Determination of the Thickness of Non-Edge-on Disk Galaxies

We propose a method to determine the thickness of non-edge-on disk galaxies from their observed structure of spiral arms, based on the solution of the truly three-dimensional Poisson‘s equation for a logarithmic disturbance of density and under the condition where the self-consistency of the density wave theory is no longer valid. From their measured number of arms, pitch angle and location of the innermost point of the spiral arms, we derive and present the thicknesses of 34 spiral galaxies.     

时间序列的趋势转折点提取算法及应用研究

针对时间序列趋势转折点的提取,提出一种基于矢量转角和极值点相结合的改进算法,并应用到地震观测资料的分析中。结合地震对应规则,对山西断陷带北部小磨流动水准XM₁-XM₂测线的地震预测效能进行评估。结果表明：1）该算法可用于时间序列趋势转折点的自动提取,提高了人工判别的工作效率,实现了转折点的定量化识别;2）从数据统计的角度考虑,该测线与200 km范围内M4.5以上地震有较好的对应关系,预测效能评估结果R=0.63（R₀=0.43）;3）2000年以后该测线的地震虚报率较高,分析认为可能与远场强震引起的应力变化有关。     

风动潜孔锤在北京地铁长螺旋旋(定)喷搅拌帷幕桩施工中的应用

本文介绍了长螺旋旋喷搅拌桩在北京地铁明挖车站帷幕施工中的应用情况,在遇到坚硬的地下障碍物时引入了风动潜孔锤形成长螺旋潜孔锤振动旋喷桩,较好地克服了地下障碍,顺利完成帷幕桩施工。为同类情况下施工帷幕桩提供了有益的借鉴。     

2017年6月20日肃南地震台洞体应变NS分量转折变化分析

在跟踪分析肃南地震台2013—2017年洞体应变观测数据时发现,2017年6月20日NS分量曲线出现转折变化,23日到30日转折速率有所降低,调研该区地震活动性、自然条件、测区环境,并与同测点其他测项数据等进行对比,分析发现,该转折变化由观测山洞降雨渗漏引起,对渗漏点封堵后,该变化消失。     

The opacity of spiral galaxy disks: IX. Dust and gas surface densities

Our aim is to explore the relation between gas, atomic and molecular, and dust in spiral galaxies. Gas surface densities are from atomic hydrogen and CO line emission maps. To estimate the dust content, we use the disk opacity as inferred from the number of distant galaxies identified in twelve HST/WFPC2 fields of ten nearby spiral galaxies. The observed number of distant galaxies is calibrated for source confusion and crowding with artificial galaxy counts and here we verify our results with sub‐mm surface brightnesses from archival Herschel ‐SPIRE data. We find that the opacity of the spiral disk does not correlate well with the surface density of atomic (H I) or molecular hydrogen (H₂) alone implying that dust is not only associated with the molecular clouds but also the diffuse atomic disk in these galaxies. Our result is a typical dust‐to‐gas ratio of 0.04, with some evidence that this ratio declines with galactocentric radius, consistent with recent Herschel results. We discuss the possible causes of this high dust‐to‐gas ratio; an over‐estimate of the dust surface‐density, an under‐estimate of the molecular hydrogen density from CO maps or a combination of both. We note that while our value of the mean dust‐to‐gas ratio is high, it is consistent with the metallicity at the measured radii if one assumes the Pilyugin & Thuan (2005) calibration of gas metallicity. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

南海台风“尤特”螺旋结构的综合分析

应用卫星观测等资料及高分辨数值模拟方法,综合分析了台风“尤特”（2001）螺旋结构的多要素三维动热力特征。结果表明：台风螺旋结构在许多动热力物理量场上都有明显表现,如散度、垂直速度、涡度、相对湿度、水汽通量散度、垂直水汽通量、θse、位势高度、对流云等,但是不同要素及在不同高度层上的表现有所不同,主要具有以下特点：（1）台风螺旋结构在大多数动热力物理量场上都有明显的表现,不同要素及不同高度上螺旋结构的表现形式有所不同,但通过动热力过程相互关联;（2）地面螺旋雨带与低空辐合、上升运动、低空高湿高θse、高空辐散等对应,反映了螺旋结构的对流特性;（3）螺旋结构自下往上明显向外倾斜,其中散度场的倾斜比垂直运动大;（4）螺旋带的强度和伸展高度沿径向渐次减弱和降低。     

