Conformally coupled Abelian gauged Q balls

A conformally coupled Abelian gauged Q ball is studied in curved space. The mass of the Q ball is calculated in terms of the conserved Q charge and the parameters in the lagrangian and a brief discussion is given on the effects produced by the conformal couplings.     

横向各向同性介质地震波场数值模拟研究

地震波场数值模拟是理解地震波在地下介质中的传播特点,帮助解释观测数据的有效手段,而提高计算精度和运算效率是所有波场数值模拟方法研究所追求的目标.有限差分技术是求解波动方程计算效率最高、应用最为广泛的方法之一.但传统的有限差分技术计算过程中的数值频散问题影响了该技术的计算精度与计算效率.本文通过交错网格高阶有限差分技术与通量校正传输方法（Flux|corrected transport method,FCT）相结合, 对横向各向同性介质（Transverse isotropic medium,TI）一阶速度|应力弹性波动方程组进行了数值求解研究.波场快照数值模拟结果表明,本文研究的数值模拟方法与波动方程二阶有限差分方法、交错网格四阶有限差分方法相比,在压制网格数值频散方面有明显的优势,计算精度提高,而且可以利用较大的空间步长,提高计算效率.     

天山北坡绿洲城市空间形态时空特征分析

借助GIS 软件支持, 综合遥感影像、地形图和其它空间数据, 提取天山北坡8 个绿洲城市 1990 年和2000 年建设用地图形信息, 计算1990 年和2000 年天山北坡8 个绿洲城市的平面轮 廓形状的分维数、紧凑度以及城市用地扩展类型, 讨论紧凑度与分维数的关系。研究结果表明, 天 山北坡绿洲城市形态总体特征表现为形状规则, 结构紧凑。1990~2000 年, 城市扩展类型主要为 外延型, 城市形态分维数增加, 紧凑度降低, 城市外部形态趋于复杂化和不规则化, 而内部结构趋 于松散化, 与同时期我国大部分城市的用地扩展方式有所不同。同时, 天山北坡绿洲城市形态特 征描述参数间存在着明显的幂函数关系, 并且是一种线性负相关关系, 即随着分维数的增加, 紧 凑度呈递减的趋势。     

Gravitational Waves and Gravitational-wave Sourcestwo

The recent discovery of gravitational-wave burst GW150914 marks the coming of a new era of gravitational-wave astronomy, which provides a new window to study the physics of strong gravitational field, extremely massive stars, extremely high energy processes, and extremely early universe. In this article, we introduce the basic characters of gravitational waves in the Einstein's general relativity, their observational effects and main generation mechanisms, including the rotation of neutron stars, evolution of binary systems, and spontaneous generation in the inflation universe. Different sources produce the gravitational waves at quite different frequencies, which can be detected by different methods. In the lowest frequency range (f < 10^?15 Hz), the detection is mainly dependent of the observation of B-mode polarization of cosmic microwave background radiation. In the middle frequency range (10^?9 < f < 10^?6 Hz), the gravitational waves are detected by analyzing the timing residuals of millisecond pulsars. And in the high frequency range (10 ? 4 < f < 10⁴ Hz), they can be detected by the space-based and ground-based laser interferometers. In particular, we focus on the main features, detection methods, detection status, and the future prospects for several important sources, including the continuous sources (e.g., the spinning neutron stars, and stable binary systems), the burst sources (e.g., the supernovae, and the merge of binary system), and the stochastic backgrounds generated by the astrophysical and cosmological process. In addition, we forecast the potential breakthroughs in gravitational-wave astronomy in the near future, and the Chinese projects which might involve in these discoveries.     

中子星中心致密天体的双星起源

探讨了认为中心致密天体(CCO)起源于双星的可能性.首先, CCO与正常遗迹脉冲星有着相似的平均自旋周期,但CCO的平均表面磁场强度(B～5.4×10~(10)Gs)低于正常遗迹脉冲星(B～7.7×10~(12)Gs)～2个量级.同时,几乎所有的正常遗迹脉冲星均分布在爱丁顿吸积加速线以上,而CCO全部分布在自旋加速线以下.因此怀疑CCO可能起源于双星吸积加速过程.其次,基于中子星再加速理论,分析了CCO可能的双星演化过程:双星系统中, CCO以M～1017g·s~(-1)的吸积率,经过～106yr的时间共吸积△M～10~(-2)M⊙的物质,其自旋周期将会从P～10 s降低至P～0.1 s,表面磁场强度将会从B～10~(12)Gs降低至B～1010Gs.考虑到～106yr的演化时标远大于CCO遗迹的年龄(～0.3–7 kyr),猜想CCO可能是双星系统中第1颗恒星超新星爆发的产物,而第2颗恒星超新星爆发后双星解体,留下CCO和第2颗恒星的超新星遗迹.该模型预言在CCO附近可能存在一颗年轻的正常脉冲星(P～0.02 s, B～1012Gs),并期望未来的射电望远镜和高能探测器能够进行搜寻.     

