Lattice dynamical system modelling of molecular clouds

Because a comprehensive microscopic treatment of interstellar molecular clouds is out of reach, an alternative approach is proposed in which most of the crucial ingredients of the problem are considered, but at some 'minimal' level of modelling. This leads to the elaboration of a lattice dynamical system , i.e. a time-dependent, spatially extended, deterministic system of macroscopic cells coupled through radiative transfer. Each cell is characterized by a small set of variables and supports a caricatural chemistry possessing the essential dynamical features of more realistic reaction schemes.   This approach naturally precludes quantitative results, but allows heretofore unavailable insights into some of the basic mechanisms at play. We focus on the response of the transfer process and the chemistry to a frozen 'turbulent' velocity field. It is shown that the system settles generically into a state where the effective coupling between cells is neither local nor global, and for which no single length-scale exists.   The spectral lines reconstructed from the spatiotemporal evolution of our model may, depending on the velocity field, exhibit profiles ranging from Gaussian to bimodal with strong realization effects. In the bimodal case, the model intrinsically displays an energy cascade transport mechanism to the cells that cool most efficiently: the feedback of chemistry on radiative transfer cannot be neglected.   Finally, extensions of this work are discussed and future developments are outlined.     

裂缝性碳酸盐岩裂缝的双侧向测井响应特征及解释方法

裂缝评价是裂缝性碳酸盐岩储层评价的关键, 其常规评价方法受到裂缝发育的不均匀性及储层各向异性的影响而存在诸多困难.采用三维数值算法, 利用宏观各向异性地层模型, 研究不同的裂缝参数条件下双侧向测井响应特征, 由此导出一种用于裂缝孔隙度计算的快速算法.分析表明, 裂缝的双侧向响应同裂缝孔隙度与孔隙流体电导率之间存在明显的线性关系, 裂缝的倾角造成双侧向测井曲线幅度差异的变化; 不同倾斜情况下, 将双侧向测井响应近似表示为岩石基岩电阻率、裂缝孔隙度、裂缝流体电导率的函数, 用于裂缝孔隙度的快速计算.实际资料处理表明, 利用双侧向依据该方法确定的裂缝参数同成像测井资料具有良好的对应性.      

Studies of ultracompact H ii regions — II. High-resolution radio continuum and methanol maser survey

High spatial resolution radio continuum and 6.67-GHz methanol spectral line data are presented for methanol masers previously detected by Walsh et al. (1997). Methanol maser and/or radio continuum emission is found in 364 cases towards IRAS -selected regions. For those sources with methanol maser emission, relative positions have been obtained to an accuracy of typically 0.05 arcsec, with absolute positions accurate to around 1 arcsec. Maps of selected sources are provided. The intensity of the maser emission does not seem to depend on the presence of a continuum source. The coincidence of water and methanol maser positions in some regions suggests there is overlap in the requirements for methanol and water maser emission to be observable. However, there is a striking difference between the general proximity of methanol and water masers to both cometary and irregularly shaped ultracompact (UC) H  ii regions, indicating that, in other cases, there must be differing environments conducive to stimulating their emission. We show that the methanol maser is most likely present before an observable UC H  ii region is formed around a massive star and is quickly destroyed as the UC H  ii region evolves. There are 36 out of 97 maser sites that are linearly extended. The hypothesis that the maser emission is found in a circumstellar disc is not inconsistent with these 36 maser sites, but is unlikely. It cannot, however, account for all other maser sites. An alternative model which uses shocks to create the masing spots can more readily reproduce the maser spot distributions.     

利用测井资料分析成岩作用对储集层的影响

应用测井资料进行压实作用、孔隙演化、裂缝、矿物成分详尽分析基础上 ,结合成岩作用各个阶段对储集层性能影响的研究 ,讨论了应用测井资料分析成岩作用对储集层影响的物理基础 ,进而指出应用测井资料分析成岩作用不同阶段对储集层影响的可行性。方法为 :(1 )成岩作用早期 :应用孔隙度测井和岩性测井资料 ,通过压实曲线分析压实作用区间 ;(2 )成岩作用中期 :首先根据孔隙度测井资料分析声波孔隙度、密度 -中子测井孔隙度 ,分析次生孔隙 ,并应用交会图技术 ,确定矿物成分 ,分析胶结、交代作用形式和强度 ,然后根据泥质指示测井确定泥质含量 ,进一步利用自然伽玛能谱测井 ,尤其是Th、K含量分析粘土矿物 ;(3)成岩作用晚期 :进行次生孔隙、裂缝、颗粒成分与含量、粘土矿物分布规律研究。以上分析方法经吐哈盆地实际资料验证 ,效果良好     

