Magnetic fields in massive star-forming regions

We present the largest sample of high-mass star-forming regions observed using submillimetre imaging polarimetry. The data were taken using the Submillimetre Common User Bolometer Array (SCUBA) in conjunction with the polarimeter on the James Clerk Maxwell Telescope (JCMT) in Hawaii. In total, 16 star-forming regions were observed, although some of these contain multiple cores. The polarimetry implies a variety of magnetic field morphologies, with some very ordered fields. We see a decrease in polarization percentage for seven of the cores. The magnetic field strengths estimated for 14 of the cores, using the corrected Chandrasekhar and Fermi (CF) method, range from <0.1 mG to almost 6 mG. These magnetic fields are weaker on these large scales when compared to previous Zeeman measurements from maser emission, implying the role of the magnetic field in star formation increases in importance on smaller scales. Analysis of the alignment of the mean field direction and the outflow directions reveals no relation for the whole sample, although direct comparison of the polarimetry maps suggests good alignment (to at least one outflow direction per source) in seven out of the 15 sources with outflows.     

在太阳磁场大气中FeIλ 5324.19(?)谱线的形成深度

本文在用Unno-Beckers方程计算光球和黑子本影磁场内FeIλ5324.19谱线形成过程中,计算了该谱线Stokes参数随5000连续谱光学深度分布的贡献函数及形成深度随波长的变化。计算结果表明:磁光效应的存在给该线横向磁场定标参数Q、U的形成深度的确定带来一定的复杂性,对I和V的形成深度的确定没有明显的影响。结合北京天文台太阳磁场望远镜半宽0.15的双折射滤光器,确定所观测磁场信息的形成深度。当对日面中心观测,在滤光器调至线心时,I形成在光球层及黑子高度100公里左右,在偏离线心0.15时V分量形成高度亦如此,Q、U分量的情况较复杂。     

An observational constraint on the existence of proto-superclusters at z =3.3

Observations have been conducted using the Ooty Radio Telescope in order to place constraints on the evolutionary scenario leading to the formation of the present day superclusters. The experiment attempted to detect 21 cm emission from massive neutral hydrogen condensates at a redshift ofz = 3.3. In an Einstein de-Sitter universe with baryon density Ω = 0.05, about ten condensates were expected in the volume surveyed if superclusters, having H I masses ≃5 × 10₁₅ M _⊙, were the first objects to separate out of the Hubble expansion. The sensitivity of our experiment rules out the existence of these condensates atz = 3.3 unless their lifetimes are less than one-tenth the dispersion in their epoch of formation or the proto-superclusters subtend angles greater than 6 arcmin. The result indicates that superclusters form at z > 3.3 if indeed they were the first objects to condense out of the Hubble flow. An erratum to this article is available at .     

南海北部琼东南盆地陵水段峡谷沉积建造及勘探意义

琼东南盆地中央峡谷为一大型轴向峡谷体系,具有明显的"分段性"特征,不同区段沉积充填和内部结构均存在明显的差异,其中陵水段位于峡谷西段,具有非常好的储层物性特征,是深水区峡谷勘探的重点区域。为了进一步精细刻画陵水段峡谷内部水道复合体的沉积充填及沉积微相展布特征,本文借助新增加的三维地震资料和新钻井资料,通过峡谷三级层序界面的识别,将峡谷充填划分为3个三级层序SQ1、SQ2和SQ3,并通过古生物有孔虫化石带、钙质超微化石带及井-震结合确定了峡谷底界为中中新世晚期S40界面,陵水段峡谷自西向东依次识别出6种主要的内部充填结构,且将SQ3层序细分为5个次级层序(SSQ1~SSQ5);结合属性特征,精细刻画了陵水段峡谷内沉积微相平面展布及空间演化特征,并指出点砂坝在SSQ1层序最发育,且规模较大,横向上连片分布,将是下步勘探的有利储集体。     