Spiral structure formed in a pair of interacting galaxies

The formation of spiral structure in a galaxy, as a result of the gravitational perturbation caused by a permanent companion, is studied. It is found that spiral structure appears only when a resonance exists between the rotational frequency of the stars in the galaxy and the rotational frequency of the companion galaxy. The number of spiral arms depends strongly on the particular resonance. In the case where the companion moves in an elliptic orbit, spiral arms are formed when a resonance, inside the galactic body, exists in almost all the parts of the orbit or, at least, in the largest part of it.     

GHASP: an Hα kinematic survey of spiral and irregular galaxies – IV. 44 new velocity fields. Extension, shape and asymmetry of Hα rotation curves

We present Fabry–Perot observations obtained in the frame of the GHASP survey (Gassendi HAlpha survey of SPirals). We have derived the Hα map, the velocity field and the rotation curve for a new set of 44 galaxies. The data presented in this paper are combined with the data published in the three previous papers providing a total number of 85 of the 96 galaxies observed up to now. This sample of kinematical data has been divided into two groups: isolated (ISO) and softly interacting (SOFT) galaxies. In this paper, the extension of the Hα discs, the shape of the rotation curves, the kinematical asymmetry and the Tully–Fisher relation have been investigated for both ISO and SOFT galaxies. The Hα extension is roughly proportional to R₂₅ for ISO as well as for SOFT galaxies. The smallest extensions of the ionized disc are found for ISO galaxies. The inner slope of the rotation curves is found to be correlated with the central concentration of light more clearly than with the type or the kinematical asymmetry, for ISO as well as for SOFT galaxies. The outer slope of the rotation curves increases with the type and with the kinematical asymmetry for ISO galaxies but shows no special trend for SOFT galaxies. No decreasing rotation curve is found for SOFT galaxies. The asymmetry of the rotation curves is correlated with the morphological type, the luminosity, the  ( B − V )  colour and the maximal rotational velocity of galaxies. Our results show that the brightest, the most massive and the reddest galaxies, which are fast rotators, are the least asymmetric, meaning that they are the most efficient with which to average the mass distribution on the whole disc. Asymmetry in the rotation curves seems to be linked with local star formation, betraying disturbances of the gravitational potential. The Tully–Fisher relation has a smaller slope for ISO than for SOFT galaxies.     

A Hybrid Collocation Method For Calculating Complete Theoretical Seismograms In Vertically Varying Media

A numerical method is presented for calculating complete theoretical seismograms, under the assumption that the earth models have velocity, density and attenuation profiles which are arbitrary piece-wise continuous functions of depth only. Solutions for the stress-displacement vectors in the medium are expanded in terms of orthogonal cylindrical functions. Our method for solving the resulting two-point boundary value problems differs from that of other investigators in three ways. First, collocation is used in traditionally troublesome situations, e.g. for highly evanescent waves, at turning points, and in regions having large gradient in material properties. Second, in some situations (high frequencies and small gradients) P and S -waves decouple and we use a different solution method for each wave type, instead of trying to force a single method to find all solutions. For example, above the P - and S -waves turning points an approximate fundamental matrix may be used for each wave type. At the P -wave turning point, the fundamental matrix may be used for the S -wave components but collocation is used for the P -wave. Between the P - and S -wave turning points collocation is used for the evanescent P -wave and the fundamental matrix is used for the S -wave. At the S -wave turning point and below, collocation is used for both. Third, the computational algorithm chooses the appropriate solution method and depth domain upon which it is employed based upon a specified error tolerance and the known inaccuracies of the various approximations employed. Once solutions of the boundary value problems are obtained, a Fourier—Bessel transform is then applied to get back into the space-time domain.