The formation of the Hubble sequence of disc galaxies: the effects of early viscous evolution

We investigate a model of disc galaxies whereby viscous evolution of the gaseous disc drives material inwards to form a protobulge. We start from the standard picture of disc formation through the settling of gas into a dark halo potential well, with the disc initially coming into centrifugal equilibrium with detailed conservation of angular momentum. We derive generic analytic solutions for the disc–halo system after adiabatic compression of the dark halo, with free choice of the input virialized dark halo density profile and of the specific angular momentum distribution. We derive limits on the final density profile of the halo in the central regions. Subsequent viscous evolution of the disc is modelled by a variation of the specific angular momentum distribution of the disc, providing analytic solutions to the final disc structure. The assumption that the viscous evolution time-scale and the star formation time-scale are similar leads to predictions of the properties of the stellar components. Focusing on small 'exponential' bulges, i.e., ones that may be formed through a disc instability, we investigate the relationship between the assumed initial conditions, such as halo 'formation', or assembly, redshift z _f, spin parameter λ , baryonic fraction F , and final disc properties such as global star formation time-scale, gas fraction, and bulge-to-disc ratio. We find that the present properties of discs, such as the scalelength, are compatible with a higher initial formation redshift if the redistribution by viscous evolution is included than if it is ignored. We also quantify the dependence of final disc properties on the ratio F λ , thus including the possibility that the baryonic fraction varies from galaxy to galaxy, as perhaps may be inferred from the observations.     

The stellar populations of spiral galaxies

We have used a large sample of low-inclination spiral galaxies with radially resolved optical and near-infrared photometry to investigate trends in star formation history with radius as a function of galaxy structural parameters. A maximum-likelihood method was used to match all the available photometry of our sample to the colours predicted by stellar population synthesis models. The use of simplistic star formation histories, uncertainties in the stellar population models and considering the importance of dust all compromise the absolute ages and metallicities derived in this work; however, our conclusions are robust in a relative sense. We find that most spiral galaxies have stellar population gradients, in the sense that their inner regions are older and more metal rich than their outer regions. Our main conclusion is that the surface density of a galaxy drives its star formation history, perhaps through a local density dependence in the star formation law. The mass of a galaxy is a less important parameter; the age of a galaxy is relatively unaffected by its mass; however, the metallicity of galaxies depends on both surface density and mass. This suggests that galaxy‐mass-dependent feedback is an important process in the chemical evolution of galaxies. In addition, there is significant cosmic scatter suggesting that mass and density may not be the only parameters affecting the star formation history of a galaxy.     

Spiral galaxy distance indicators based on near-infrared photometry

We compare two methods of distance determination to spiral galaxies using optical/near-infrared (NIR) observations, the ( I − K ) versus M _K colour–absolute magnitude (CM) relation and the I - and K -band Tully–Fisher relation (TFR).
Dust-free colours and NIR absolute magnitudes greatly enhance the usefulness of the NIR CM relation as a distance indicator for moderately to highly inclined spiral galaxies in the field (inclinations between ∼80° and 90°); by avoiding contamination by dust the scatter in the CM relation is significantly reduced, compared with similar galaxy samples published previously. The CM relation can be used to determine distances to field spiral galaxies with M _K >−25.5, to at least M _K ≈−20.
Our results, supplemented with previously published observations for which we can – to some degree – control the effects of extinction, are consistent with a universal nature of the CM relation for field spiral galaxies.
High-resolution observations made with the Hubble Space Telescope can provide a powerful tool to calibrate the relation and extend the useful distance range by more than a factor of 2 compared with ground-based observations.
The intrinsic scatter in the NIR CM relation in the absolute K -band magnitudes is ∼0.5 mag, yielding a lower limit to the accuracy of distance determinations of the order of 25 per cent.
Although we find an unusually low scatter in the TFR (probably a statistical accident), a typical scatter in the TFR would yield distances to our sample galaxies with uncertainties of only ∼15 per cent. However, one of the main advantages of the use of the NIR CM relation is that we need only photometric data to obtain distance estimates; use of the TFR requires additional kinematic data, although it can be used to significantly greater distances.     