大气海洋环境数值模拟中的若干计算问题

为了适应发展气候数值模拟和环境数值模拟的需要,综合介绍了与此密切有关的若干计算问题。首先,指出这类问题易于出现计算紊乱、非物理解和非线性计算不稳定,同时,简要介绍造成这些问题出现的三种机理：虚假频散、能量关系破坏和能谱的非线性转移。然后,把这类问题归结为一种“发展方程”,给出了与此有关的几个定理,阐述了计算稳定性、能量守恒性和算子非负性之间的密切关系。接着,分别介绍了多种完全平方守恒的差分格式的构造方法,其中包括隐式的和显式的完全平方守恒的差分格式,高时间精度和高阶紧致的完全平方守恒的差分格式,同时也给出若干具体算例说明这些格式的计算效果。最后,对全文作了小结,并指出今后应进一步研究的若干重要问题。     

Global velocity field and bubbles in the blue compact dwarf galaxy Mrk 86

We have studied the velocity field of the blue compact dwarf galaxy Mrk 86 (NGC 2537) using data provided by 14 long-slit optical spectra obtained in 10 different orientations and positions. This kinematical information is complemented with narrow-band ([O  iii ]5007 Å and H α ) and broad-band ( B , V , Gunn r and K ) imaging. The analysis of the galaxy global velocity field suggests that the ionized gas could be distributed in a rotating inclined disc, with projected central angular velocity of Ω=34 km s⁻¹ kpc⁻¹. The comparison between the stellar, H  i and modelled dark matter density profile indicates that the total mass within its optical radius is dominated by the stellar component. Peculiarities observed in its velocity field can be explained by irregularities in the ionized gas distribution or local motions induced by star formation.
Kinematical evidences for two expanding bubbles, Mrk 86–B and Mrk 86–C, are given. They show expanding velocities of 34 and 17 km s⁻¹, H α luminosities of 3×10³⁸ and 1.7×10³⁹ erg s⁻¹, and physical radii of 374 and 120 pc, respectively. The change in the [S  ii ]/H α , [N  ii ]/H α , [O  ii ]/[O  iii ] and [O  iii ]/H β line ratios with the distance to the bubble precursor suggests a diminution in the ionization parameter and, in the case of Mrk 86–B, an enhancement of the shock-excited gas emission. The optical–near-infrared colours of the bubble precursors are characteristic of low‐metallicity star‐forming regions (∼0.2 Z_⊙) with burst strengths of about 1 per cent in mass.     

储层构造裂缝定量预测研究及评价方法

裂缝型油气藏油气产量占整个石油天然气产量的一半以上，是21世纪石油增储上产的重要领域之一，但目前致密储集体裂缝参数的定量表征和空间分布规律定量预测评价，仍是石油地质界的前沿问题，在一定程度上阻碍了世界石油工业的发展。从国内、外研究现状来看，对裂缝及裂缝型油气藏预测评价研究仍处于探索阶段。世界上大多数裂缝性油气田的裂缝主要为构造裂缝，对构造裂缝空间分布规律的合理预测评价，无疑对油气勘探开发起到科学的指导作用。本文综述了储层裂缝研究现状、进展和主要研究方法，同时通过近几年工作典型实例阐明裂缝研究在不同类型油气藏勘探中的作用。     

铵盐镍基电镀金刚石钻头

探讨了在普通镀镍溶液中加入铵离子后,电镀液成分和电镀工艺条件对镀层性能的影响,得到了一种用于钻进坚硬致密弱研磨性岩层的优化配方及工艺条件,讨论了铵离子引起的络合作用.实验表明,当氯化铵的质量浓度为18 g/L时可细化镀层晶粒,提高胎体的硬度和脆性,改变胎体与金刚石的包镶程度,从而改变电镀金刚石钻头的性能,得到一种能有效钻进坚硬致密弱研磨性岩石的新性能电镀金刚石钻头.     

Star-forming regions in blue compact dwarf galaxies

We present near-infrared 2.1-μm continuum and Brγ and 1–0S(1) line images of three blue compact dwarf galaxies: II Zw 40, NGC 5253 and He 2-10. Comparison of the morphologies of the emission-line regions and continuum together with the line ratios shows that in these cases the starbursts are typified by strongly peaked Brγ and weak diffuse H₂ emission, indicating the presence of one or more compact nuclei, and also tidal tails. We consider the possible origins of the H₂ emission, and conclude that shock excitation in cloud collisions, and hence dynamical processes such as interactions or mergers, is important. By comparing models of the equivalent width of Brγ to other age constraints from the literature we show that the star formation must have occurred not only recently but in a short-duration burst. The current centres of star formation in all three galaxies are of a similar age but, whereas the hotspots in He 2-10 are coeval, we find phase differences between those in NGC 5253. We compare the masses and sizes of the star formation sites to those of present-day globular clusters.