Revisiting the Local Kinematics of the Milky Way using the New Hipparcos Data

With the new Hipparcos data recently released, we reexamine the kinematics in the solar neighborhood. Two different populations of objects, namely the thin-disk O-B5 stars and the thick-disk K-M giants, are selected for tracing the kinematical parameters of the Galaxy. Using a 3-D kinematical model, the components of the solar motion and the Oort constants are derived. The solutions and the kinematics inferred from both types of stars are analyzed. The results obtained with the new data are compared with those from the old Hipparcos data. We conclude that the present solution provides a more reliable estimation of the Oort constants, thanks to the new reduction of the Hipparcos data that provides even more accurate astrometric measurements of stars.     

The Vignetting Effect of a LAMOST-Type Schmidt Telescope

Optical vignetting of a Schmidt reflector is caused mainly by the spherical primary mirror not being big enough and by the effective light-collecting area of the corrector,which depends on the direction of the star light.Calculations of the vignetting of LAMOST,a special reflecting Schmidt telescope,are made by ray-tracing methods.The results show various features due to LAMOST's structure and observing modes.The un-vignetted field is small compared with its field of view.In the outmost portions of the field vignetting increases rapidly with the distance to the field center.The vignetting at a general position within the field of view is a function of both its distance to the field center and its position angle.Vignetting varies when the telescope points at different declinations and during observations.There is difference in vignetting between direct imaging and multi-fiber spectroscopy.Vignetting distorts the relative intensity of celestial objects at different positions in a field and also affects accurate sky-estimation and sky-subtraction.The determined vignetting functions may be used to correct the vignetting effect; alternatively flat-fielding may be adopted for the calibration.The effective apertures,which affect the signal-to-noise ratio of the observations,depend on the different declinations the telescope is pointing at and also different positions within a field due to vignetting.     

Hyperaccretion after the Blandford-Znajek Process： A New Model for GRBs with X-Ray Flares Observed in Early Afterglows

We propose a three-stage model with Blandford-Znajek (BZ) and hyperaccretion process to interpret the recent observations of early afterglows of Gamma-Ray Bursts (GRBs). In the first stage, the prompt GRB is powered by a rotating black hole (BH) invoking the BZ process. The second stage is a quiet stage, in which the BZ process is shut off, and the accretion onto the BH is depressed by the torque exerted by the magnetic coupling (MC) process. Part of the rotational energy transported by the MC process from the BH is stored in the disk as magnetic energy. In the third stage, the MC process is shut off when the magnetic energy in the disk accumulates and triggers magnetic instability. At this moment, the hyperaccretion process may set in, and the jet launched in this restarted central engine generates the observed X-ray flares. This model can account for the energies and timescales of GRBs with X-ray flares observed in early afterglows.     

国际天文联合会第248届讨论会(2007年10月15-19日,上海)

2007年10月15-19日在中国科学院上海天文台举办了国际天文联合会第248届讨论会,题目为"巨大的飞跃:从毫角秒级到微角秒级的天体测量".     

利用多测井参数预测致密砂岩脆性指数方法研究

致密砂岩储层脆性指数精准预测直接关系到储层压裂方案设计和施工效果.本文以吉林大情字井油田青一段致密砂岩储层为研究对象,充分利用测井和脆性指数室内分析测试资料,在岩心归位的基础上,采用交会图相关性分析法开展了脆性指数的敏感性测井参数优选,并结合层次分析法构建了适用于研究区致密砂岩储层的脆性指数测井预测模型.研究结果表明,...     

安塞坪桥区延长组长9致密油储层预测及有利区优选

针对安塞坪桥区长9油层组致密油储层难以预测、勘探开发有利区不明确、严重制约勘探开发进程等问题,笔者通过对典型取心井岩相、测井相研究,在确定砂岩沉积微相类型及其空间演化的基础上,对砂岩进行横向追踪对比,准确获取单砂体厚度数据,刻画出单砂体展布特征,并结合生产动态情况,优选出致密油勘探开发有利目标区.研究结果表明,研究区致...     