天山北坡中部一次强对流风暴的雷达回波特征分析

利用Doppler雷达产品、结合常规观测资料,对2008年7月25日发生在石河子垦区中部、南部强对流天气的雷达回波特征进行了详细分析。结果表明:石河子垦区2008年7月25日强对流风暴发生在西伯利亚至巴尔喀什湖冷槽东南象限的对流不稳定层结中,近低层至地面有中尺度辐合切变线。该强风暴呈现出超级单体螺旋状回波,相应的径向速度图上出现中气旋和中尺度辐合带;冰雹的强回波中心强度达65dBz,60dBz回波顶高达5km、65dBz回波顶高达3km,垂直累积液态含水量由10kg.m-2跃增到75 kg.m-2,暴雨的强回波中心强度为55dBz,55dBz顶高达3.5km,垂直累积液态含水量由15kg.m-2增加到55 kg.m-2;Doppler雷达产品特征对冰雹、暴雨等强对流天气监测预警具有重要的指示意义。     

Energy, angular momentum and wave action associated with density waves in a rotating magnetized gas disc

Both fast and slow magnetohydrodynamic (MHD) density waves propagating in a thin rotating magnetized gas disc are investigated. In the tight-winding or WKBJ regime, the radial variation of MHD density-wave amplitude during wave propagation is governed by the conservation of wave action surface density which travels at a relevant radial group speed C _g. The wave energy surface density and the wave angular momentum surface density are related to by = and = m respectively, where is the angular frequency in an inertial frame of reference and the integer m , proportional to the azimuthal wavenumber, corresponds to the number of spiral arms. Consequently, both wave energy and angular momentum are conserved for spiral MHD density waves. For both fast and slow MHD density waves, net wave energy and angular momentum are carried outward or inward for trailing or leading spirals, respectively. The wave angular momentum flux contains separate contributions from gravity torque, advective transport and magnetic torque. While the gravity torque plays an important role, the latter two can be of comparable magnitudes to the former. Similar to the role of gravity torque, the part of MHD wave angular momentum flux by magnetic torque (in the case of either fast or slow MHD density waves) propagates outward or inward for trailing or leading spirals, respectively. From the perspective of global energetics in a magnetized gas sheet in rotation, trailing spiral structures of MHD density waves are preferred over leading ones. With proper qualifications, the generation and maintenance as well as transport properties of MHD density waves in magnetized spiral galaxies are discussed.     

钢立柱结合旋喷灌浆在处理桥位桩断桩事故中的应用

采用高压旋喷灌浆与四根钢立柱桩相结合的方法处理质量未达要求的观音地桥的横市台2号桩,经承载力计算,可满足设计要求。加之施工中严格控制相关质量,使事故处理圆满成功。     

公路切线渐变加宽的严密公式及其应用

《公路路线设计规范》[1]给出的四级公路超高、加宽缓和段的加宽过渡方式有三角形渐变与近似切线渐变两种。推导了切线渐变加宽的严密公式,并将其应用到含超高、加宽缓和段的圆曲线数字化放样中,实现了道路曲线加桩的数字化放样。     

螺旋CT三维及多平面重建在骨与关节创伤的临床应用

目的:探讨螺旋CT三维(3D)及多平面重建(MPR)在骨与关节创伤的临床应用价值。方法:对65例骨与关节创伤患者行螺旋CT容积扫描,应用MPR及3D重建技术进行图像重建,对各种MPR及3D重建图像进行观察和分析,并与手术所见相对照。结果:螺旋CTMPR及3D重建图像能全面、直观地显示骨折线、关节脱位、关节内及椎管内骨碎片移位情况,术后重建图像能清晰显示骨折内固定物的形态、位置及骨折复位情况,螺旋CT3D图像与手术中骨科医生所见一致。结论:螺旋CTMPR及3D重建作为轴位图像的重要补充,能立体、直观地显示骨折的情况,是一种快速无创伤性显示骨与关节创伤的最佳方法,为制定手术方案提供可靠依据。