广西福海山地区物探测量结果及其解释

简要介绍了高精度磁测、210 Po法和EH-4电导率成像系统的工作原理。通过对已知矿床剖面试验成果分析解释,发现在铀矿体上方地表存在负磁异常和210 Po异常。把福海山地区高精度磁测和210Po法面积测量结果与已知矿床剖面试验成果进行对比分析,圈出了铀矿化区和断裂构造F1、隐伏断裂F0的分布特征,并采用EH-4电磁测深进行验证。说明利用高精度磁测和210 Po法可以有效地推测出测区构造、断裂带的分布范围,为矿区矿化地段深部找矿工作提供有利的勘查区域范围,为下一步的普查工作提供了可靠的地球物理依据。     

高密度电法在宝兴县草坪鞋石膏矿勘查中的应用

通过对四川宝兴县草坪鞋石膏矿区开展高密度电法工作,经采对数据的处理及地质解释,发现了石膏工业矿层及分布状态,取得了较好的地质效果。     

基于岩性相单元和孔隙结构的低孔低渗储层有效性测井识别方法:以西湖凹陷NB1构造为例

东海西湖凹陷是近海最大的盆地之一,近些年在中深层花港组储层中获得重大发现.然而,由于储层具有厚度大、非均质性强、低孔低渗、孔隙结构复杂等特征,给精细评价和甜点储层的预测带来极大困难.利用高分辨率电成像资料,在岩性和层理构造识别的基础上,将研究区储层划分成槽状交错层理细中砂岩、板状交错层理细中砂岩、槽状交错层理细砂岩、板...     

斜井三维VSP动校叠加处理方法

针对三维VSP目的层成像问题,在反射点计算、道集抽取、动校正和叠加等处理方法上进行了研究和总结。采用等效连续速度模型折射线算法计算反射点位置,以反射点面元抽出共反射点道集,然后进行动校正。这里采用扫描的办法计算出正确的双程垂直旅行时,再进行变叠加次数的叠加处理,得到叠加剖面。最后对射线追踪方法得到的斜井三维VSP理论记录进行了处理,验证了方法的正确性。     

A ballistics analysis of the Deep Impact ejecta plume: Determining Comet Tempel 1's gravity, mass, and density

In July of 2005, the Deep Impact mission collided a 366 kg impactor with the nucleus of Comet 9P/Tempel 1, at a closing speed of 10.2 km s⁻¹. In this work, we develop a first-order, three-dimensional, forward model of the ejecta plume behavior resulting from this cratering event, and then adjust the model parameters to match the flyby-spacecraft observations of the actual ejecta plume, image by image. This modeling exercise indicates Deep Impact to have been a reasonably “well-behaved” oblique impact, in which the impactor-spacecraft apparently struck a small, westward-facing slope of roughly 1/3-1/2 the size of the final crater produced (determined from initial ejecta plume geometry), and possessing an effective strength of not more than . The resulting ejecta plume followed well-established scaling relationships for cratering in a medium-to-high porosity target, consistent with a transient crater of not more than 85-140 m diameter, formed in not more than 250-550 s, for the case of (gravity-dominated cratering); and not less than 22-26 m diameter, formed in not less than 1-3 s, for the case of (strength-dominated cratering). At , an upper limit to the total ejected mass of 1.8×¹⁰⁷ kg (1.5-2.2×¹⁰⁷ kg) is consistent with measurements made via long-range remote sensing, after taking into account that 90% of this mass would have stayed close to the surface and then landed within 45 min of the impact. However, at , a lower limit to the total ejected mass of 2.3×¹⁰⁵ kg (1.5-2.9×¹⁰⁵ kg) is also consistent with these measurements. The expansion rate of the ejecta plume imaged during the look-back phase of observations leads to an estimate of the comet's mean surface gravity of (0.17-0.90 mm s⁻²), which corresponds to a comet mass of mt=4.5×¹⁰¹³ kg (2.3-12.0×¹⁰¹³ kg) and a bulk density of (200-1000 kg m⁻³), where the large high-end error is due to uncertainties in the magnitude of coma gas pressure effects on the ejecta particles in flight.     