德州市城区沙河街组热储地热地质特征研究

通过该井地热钻探及区内已有石油钻探研究资料,对德州市城区古近纪沙河街组地热资源的地质背景、地热地质特征等进行了综合分析研究,认为沙河街组地热资源属于层控型低温地热田,在沧东断裂以东都有分布,热储层厚度超过120m,地热水中碘、锶、铁、偏硅酸达命名浓度,具有一定的开发利用价值。     

东营凹陷八面河北部斜坡带构造特征及形成机制

研究了东营凹陷八面河北部斜坡带的断裂特征、构造演化特征及其形成机制,明确了该区的断裂展布特点和断层活动性,弄清了北部斜坡带的演化规律,同时分析该区的构造变形特征。结果表明：中生代以后,八面河地区存在2种独立的构造变形系统：一是板块边缘相互作用力;二是到后期由于板块的持续俯冲,地幔底辟作用在岩石圈底面产生的牵引力。八面河北部地区在这2种构造力的综合作用下,不同时期表现出不同的构造变形特征。     

塔里木盆地克拉苏构造带巴什基奇克组地层水化学特征及流体成因

地层水化学特征及流体成因的分析对油气成藏的研究具有重要意义,对库车坳陷克拉苏构造带的地层水化学特征及流体成因的研究有助于油气藏的勘探开发。塔里木盆地库车坳陷克拉苏构造带构造特征复杂,地层水化学特征及流体系统缺乏系统研究。为了明确克拉苏构造带地层水化学特征及其流体系统,对地层水的溶解性总固体(TDS)、离子比例系数及压力分布特征进行了分析。研究结果表明：克拉苏构造带地层水以高TDS的卤水为主(平均值为154.92 g/L),按照苏林分类主要为CaCl₂型,按照舒卡列夫分类为Cl-Na型和Cl-Na·Ca型,为典型的沉积埋藏水。地层水的脱硫系数较低(平均值小于1.2)、变质系数较高(平均值大于6),表明地层的封闭性较好,地层水经历了较强的水岩反应。参照地层压力场、岩性特征及地层水特征,将库车凹陷克拉苏构造带划分为第四系—新近系、古近系、白垩系、侏罗系及下伏地层四套流体系统。结合研究区岩性组成、构造演化特征及地层水化学特征分析,明确了白垩系巴什基奇克组地层水的成因为白垩系原始沉积水与侏罗系烃源岩生烃时排出的有机物转化流体、沉积水及古近系膏盐层高盐度流体的混合。     

银河系卫星星系研究进展

对银河系内卫星星系进行全面的"人口普查"具有重要的意义。目前已经发现了二十几个卫星星系,其光度范围分布很广,最暗的矮星系比球状星体还暗。叙述了卫星星系的光度分布、空间分布和动力学性质。总结了观测和理论研究进展,并讨论了星流和伽玛射线在研究银河系结构和暗物质性质方面的贡献。表明了卫星星系的统计分布能用来很好地限制冷暗物质理论和星系形成的相关物理过程,同时指出当前研究的局限性和可能的发展方向。     

Impact megadomes and the origin of the martian crustal dichotomy

We show that a sufficiently energetic impact can generate a melt volume which, after isostatic adjustment and differentiation, forms a spherical cap of crust with underlying depleted mantle. Depending on impact energy and initial crustal thickness, a basin may be retained or impact induced crust may be topographically elevated. Retention of a martian lowland scale impact basin at impact energies ∼3 × 10²⁸-3 × 10²⁹ J requires an initial crustal thickness greater than 10 km. Formation of impact induced crust with size comparable to the martian highlands requires a larger impact energy, ∼1-3 × 10³⁰ J, and initial crustal thickness <20 km. Furthermore, we show that the boundary of impact induced crust can be elliptical due to a spatially asymmetric impact melt volume caused by an oblique impact. We suggest the term “impact megadome” for topographically elevated, impact induced crust and propose that processes involved in megadome formation may play an important role in the origin of the martian crustal dichotomy.