油气聚集链:内涵、特征与勘探实践:以渤海湾盆地冀中、黄骅坳陷为例

成熟盆地仍然蕴藏着可观的油气资源,目前的油气成藏理论面临越来越难、复杂、隐蔽油气藏勘探的挑战。受“链”事物属性的启发,通过调研、类比国内外油气成藏过程与分布规律,在继承和发展已有油气成藏理论基础上,结合勘探实践,学界提出了“油气聚集链”的概念和认识。油气聚集链指在成因上有密切联系、空间上多呈串珠状链式排列在一起的一系列油气藏组合,是油气成藏与分布本质规律的客观体现。油气聚集链在形式上多表现为油气藏多呈串珠状的链式空间分布特征,实质上表现为油气生成、运移、聚集的沿优势运移通道的链式反应和成藏事件;现今复杂的油气分布是地史上多条油气聚集链叠合的反映;一条完整的油气聚集链由内链、中链和外链组成,它们在成藏背景、成藏条件、成藏机理、富集规律和分布模式上既各有特征,又有连续性,更是紧密有机的油气生运聚成藏整体。“同源多链、一链多藏、多链成域、主链富集”是“油气聚集链”的四大特征。与目前油气成藏理论相比,油气聚集链认识的突出优势在于:发现和论证了油气聚集的链式成藏特点和多呈串珠状链式分布规律,提出沿“油气聚集链”寻找油气藏,比沿“油气聚集带”寻找油气藏的效率更高;将勘探目标的预测精度从油气聚集区带范围提高到某个具体圈闭或甜点。油气聚集链认识具有目前其他油气成藏理论所不具有的独特优势——链式思维,精准定位。依据油气聚集链的认识,提出了“找准链源,梳理链节,确定链环,重视主链”和“全链思维、整体研究,顺链找油、精准勘探”的思路,对指导成熟盆地继续挖掘勘探潜力、新区新领域获得勘探突破,都具有重要现实意义。以油气聚集链的认识为指导,转变勘探思维,在冀中、黄骅坳陷油气勘探中获得重大突破。     

Reanalysis of the Atmospheric Flux of Nutrient Elements to the Southern Yellow Sea and the East China Sea

Based on the recent research results on dry and wet deposition of nutrient elements and sulphate,we estimate the atmospheric flux of nutrient elements and sulphate to the southern Yellow Sea and the East China Sea in each season.The results suggest that the concentrations of nutrient elements and sulphate in aerosol and precipitation show an apparent seasonal cycle with the maximum values in winter and the minimum values in summer.Depositions of nitrate and sulphate are dominated by wet deposition,while the deposition for phosphate is mainly dry deposition.Moreover,compared with the riverine inputs,the atmospheric deposition may be the main source of dissolved inorganic nutrients in the southern Yellow Sea and the East China Sea.     

Bathymetry enhancement by altimetry-derived gravity anomalies in the East Sea (Sea of Japan)

The gravity-geologic method (GGM) was used to enhance the bathymetry of the East Sea (Sea of Japan) with satellite altimetry-derived free-air gravity anomalies and shipborne depth measurements. By comparison with the bathymetry model of Smith and Sandwell’s (SAS) approach (1994), GGM was found to have an advantage with short wavelength (≤12 km) components, while SAS better predicts longer wavelength (≥25 km) components, despite its dependency on density contrast. To mitigate this limitation, a tuning density contrast of 10.25 g/cm³ between seawater and the seafloor was primarily estimated by the downward continuation method and then validated by the check points method with GGM. Similarly, SAS is limited by the “A” value in low-pass part of the Wiener filter, which defines the effective range of the wavelength components on bathymetry. As a final result, we present an enhanced GGM bathymetry model by integrating all available data.     