地壳内的岩浆动力学过程及其资源与环境效应SCIEI北大核心CSCD

岩浆是将地球内部物质传送到表层系统的主要载体,并造成显著的资源聚集和环境效应。岩浆动力学是研究岩浆的迁移、储存、演化、就位以及喷发过程,侧重物理机制。这些岩浆过程主要发生在岩浆通道系统中,包括岩浆储库和岩浆管道。本文对目前国际岩浆动力学领域一些热点和前沿进行了介绍,这包括从岩浆房到岩浆储库概念的转变、岩浆储库的生长和动力学演化过程、岩浆过程的时间尺度以及岩浆中晶体的生长。然后阐述了岩浆中挥发分的种类和溶解度、获取天然岩浆挥发分含量的方法、一些典型镁铁质岩浆中的挥发分含量、岩浆去气的化学和物理机制,并简要梳理了热液金属矿床的形成过程和岩浆挥发分进入地表圈层系统引发的环境气候效应。最后列举了一些岩浆动力学有关的重要科学问题并建议了进一步的研究方向。     

甘肃花草滩煤矿区沉积相演化与内部构造的地质意义探讨

花草滩煤矿区地处北祁连褶皱带中段北侧,酒东盆地东端。古生界和中生界地层在区内发育较完整,其中石炭系太原组为含煤地层。经二、三维地震勘探、钻探等工作证实矿床总体上受单斜构造控制。石炭纪中期盆地呈逐渐上升趋势,沉积相演化经历了由海相逐渐过渡到海陆交汇相,再到陆相沉积的阶段。F5和F8断层具顺层断裂特征,破坏煤层的连续性,在一定程度上控制了瓦斯突出区的分带,可作为煤矿瓦斯含量高低的分界标志。     

Galaxy formation and evolution – I. The Padua tree-sph code (pd-sph)

In this paper we report on pd-sph , the new tree-sph code developed in Padua. The main features of the code are described and the results of a new and independent series of 1D and 3D tests are shown. The paper is mainly dedicated to the presentation of the code and to the critical discussion of its performance. In particular, great attention is devoted to the convergency analysis. The code is highly adaptive in space and time by means of individual smoothing lengths and individual time-steps. At present it contains both dark and baryonic matter, this latter in the form of gas and stars, cooling, thermal conduction, star formation, feedback from Type I and II supernovae, stellar winds, and ultraviolet flux from massive stars, and finally chemical enrichment. New cooling rates that depend on the metal abundance of the interstellar medium are employed, and the differences with respect to the standard ones are outlined. Finally, we show the simulation of the dynamical and chemical evolution of a disc-like galaxy with and without feedback. The code is suitably designed to study in a global fashion the problem of formation and evolution of elliptical galaxies, and in particular to feed a spectrophotometric code from which the integrated spectra, magnitudes and colours (together with their spatial gradients) can be derived.     

Equivalent width, shape and proper motion of the iron fluorescent line emission from molecular clouds as an indicator of the illuminating source X-ray flux history

Observations of the diffuse emission in the 8–22 keV energy range, elongated parallel to the Galactic plane, and detection of the strong 6.4-keV fluorescent line with ∼ 1 keV equivalent width from some giant molecular clouds (e.g. Sgr B2) in the Galactic Centre region suggest that the neutral matter of these clouds is (or was) illuminated by powerful X-ray radiation, which gave rise to the reprocessed radiation. The source of this radiation remains unknown. A transient source close to the Sgr B2 cloud, or a short outburst of the X-ray emission from a supermassive black hole at the Galactic Centre are the two prime candidates under consideration. We argue that a new generation of X-ray telescopes combining very high sensitivity and excellent energy and angular resolutions would be able to discriminate between these two possibilities when studying time-dependent changes of the morphology of the surface brightness distribution, the equivalent width and the shape of the fluorescent line in Sgr B2 and other molecular clouds in the region. We note also that detection of broad and complex structures near the 6.4-keV line in the spectra of distant AGNs, which are X-ray weak now, may prove the presence of violent activity in the central engines of these objects in the past. Accurate measurements of the line shape may provide information on the time elapsed since the outburst. Proper motion (super- or subluminal) of the fluorescent radiation wave front can give additional information on the location of the source. Observations of the described effects can provide unique information on the matter distribution inside Sgr B2 and other giant molecular clouds.