致密砂岩气藏储层成岩流体演化与致密成因机理——-以四川盆地上三叠统须家河组为例

四川盆地上三叠统须家河组储层在岩石学上表现为低成分成熟度、低胶结物含量和结构成熟度中等的“两低一中”特征,总体储层物性较差,属低孔低渗和特低孔特低渗储层,局部发育有少量中孔低渗储层．根据各成岩矿物共生组合关系,可以确定成岩矿物由早到晚形成的相对顺序：早期方解石（泥晶菱铁矿）-石英Ⅰ期加大-绿泥石薄膜-长石、岩屑溶解-绿泥石孔隙衬边-石英Ⅱ期加大（加大、剩余粒间孔、粒间溶孔充填石英）-溶蚀作用-石英Ⅲ期加大（粒间溶孔、粒内溶孔中充填石英）-连晶（含铁）方解石-白云石-铁（方解石）白云石-后期溶蚀作用-石英、方解石脉形成．机械压实作用是使本区岩石固结成岩最主要的因素,石英Ⅱ,Ⅲ期加大作用是使本层砂岩致密化的另一个重要原因．长期封闭条件下成岩流体只对长石和部分岩屑进行溶解,而粒间的胶结物如石英、碳酸盐则未发生溶解,使已致密化的须家河组砂岩孔隙度改变不大,这是须家河组砂岩最终保持致密化的又一个原因．有机质大规模生烃发生在第Ⅱ期石英加大后,烃类选择性进入相对有利的储层中形成致密砂岩烃类气藏．     

滇东威信地区龙潭组致密砂岩矿物组成特征及其油气地质意义

致密气是发育于低孔、特低渗透砂岩中的一种非常规资源,具有丰富的潜在油气储量,但由于其致密低渗透性,压裂改造是致密气高效开发的必须手段,而砂岩储集特征及物质组成对初步评价致密砂岩储层的资源潜力和生产能力有重要意义.运用X射线衍射、显微镜及扫描电镜等技术手段,对滇东威信地区二叠系龙潭组10个致密砂岩露头样品进行定性和定量分...     

中国东部陆相断陷盆地成熟探区油气勘探新领域分析*

经过50多年勘探开发,中国东部陆相油气田均已进入勘探中后期阶段,受石油地质认识局限性和勘探技术的限制,待发现目标日趋隐蔽,油气勘探难度日益增大。针对中国东部陆相断陷盆地深层低孔渗—致密砂岩储集层评价方法的局限性、深部砂砾岩储集体成因模式问题以及基岩风化壳形成和分布的复杂性问题,作者经过近几年的探索和总结,取得以下主要研究进展: (1)基于砂岩储集层物性演化动力学原理,提出了致密砂岩储集层动态评价的新思路和新方法,指出过去评价较低的深部凹陷带低孔渗—致密砂岩体仍然具有较大的勘探潜力; (2)运用地震地层学方法,通过建立断陷盆地陡坡带斜向大型扇三角洲沉积模式,指出斜向大型扇三角洲砂砾岩是断陷盆地深层有利的储集体,可以作为下一步有利勘探方向; (3)根据基岩风化壳双层结构新模式,结合风化壳储集层改造—破坏—保存机理的动力学新模型,指出断陷盆地中低部位是最有利风化壳储集层发育带,断陷盆地缓坡内带(洼槽区)风化壳是下一步油气勘探的重要新领域。文中提出的上述3大勘探新领域不仅是对断陷盆地油气成藏模式的补充和发展,更重要的是展现出中国东部断陷盆地深层常规和非常规油气勘探领域的巨大潜力,为深化东部成熟盆地油气勘探指出了明确的方向。     

四川汶川8.0级地震地下流体异常分析

汶川8.0级地震引起了社会广泛地关注,产生了地震能否预测的疑问以及汶川地震前是否出现了异常的讨论,震后一些学者对前兆资料进行了研究总结,本文在前人研究的基础上仅对地下流体异常进行了分析,认为汶川地震前存在着一些地下流体异常,本文从中期异常、短临异常、同震及震后调整这几个方面对水氡、水位、水温、流量资料进行了分析研究。通过对中期异常的识别及提取,认为采用从属函数方法定量提取异常效果较为理想。