Estimating Black Hole Masses of AGNs using Ultraviolet Emission Line Properties

Based on measured broad line region sizes in the reverberation-mapping AGN sample, two new empirical relations are introduced to estimate the central black hole masses of radio-loud high-redshift (z > 0.5) AGNs. First, using the archival IUE/HST spectroscopy data at UV band for the reverberation-mapping objects, we obtained two new empirical relations between the BLR size and Mg II/C IV emission line luminosity. Secondly, using the newly determined black hole masses of the reverberation-mapping sample as calibration, we found two new relationships for determining the black hole mass with the full width at half maximum and the luminosity of Mg II/C IV line. We then apply the relations to estimate the black hole masses of the AGNs in the Large Bright Quasar Survey and a sample of radio-loud quasars. For the objects with small radio-loudness, the black hole mass estimated using the RBLR-LMgII/C IV relation is consistent with that from the RBLR-L3000 (?)/1350(?) relation. For radio-loud AGNs, however, the mass estimated from the RBLR-LMgII/CIV relation is sys- tematically lower than that from the continuum luminosity L3000(?)/1350(?). Because jets could have significant contributions to the UV/optical continuum luminosity of radio-loud AGNs, we emphasize once again that for radio-loud AGNs, the emission line luminosity may be a better tracer of the ionizing luminosity than the continuum luminosity, so that the relations between the BLR size and UV emission line luminosities should be used to estimate the black hole masses of high redshift radio-loud AGNs.     

Ghost Images in Schmidt CCD Photometry

The wide field of the Schmidt telescope implies a greater chance of the field containing bright objects, and the presence of a corrector lens produces a certain type of ghost images. We summarize and confirm the features of such ghost images in Schmidt CCD photometry. The ghost images could be star-like under special observational conditions. The zenith distance of the telescope, among other factors, is found to correlate with different patterns of the ghost images. Some relevant issues are discussed and possible applications of our results are suggested.     

瑞雷面波勘探的过去、现在和未来

回顾了瑞雷面波勘探发展的历史,剖析了面波频散曲线正反演的进展及存在的问题,重点指出在石油和煤炭反射地震中,应从剔除面波转变为利用面波,并借助现有石油“大炮”反射地震资料中“有害的”瑞雷面波提取浅层地质结构信息,为反射地震静校正、近地表工程地质评价等提供物性参数,把反射地震的面波干扰变为对勘探十分有利的参数提取源,实现以强干扰面波为主要数据源的浅层结构探测,以促进瑞雷面波勘探技术的进一步发展。     

Search for shadowing of primary cosmic radiation by the moon at TeV energies

The antimatter research through the earth moon ion spectrometer (ARTEMIS) experiment is described in terms of searching for the moon's shadow in the primary cosmic radiation at TeV energies. Observations were made using the Whipple 10 m Imaging Atmospheric erenkov Telescope, in conjunction with a special optical filter to suppress unwanted moonlight. Monte Carlo simulations were used to predict that the magnitude of shadowing based on a pure proton beam would be 1% of the cosmic ray background. Observations and event classification are discussed, and results of a search for shadowing based on both protons and antiprotons are presented. Atmospheric fluctuations giving rise to non-statistical event rates constituted a limiting factor to the sensitivity of the shadow search as they rivaled or exceeded statistical errors. It is demonstrated that the experiment does not have sufficient sensitivity to moon shadowing which would allow a search for an antimatter component in the primary cosmic ray flux at the percent level. Possible future improvements of the technique are discussed.     

Results from the AIM-IT Meteor Tracking System

The recent development and data collection results of the Astrobiology Instrumentation for Meteor Imaging and Tracking (AIM-IT) system, has demonstrated an ability to point narrow field-of-view instruments at transient events such as meteors. AIM-IT uses the principle of tracking moving objects via a paired set of relay mirrors along with an integrated hardware/software solution, to acquire and track meteors in real-time. Development of the instrument has progressed from a prototype rocker-box system through more recent use of a fast response mirror system during several meteor shower campaigns. Several narrow field of view instruments have been deployed using AIM-IT including high spatial resolution video, high frame rate video, and meteor spectrographic equipment. Analysis of the imagery shows evidence for meteor fragmentation in as many as 20% of the meteors tracked thus far. The success of the AIM-IT technology in tracking meteors during their luminous flight provides a new tool in enhancing the capabilities and data volume that can be obtained with existing narrow field of view instruments.