Kinematic properties and stellar populations of faint early-type galaxies – I. Velocity dispersion measurements of central Coma galaxies     

A. Matkovi&#;  R. Guzmán 《Monthly notices of the Royal Astronomical Society》2005,362(1):289-300

We present velocity dispersion measurements for 69 faint early-type galaxies in the core of the Coma cluster, spanning  −22.0 ≲ M_R ≲−17.5 mag  . We examine the   L –σ  relation for our sample and compare it to that of bright elliptical galaxies (Es) from the literature. The distribution of the the faint early-type galaxies in the   L –σ  plane follows the relation   L ∝σ^2.01±0.36  , which is significantly shallower from   L ∝σ⁴  as defined for the bright Es. While increased rotational support for fainter early-type galaxies could account for some of the difference in slope, we show that it cannot explain it. We also investigate the colour–σ relation for our Coma galaxies. Using the scatter in this relation, we constrain the range of galaxy ages as a function of their formation epoch for different formation scenarios. Assuming a strong coordination in the formation epoch of faint early-type systems in Coma, we find that most had to be formed at least 6 Gyr ago and over a short 1-Gyr period.  相似文献   

A three-dimensional model of moist convection for the giant planets II: Saturn's water and ammonia moist convective storms     

Ricardo Hueso  Agustín Sánchez-Lavega 《Icarus》2004,172(1):255-271

Moist convective storms constitute a key aspect in the global energy budget of the atmospheres of the giant planets. Among them, Saturn is known to develop the largest scale convective storms in the Solar System, the Great White Spots (GWS) which occur rarely and have been detected once every 30 years approximately. On the average, Saturn seems to show much less convective storms than Jupiter with smaller size and reduced frequency and intensity. Here we present detailed simulations of the onset and development of storms at the Equator and mid-latitudes of Saturn. These are the regions where most of the recent convective activity of the planet has been observed. We use a 3D anelastic model with parameterized microphysics (Hueso and Sánchez-Lavega, 2001, Icarus 151, 257) studying the onset and evolution of water and ammonia moist convective storms up to sizes of a few hundred km. Water storms, while more difficult to initiate than in Jupiter, can be very energetic, arriving to the 150 mbar level and developing vertical velocities on the order of 150 m s⁻¹. Ammonia storms develop easier but with a much smaller intensity unless very large abundances of ammonia (10 times solar) are present in Saturn's atmosphere. The Coriolis forces play a major role in the morphology and properties of water based storms.  相似文献   

On the origin of red giant depletion through low-velocity collisions     

Tim Adams  Melvyn B. Davies  Alison Sills 《Monthly notices of the Royal Astronomical Society》2004,348(2):469-481

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Effect of property variation and modelling on convection in a fluid overlying a porous layer     

B. Straughan 《国际地质力学数值与分析法杂志》2002,26(1):75-97

An accurate computational analysis is presented for the onset of thermal convection in a two‐layer system which is comprised of a saturated layer of porous material described by Darcy's law, over which lies a layer of the same saturating fluid. The two‐layer system is heated from below and the upper (fluid) surface is allowed to be fixed or stress free. The onset of convection may have a bi‐modal nature in which convection may be dominated by the porous medium or by the fluid depending on the depths of the relative layers, but this is strongly controlled by material parameters. The effect of variation of relevant fluid and porous material properties is investigated in detail, as is the effect of the interface boundary condition between the fluid and the porous medium. Copyright © 2001 John Wiley & Sons, Ltd.  相似文献   

Cuspy dark matter haloes and the Galaxy     

J.J. Binney  N.W. Evans 《Monthly notices of the Royal Astronomical Society》2001,327(2):L27-L31

The microlensing optical depth to Baade's Window constrains the minimum total mass in baryonic matter within the Solar circle to be greater than ∼     , assuming the inner Galaxy is barred with viewing angle ∼20°. From the kinematics of solar neighbourhood stars, the local surface density of dark matter is ∼     . We construct cuspy haloes normalized to the local dark matter density and calculate the circular-speed curve of the halo in the inner Galaxy. This is added in quadrature to the rotation curve provided by the stellar and ISM discs, together with a bar sufficiently massive so that the baryonic matter in the inner Galaxy reproduces the microlensing optical depth. Such models violate the observational constraint provided by the tangent-velocity data in the inner Galaxy (typically at radii     . The high baryonic contribution required by the microlensing is consistent with implications from hydrodynamical modelling and the pattern speed of the Galactic bar. We conclude that the cuspy haloes favoured by the cold dark matter cosmology (and its variants) are inconsistent with the observational data on the Galaxy.  相似文献   

A SAURON study of M32: measuring the intrinsic flattening and the central black hole mass     

