3-D BAROCLINIC NUMERICAL SIMULATION OF THE SOUTH CHINA SEA I. UPPER CIRCULATION     

蔡树群甘子钧  刘秦玉 《中国海洋湖沼学报》2001,19(3):208-216

A three-dimensional baroclinic shelf sea model was employed to simulate the seasonal characteristics of the South China Sea (SCS) upper circulation. The results showed that: in summer, an anticyclonic eddy, after its formation between the Bashi Channel and Dongsha Islands in the northeastern SCS, moves southwestward until it disperses slowly. There exists a northward western boundary current along the east shore of the Indo-China Peninsula in the western SCS and an anticyclonic gyre in the southern SCS. But at the end of summer and beginning of autumn, a weak local cyclonic eddy forms in the Nansha Trough, then grows slowly and moves westward till it becomes a cyclonic gyre in the southern SCS in autumn. At the beginning of winter, there exists a cyclonic gyre in the northern and southern SCS, and there is a southward western boundary current along the east shore of the Indo-China Peninsula. But at the end of winter, an anticyclonic eddy grows and moves toward the western boundary after forming in the Nansha Trough. The eddy‘s movement induces a new opposite sign eddy on its eastern side, while the strength of the southward western boundary current gets weakened. This phenomenon continues till spring and causes eddies in the southern SCS.  相似文献   

Including star formation and supernova feedback within cosmological simulations of galaxy formation   总被引：1，自引：0，他引：1  

Scott T.Kay  Frazer R.Pearce  Carlos S.Frenk  AdrianJenkins 《Monthly notices of the Royal Astronomical Society》2002,330(1):113-128

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An iterative technique for solving equations of statistical equilibrium   总被引：3，自引：0，他引：3  

L.B. Lucy 《Monthly notices of the Royal Astronomical Society》2001,326(1):95-101

Superlevel partitioning is combined with a simple relaxation procedure to construct an iterative technique for solving equations of statistical equilibrium. In treating an N -level model atom, the technique avoids the N ³ scaling in computer time for direct solutions with standard linear equation routines and also does not fail at large N due to the accumulation of round-off errors. As a consequence, the technique allows detailed model atoms with N ≳10³ , such as those required for iron peak elements, to be incorporated into diagnostic codes for analysing astronomical spectra. Tests are reported for a 394-level Fe  ii ion and a 1266-level Ni  i – iv atom.  相似文献   

EFFECTS OF DIETARY LEVELS OFCARBOHYDRATE,LIPID,PHOSPHORUS ANDZINC ON THE GROWTH,FEED CONVERSIONAND PROTEIN EFFICIENCY RATIO OF NILETILAPIA (OREOCHROMIS NILOTICUS)     

李钟杰  雷武  杨云霞  叶军 《中国海洋湖沼学报》1993,(3)

INTRODUCTION The eonversion of dietary Protein,liPid and earbohydrate in the body of thevertebrate 15 conneeted with the intermediate metabolism Proeesses in whieh themetalloenzymes Play very imPortant roles.Anderson et al.(1984)and Teshimaand Kanazawa(1 986)Proved the maintenanee of ProPer Protein and liPidlevelsin the diets eoneomitant with inereasing the dietary earbohydrate eontent to 40%ean Promote teh growth of Nile tilaPia fingerlings.EI一Sayed and Garling(1988)indi eated th…  相似文献   

The 2dF Galaxy Redshift Survey: luminosity dependence of galaxy clustering     

Peder Norberg  Carlton M. Baugh  Ed Hawkins  Steve Maddox  John A. Peacock  Shaun Cole  Carlos S. Frenk  Joss Bland-Hawthorn  Terry Bridges  Russell Cannon  Matthew Colless  Chris Collins  Warrick Couch  Gavin Dalton  Roberto De Propris  Simon P. Driver  George Efstathiou  Richard S. Ellis  Karl Glazebrook  Carole Jackson  Ofer Lahav  Ian Lewis  Stuart Lumsden  Darren Madgwick  Bruce A. Peterson  Will Sutherland  Keith Taylor 《Monthly notices of the Royal Astronomical Society》2001,328(1):64-70

We investigate the dependence of the strength of galaxy clustering on intrinsic luminosity using the Anglo-Australian two degree field galaxy redshift survey (2dFGRS). The 2dFGRS is over an order of magnitude larger than previous redshift surveys used to address this issue. We measure the projected two-point correlation function of galaxies in a series of volume-limited samples. The projected correlation function is free from any distortion of the clustering pattern induced by peculiar motions and is well described by a power law in pair separation over the range     . The clustering of     galaxies in real space is well-fitted by a correlation length     and power-law slope     . The clustering amplitude increases slowly with absolute magnitude for galaxies fainter than M *, but rises more strongly at higher luminosities. At low luminosities, our results agree with measurements from the Southern Sky Redshift Survey 2 by Benoist et al. However, we find a weaker dependence of clustering strength on luminosity at the highest luminosities. The correlation function amplitude increases by a factor of 4.0 between     and −22.5, and the most luminous galaxies are 3.0 times more strongly clustered than L * galaxies. The power-law slope of the correlation function shows remarkably little variation for samples spanning a factor of 20 in luminosity. Our measurements are in very good agreement with the predictions of the hierarchical galaxy formation models of Benson et al.  相似文献   

