simulations of rotation-modulated time profiles of the 9 RHESSI detectors, based on single and multiple source structures, and perform their image reconstruction. We quantify the fidelity of the image reconstruction, as function of photon statistics, and the accuracy of retrieved source positions, widths, and fluxes. We outline applications for which the forward-fitting code is most suitable, such as measurements of the energy-dependent altitude of energy loss near the limb, or footpoint separation during flares. Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1022469811115     

北祁连中西段与超基性岩有关的金矿化特征及成因探讨

北祁连中西段发育三套早古生代蛇绿岩及相应的基性、超基性岩,呈北、中、南三条带状分布。区内金的活化、迁移主要受控于超基性岩带和与其分布近于一致的两条韧性剪切带,金矿化主要发生在强蚀变超基性岩体内、岩体与围岩接触带、断裂破碎蚀变带内。根据包裹体测温及成分测定、稳定同位素特征资料及超基性岩中金丰度值等分析,金矿物质主要来自超基性岩,流体来源于深部,其成因属与超基性岩有关的韧性剪切带型金矿床。     

青藏高原多年冻土概论

本文较系统地阐述了青藏高原多年冻土的地带性规律、冻土构造以及融区的类型和分布特征,详细论述了不同作用下形成的冻土(冰缘)地貌,并对青藏高原的冰缘期进行了初步划分与对比。     

湿浸硫酸镍工艺中的二次浸取

湿法浸取硫酸镍工艺研究中,净化提纯工艺采取了蒸发浓缩浸液、分步沉淀杂质的技术方案。中试表明,采用此种工艺生产效率很低,还导致生产流水线上的设备匹配性差。为此,作者提出了二次浸取的技术方案。实验室及中试试验表明:采用二次浸取工艺替代蒸发浓缩工艺,行之有效。     

海拉尔盆地贝尔凹陷布达特群水力破裂的岩石学特征及其成因探讨

海拉尔盆地贝尔凹陷布达特群凝灰质泥岩中发育大量凝灰质泥岩角砾。岩芯及透射光显微镜观察发现,这是一种水力破裂体系中流体和岩石作用的产物一水压碎屑岩。水压碎屑岩的岩石学特征表现为：角砾之间具有可拼合性、岩芯横切面上发育大量“T”型垂直裂缝、微细纤维状铁白云石脉对壁生长。水力破裂作用的成因主要与布达特群岩性组合特征、构造-流体作用有关。     

塔里木盆地晚泥盆世-早石炭世东河砂岩沉积相

东河砂岩是塔里木盆地主要的勘探目的层和产油层之一。经过多年艰苦勘探和多学科综合研究,现已认识到东河砂岩为晚泥盆世晚期至早石炭世早期海平面上升背景下沉积的一套海侵底砂（砾）岩,在盆地范围内是一个明显的穿时沉积体。东河砂岩以滨浅海相陆源碎屑沉积占优势,局部发育海陆过渡相陆源碎屑沉积。根据盆地内100多口井资料的岩石学特征、沉积特征以及其它指相标志的综合分析,在东河砂岩中识别出滨岸、河口湾、辫状河三角洲以及冲积扇等不同的沉积相类型,其中高能碎屑滨岸相最重要,分布最广。东河砂岩沉积早期和中期,盆地主要为高能碎屑滨岸相和碎屑陆棚相沉积,末期海侵达到最大,盆地内为碳酸盐台地沉积,而轮南及盆地北部一带受物源区的影响,出现混积滨岸和碎屑滨岸沉积。东河砂岩明显具有填平补齐的沉积特征,其砂体厚度在缓坡处减薄、陡坡处增厚、遇孤岛减薄或尖灭,这些沉积特征为形成东河砂岩非构造圈闭奠定了良好的地质基础。满加尔、轮南、塔中、玛扎塔格以及草湖地区都有可能找到该类油气藏（田）,展示了东河砂岩非构造圈闭的良好勘探前景。     