E. K. Verolme  M. Cappellari  Y. Copin  R. P. van der Marel  R. Bacon  M. Bureau    R. L. Davies  B. M. Miller  P. T. de Zeeuw 《Monthly notices of the Royal Astronomical Society》2002,335(3):517-525

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中国大陆东南边缘海现时地壳运动与地震动力学综合研究   总被引：3，自引：3，他引：0  

周硕愚  吴云  施顺英  杨福平 《大地测量与地球动力学》2001,21(1):1-14

在东亚大陆动力学和西太平洋动力学背景下 ,定量研究中国大陆东南边缘海的现今区域地壳运动、动力学及地震危险性。基于 1994～ 1998年福建 -台北网、中国大陆网、台湾 -吕宋 (菲律宾 )网和东亚大陆及西太平洋的 IGS网等 4种不同空间尺度的 GPS测量结果 ,结合近 10 0年来的强震震源机制解、近 2 0余年来跨断层形变网、精密水准网、激光测距网及原地应力测量等结果 ,以及地球物理数值模拟与地质学成果 ,通过对多层次构造运动的分析、多学科结果的互验互补和整体综合研究 ,获得如下结果 :( 1)本研究区同时存在陆、海相互对进的两种地壳水平运动 :大陆东南沿海 11～ 12 mm/ a向东南、海洋对大陆 3mm/ a向西北以及台湾东海岸 53mm/ a向西北的运动 ;( 2 )台湾岛可能存在着以 2 4°N附近为其旋转轴的右旋运动 ;( 3) GPS和地形变测量求出现今区域应力场主压应力方向为 NW( NWW)向 ,与不同时间尺度的地震学和地质学结果一致 ;( 4 )观测与数值模拟共同证实 ,印度板块和菲律宾海板块对欧亚板块的联合动力作用是导致本区上述地壳运动的原因 ;前者导致的地壳运动速度比后者约大 4倍 ,但前者仅导致准均匀场 ,而后者则可产生变形局部化过程的非均匀场 ,从而为强震孕育提供动力 ;( 5)菲律宾海板块在台湾东侧对欧亚板块  相似文献   

Modelling line profiles in infalling cores     

J.M.C. Rawlings  J.A. Yates 《Monthly notices of the Royal Astronomical Society》2001,326(4):1423-1430

Results are presented from a model of molecular line formation in collapsing star-forming cores. The study includes, for the first time, a self-consistent chemical and dynamical model which is then directly coupled to an appropriate radiative transfer model. The assumptions of chemical uniformity or simple monotonic variations within such cores are shown to be unacceptable. The results show that the abundance variations and the line profiles are highly sensitive to the assumed values of the free parameters in the chemical model. Extreme caution is therefore advised in the quantitative analysis of emission-line profiles from infall sources. The implied degeneracy can be overcome by multiple line-of-sight observations of many species and transitions.  相似文献   

Hydrodynamics of photoionized columns in the Eagle Nebula, M 16     

R.J.R. Williams  D. Ward-Thompson  A.P. Whitworth 《Monthly notices of the Royal Astronomical Society》2001,327(3):788-798

We present hydrodynamical simulations of the formation, structure and evolution of photoionized columns, with parameters based on those observed in the Eagle Nebula. On the basis of these simulations we argue that there is no unequivocal evidence that the dense neutral clumps at heads of the columns were cores in the pre-existing molecular cloud. In our simulations, a variety of initial conditions leads to the formation and maintenance of near-equilibrium columns. Therefore, it is likely that narrow columns will often occur in regions with large-scale inhomogeneities, but that observations of such columns can tell us little about the processes by which they formed. The manner in which the columns in our simulations develop suggests that their evolution may result in extended sequences of radiation-induced star formation.  相似文献   

ON THE BEHAVIORS OF OCEAN BOTTOM EDDY     

吴德星  冯土 《中国海洋湖沼学报》1994,12(4):343-350

On the basis of scaling analysis,this paper presents a frontal geostrophic dynamic system which canbe used to describe the dynamics of an isolated bottom eddy and shows that five possible dynamicsubregimes are included in the system.A particle-in-cell method is used to investigate the behavior of the eddy in the two dynamic subregimes,with 1)nonlinear effect(ε)relevant to the sloping bottom-inducedbeta effect(β_1)and 2)seamount-induced beta effect(β_2)dominant.In the dynamic subregime of β_1～ ε～10~(-2)and β_2=0,the eddy can keep as a whole for a long time and migrates for a long distance.Inthe dynamic subregime where the seamount-induced beta effect (β_2～10~(-1))is dominant,the seamounttraps the water particles,causing the eddy to break up into a discrete set of eddies moving around the seamount.  相似文献