An Experi mental Study on Wave-Induced Dynamic Stresses in Seabed

1 .IntroductionEvery year ,Taiwanis subjectedtotwo or three typhoonintrusions in average which always causedisasters . Most of the disasters which occur around the coastal zone are due to seabed instability andcoastal structure destruction caused bytyphoo…     

A moving PIV system for ship model test in a towing tank

A moving particle image velocimetry (PIV) system was successfully developed and used in a large towing tank for ship model tests to observe velocity fields near ship models. The experimental method involved adjustable optical devices for various test conditions and a special particle-seeding device. The streamwise and cross-streamwise flow fields of a yacht model and a tanker model were measured. Ship type, bottom shape, and towing speed were found to be the causes of problems affecting optical access and image quality. Possible solutions, deeper optical ducts, dark painting color, and pre-processed analysis method, were proposed and discussed.     

临汾盆地晚冰期至中全新世黄土-古土壤序列的风化特征及指示的气候意义

了解中国北方晚冰期和全新世时期的气候环境变化及其驱动机制,有助于预测未来气候变化的可能情景。基于黄土高原东南缘临汾盆地的黄土-古土壤剖面,在3个AMS14C年代的支持下,通过粒度、磁化率、土壤有机碳以及地球化学元素等指标,重建了临汾盆地晚冰期至中全新世晚期的气候变化历史。结果表明：宋村沟剖面的黄土和古土壤分别处于初等和中等化学风化阶段,而不同地区风成堆积物的化学风化强度存在明显差异,主要受控于东亚夏季风的区域变化。多指标综合分析表明,晚冰期以来临汾盆地的气候演变经历了4个阶段：晚冰期东亚冬季风较强,气候干冷;早全新世东亚夏季风强化,气候向暖湿转变;早中全新世东亚夏季风达到峰值,为最暖湿的适宜期;中全新世晚期东亚夏季风减弱,气候再次转向干冷;临汾盆地的气候变化主要受控于北半球太阳辐射强度和冰量的变化。     

Pulsar radio emission

Radio emission by pulsars is calculated from first principles. In an almost current-free magnetosphere, the two charged components (of the unsteadily escaping pair plasma) have different (and varying) bulk Lorentz factors. Curvature radiation emitted by the more energetic component is thus locally coherent, (so-called antenna mechanism). Strong enough seed signals cause the relativistically streaming charges to enhance their radiation, via an induced drift that can largely exceed the curvature drift. This amplification mechanism is similar to - but different from - that of a maser; we call it a MAIDER. Maximal amplification occurs at an (emission) altitude where the two components have sufficiently separated in energy though not yet separated too strongly in space.     

On measuring low-degree p-mode frequency splitting with full-disc integrated data

The standard method of measuring rotational splitting from solar full-disc oscillation data, based on maximum-likelihood fitting of multi-Lorentzian profiles to oscillation power spectra, systematically overestimates the splitting. One of the reasons is that the maximum likelihood estimators (MLE) become unbiased only asymptotically as the number of data tends to infinity; for a finite data set they are often biased, inducing a systematic error. In this paper we assess by Monte Carlo simulations the amount of systematic error in the splitting measurement, using artificially generated power spectra. The simulations are carried out for multiplets of degree     2 and 3 with various signal-to-noise ratios, linewidths and observing times. We address the possible use of non-MLE estimators that could provide a smaller or negligible systematic error. The implication for asteroseismology is also discussed.     

A Statistical Study of Rapid Sunspot Structure Change Associated with Flares

We reported recently some rapid changes of sunspot structure in white-light(WL) associated with major flares.We extend the study to smaller events and present here results of a statistical study of this phenomenon.In total,we investigate 403 events from 1998 May 9 to 2004 July 17,including 40 X-class,174 M-class,and 189 C-class flares.By monitoring the structure of the flaring active regions using the WL observations from the Transition Region and Coronal Explorer(TRACE),we find that segments in the outer sunspot structure decayed rapidly right after many flares;and that,on the other hand,the central part of sunspots near the flare-associated magnetic neutral line became darkened.These rapid and permanent changes are evidenced in the time profiles of WL mean intensity and are not likely resulted from the flare emissions.Our study further shows that the outer sunspot structure decay as well as the central structure darkening are more likely to be detected in larger solar flares.For X-class flares,over 40% events show distinct sunspot structure change.For M-and C-class flares,this percentage drops to 17% and 10%,respectively.The results of this statistical study support our previously proposed reconnection picture,i.e.,the flare-related magnetic fields evolve from a highly inclined to a more vertical configuration.