Analysis and interpretation of Cassini Titan radar altimeter echoes

The Cassini spacecraft has acquired 25 radar altimeter elevation profiles along Titan's surface as of April 2008, and we have analyzed 18 of these for which there are currently reconstructed ephemeris data. Altimeter measurements were collected at spatial footprint sizes from 6-60 km along ground tracks of length 400-3600 km. The elevation profiles yield topographic information at this resolution with a statistical height accuracy of 35-50 m and kilometer-scale errors several times greater. The data exhibit significant variations in terrain, from flat regions with little topographic expression to very rugged Titanscapes. The bandwidth of the transmitted waveform admits vertical resolution of the terrain height to 35 m at each observed location on the surface. Variations in antenna pointing and changes in surface statistics cause the range-compressed radar echoes to exhibit strong systematic and time-variable biases of hundreds of meters in delay. It is necessary to correct the received echoes for these changes, and we have derived correction algorithms such that the derived echo profiles are accurate at the 100 m level for off-nadir pointing errors of 0.3° and 0.6°, for leading edge and echo centroid estimators, respectively. The leading edge of the echo yields the elevation of the highest points on the surface, which we take to be the peaks of any terrain variation. The mean value of the echo delay is more representative of the mean elevation, so that the difference of these values gives an estimate of any local mountain heights. Finding locations where these values diverge indicates higher-relief terrain. Elevation features are readily seen in the height profiles. Several of the passes show mountains of several hundred m altitude, spread over 10's or even 100's of km in spatial extent, so that slopes are very small. Large expanses of sub-100 m topography are commonplace on Titan, so it is rather smooth in many locations. Other areas exhibit more relief, although the overall observed variation in surface height on any pass is less than about 1 km. Some elevation features correspond to observed changes in brightness in Cassini infrared images, but many do not. Correspondence between the imaging SAR ground tracks and the altimeter paths is limited, so that identifying elevation changes with higher resolution SAR features is premature at present.     

Titan's surface at 2.2-cm wavelength imaged by the Cassini RADAR radiometer: Calibration and first results

The first comprehensive calibration and mapping of the thermal microwave emission from Titan's surface is reported based on radiometric data obtained at 2.2-cm wavelength by the passive radiometer included in the Cassini Radar instrument. The data reported were accumulated from 69 separate observational segments in Titan passes from Ta (October 2004) through T30 (May 2007) and include emission from 94% of Titan's surface. They are diverse in the key observing parameters of emission angle, polarization, and spatial resolution, and their reduction into calibrated global mosaic maps involved several steps. Analysis of the polarimetry obtained at low to moderate resolution (50+ km) enabled integration of the radiometry into a single mosaic of the equivalent brightness temperature at normal incidence with a relative precision of about 1 K. The Huygens probe measurement of Titan's surface temperature and radiometry obtained on Titan's dune fields allowed us to infer an absolute calibration estimated to be accurate to a level approaching 1 K. The results provide evidence for a surface that is complex and varied on large scales. The radiometry primarily constrains physical properties of the surface, where we see strong evidence for subsurface (volume) scattering as a dominant mechanism that determines the emissivity, with the possibility of a fluffy or graded-density surface layer in many regions. The results are consistent with, but not necessarily definitive of a surface composition resulting from the slow deposition and processing of organic compounds from the atmosphere.     

Fundamentally distinct outcomes of asteroid collisional evolution and catastrophic disruption

The outcomes of asteroid collisional evolution are presently unclear: are most asteroids larger than 1 km size gravitational aggregates reaccreted from fragments of a parent body that was collisionally disrupted, while much smaller asteroids are collisional shards that were never completely disrupted? The 16 km mean diameter S-type asteroid 433 Eros, visited by the NEAR mission, has surface geology consistent with being a fractured shard. A ubiquitous fabric of linear structural features is found on the surface of Eros and probably indicates a globally consolidated structure beneath its regolith cover. Despite the differences in absolute scale and in lighting conditions for NEAR and Hayabusa, similar features should have been found on 25143 Itokawa if present. This much smaller, 320 m diameter S-asteroid was visited by the Hayabusa spacecraft. Comparative analyses of Itokawa and Eros geology reveal fundamental differences, and interpretation of Eros geology is illuminated by comparison with Itokawa. Itokawa lacks a global lineament fabric, and its blocks, craters, and regolith may be inconsistent with formation and evolution as a fractured shard, unlike Eros. An object as small as Itokawa can form as a rubble pile, while much larger Eros formed as a fractured shard. Itokawa is not a scaled-down Eros, but formed by catastrophic disruption and reaccumulation.