Morphology, photometry and kinematics of N-body bars – I. Three models with different halo central concentrations     

E.Athanassoula  A.Misiriotis 《Monthly notices of the Royal Astronomical Society》2002,330(1):35-52

We discuss the morphology, photometry and kinematics of the bars which have formed in three N -body simulations. These have initially the same disc and the same halo-to-disc mass ratio, but their haloes have very different central concentrations. The third model includes a bulge. The bar in the model with the centrally concentrated halo (model MH) is much stronger, longer and thinner than the bar in the model with the less centrally concentrated halo (model MD). Its shape, when viewed side-on, evolves from boxy to peanut and then to 'X'-shaped, as opposed to that of model MD, which stays boxy. The projected density profiles obtained from cuts along the bar major axis, for both the face-on and the edge-on views, show a flat part, as opposed to those of model MD which are falling rapidly. A Fourier analysis of the face-on density distribution of model MH shows very large  m=2  , 4, 6 and 8 components. Contrary to this, for model MD the components  m=6  and 8 are negligible. The velocity field of model MH shows strong deviations from axial symmetry, and in particular has wavy isovelocities near the end of the bar when viewed along the bar minor axis. When viewed edge-on, it shows cylindrical rotation, which the MD model does not. The properties of the bar of the model with a bulge and a non-centrally concentrated halo (MDB) are intermediate between those of the bars of the other two models. All three models exhibit a lot of inflow of the disc material during their evolution, so that by the end of the simulations the disc dominates over the halo in the inner parts, even for model MH, for which the halo and disc contributions were initially comparable in that region.  相似文献   

绝热非径向太阳振动的数值计算方法     

毕少兰  李如凤 《中国天文和天体物理学报》1996,(2)

本文采用改进后的平行Shooting方法，即连续正交归一化方法，通过增加系统的秩和把微分方程从线性变成非线性的方法，使得病态方程变成非病态方程，克服了平行Shooting方法（不连续正交归一化方法）的主要困难：一是选择径向网格点数目的问题，如果被检验振动模的径向节点数大或小，所需要的网格点数则多或少；二是在远离阈值的时候，尚未有合适的方法提高计算精度的问题．数值计算出了标准太阳模型的绝热非径向太阳振动的理论本征频率谱．从数值计算的结果发现改进后的平行Shooting方法比线性化的Henyey方法和平行Shooting方法收敛性更好且精度更高．其误差可以达到1％的精度．  相似文献   

空间无碰撞激波的数值研究   总被引：2，自引：0，他引：2  

王水  陆全明 《天文学进展》1997,15(3):218-230

无碰撞激波是空间等离子体和宇宙等离子体中的重要物理现象。文中评述了数值研究空间无碰撞激波的两种方法－粒子模拟和混合模拟，给出了准垂直和准平行无碰撞激波的数值研究结果。还指出了一些尚未解决的研究问题。  相似文献   

Advances in Numerical Modeling of Astrophysical and Space Plasmas     

Anthony L. Peratt 《Astrophysics and Space Science》1997,256(1-2):51-75

Advances in the simulation of astrophysical and cosmic plasmas are the direct result of advances in computational capabilities, today consisting of new techniques such as multilevel concurrent simulation, multi-teraflop computational platforms and experimental facilities for producing and diagnosing plasmas under extreme conditions for the benchmarking of simulations. Examples of these are the treatment of mesoscalic plasma and the scaling to astrophysical and cosmic dimensions and the Accelerated Strategic Computing Initiative whose goal is to construct petaflop (10¹⁵ floating operations per second) computers, and pulsed power and laser inertial confinement plasmas where megajoules of energy are delivered to highly-diagnosed plasmas. This paper concentrates on the achievements to date in simulating and experimentally producing plasmas scaled to both astrophysical and cosmic plasma dimensions. A previous paper (Part I, Peratt, 1997) outlines the algorithms and computational growth.  相似文献   

Torsional oscillations of magnetized relativistic stars     

Neophytos Messios  Demetrios B. Papadopoulos  Nikolaos Stergioulas 《Monthly notices of the Royal Astronomical Society》2001,328(4):1161-1168

Strong magnetic fields in relativistic stars can be a cause of crust fracturing, resulting in the excitation of global torsional oscillations. Such oscillations could become observable in gravitational waves or in high-energy radiation, thus becoming a tool for probing the equation of state of relativistic stars. As the eigenfrequency of torsional oscillation modes is affected by the presence of a strong magnetic field, we study torsional modes in magnetized relativistic stars. We derive the linearized perturbation equations that govern torsional oscillations coupled to the oscillations of a magnetic field, when variations in the metric are neglected (Cowling approximation). The oscillations are described by a single two-dimensional wave equation, which can be solved as a boundary-value problem to obtain eigenfrequencies. We find that, in the non-magnetized case, typical oscillation periods of the fundamental     torsional modes can be nearly a factor of 2 larger for relativistic stars than previously computed in the Newtonian limit. For magnetized stars, we show that the influence of the magnetic field is highly dependent on the assumed magnetic field configuration, and simple estimates obtained previously in the literature cannot be used for identifying normal modes observationally.  相似文献