P-Vector inverse method evaluated using the modular ocean model (MOM)

Several major inverse methods (Stommel-Schott method, Wunsch method, and Bernoulli method) have been successfully developed to quantitatively estimate the geostrophic velocity at the reference level from hydrographic data. No matter the different appeance, they are based on the same dynamical sophistication: geostrophy, hydrostatic, and potential density (ϱ) conservation (Davis, 1978). The current inverse methods are all based on two conservation principles: potential density and potential vorticity (q=f∂ϱ/∂z) and require β-turning. Thus, two necessary conditions can be incorporated into any inverse methods: (1) non-coincidence of potential density and potential vorticity surfaces and (2) existence of vertical turning of the velocity (β-turning). This can be done using the P-Vector, a unit vector in the direction of ▽ϱ×▽q (Chu, 1994, 1995). The first necessary condition becomes the existence of the P-vector, and the second necessary condition leads to the existence of the P-vector turning in the water column. Along this line, we developed the P-vector inverse emthod with a pre-requirement check-up. The method was verified in this study using the Modular Ocean Model (MOM) from Pacanowskiet al. (1991) version of Bryan-Cox-Semtner ocean general circulation model (OGCM), which is based on the work of Bryan (1969). The statistically steady solutions of temperature and salinity from MOM are used as a “no-error data” set for computing absolute geostrophic velocities by the P-vector inverse method. Circulations are similar between the MOM statistically steady solutions and the P-vector solutions. Furthermore, the quantitative analysis shows that this inverse method has capability of picking up the major signal of the velocity field.     

急诊主动脉夹层多层螺旋CT与超声心动图的诊断效果对照分析

目的:对比分析急诊主动脉夹层应用多层螺旋CT和超声心动图诊断的应用价值。方法:选取2014年12月至2016年12月我院收治的经CT血管显像确诊的急诊主动脉夹层患者61例,对所有患者临床治疗进行回顾性分析。所有患者均通过超声心动图检查和多层螺旋CT平扫,对比分析两组诊断结果。结果:所有61例主动脉夹层患者中,总体异常61例,主动脉瓣异常41例,主动脉弓部异常44例,胸、腹主动脉异常45例,冠状动脉异常6例。多层螺旋CT诊断的总体异常、胸、腹主动脉异常以及冠状动脉异常诊断率均为100%,相比于超声心动图的91.8%、86.7%及0.0%更高,差异有统计学意义(P<0.05);两组在主动脉瓣异常、主动脉弓部异常诊断率之间的差异无统计学意义(P>0.05)。结论:超声心动图在诊断主动脉夹层时具有无创性、可重复性,且操作简便,能够对诊断主动脉弓部异常、DebakeyⅠ型主动脉瓣具有较高准确性。而多层螺旋CT相比于超声心动图具有更大优势,可进一步准确诊断胸、腹主动脉分支异常和冠状动脉异常等,具有更高临床诊断价值。      

The generalized energy equation and instability in the two-layer barotropic vortex

The linear two-layer barotropic primitive equations in cylindrical coordinates are used to derive a gen- eralized energy equation, which is subsequently applied to explain the instability of the spiral wave in the model. In the two-layer model, there are not only the generalized barotropic instability and the super high- speed instability, but also some other new instabilities, which fall into the range of the Kelvin-Helmholtz instability and the generalized baroclinic instability, when the upper and lower basic flows are different. They are perhaps the mechanisms of the generation of spiral cloud bands in tropical cyclones as well.     

The evolution of barred spiral galaxies in the Hubble Deep Fields North and South

The frequency of barred spiral galaxies as a function of redshift contains important information on the gravitational influence of stellar discs in their dark matter haloes and may also distinguish between contemporary theories for the origin of galactic bulges. In this paper we present a new quantitative method for determining the strength of barred spiral structure, and verify its robustness to redshift-dependent effects. By combining galaxy samples from the Hubble Deep Field North with newly available data from the Hubble Deep Field South, we are able to define a statistical sample of 46 low-inclination spiral systems with I _814 W<23.2 mag. Analysing the proportion of barred spiral galaxies seen as a function of redshift, we find a significant decline in the fraction of barred spirals with redshift. The redshift distribution of 22 barred and 24 non-barred spirals with suitable inclinations is inconsistent with their being drawn from the same distribution at the 99 per cent confidence level. The physical significance of this effect remains unclear, but several possibilities include dynamically hotter (or increasingly dark-matter-dominated) high-redshift discs, or an enhanced efficiency in bar destruction at high redshifts. By investigating the formation of the 'orthogonal' axis of Hubble's classification tuning fork, our result complements studies of evolution in the early–late sequence, and pushes to later epochs the redshift at which the Hubble classification sequence is observed to be in place.     

Supernova remnants and the spiral structure of the Galaxy

A set of unit clouds of 10⁴ M randomly distributed between 3 and 7 kpc radii, move under the general gravitation of the galactic disk and their mutual gravitation. When the clouds collide they form loose aggregates or giant molecular clouds (GMC). Star formation rate is assumed to be proportional to the mass of the GMC. The more massive stars formed soon turn into supernovae, which in turn break up the GMC back into the unit clouds. After some 350 Myr a steady state is reached, in which the GMCs have a mass spectrum of gradient −1.6, and has the mass-radius relation M ∞ R², both in agreement with the observations. From our simulation we find there should be 775 ± 12 supernova remnants in our galaxy. The existence of spiral arms does not increase the production rate of supernova remnants, but it does make the GMCs to concentrate around them.     

极地低压研究的最新进展(英文)

论述有关发生在高纬度海洋上的极地低压研究的最新进展。不仅涉及观测研究,而且对有关的动力学机制和数值模拟也进行了介绍。因日本海沿岸各国的经济活动越来越活跃,而对发生在日本海上的极地低压进行了专门讨论。     

Chemo-spectrophotometric evolution of spiral galaxies – III. Abundance and colour gradients in discs

We study the relations between luminosity and chemical-abundance profiles of spiral galaxies, using detailed models for the chemical and spectrophotometric evolution of galactic discs. The models are 'calibrated' on the Milky Way disc and are successfully extended to other discs with the help of simple 'scaling' relations, obtained in the framework of semi-analytic models of galaxy formation. We find that our models exhibit oxygen abundance gradients that increase in absolute value with decreasing disc luminosity (when expressed in dex kpc⁻¹) and are independent of disc luminosity (when expressed in dex scalelength⁻¹), both in agreement with observations. We notice an important strong correlation between abundance gradient and disc scalelength. These results support the idea of 'homologous evolution' of galactic discs.     

Constraining the star formation histories of spiral bulges

Stellar populations in spiral bulges are investigated using the Lick system of spectral indices. Long-slit spectroscopic observations of line strengths and kinematics made along the minor axes of four spiral bulges are reported. Comparisons are made between central line strengths in spiral bulges and those in other morphological types [elliptical, spheroidal (Sph) and S0]. The bulges investigated are found to have central line strengths comparable to those of single stellar populations of approximately solar abundance or above. Negative radial gradients are observed in line strengths, similar to those exhibited by elliptical galaxies. The bulge data are also consistent with correlations between Mg₂, Mg₂ gradient and central velocity dispersion observed in elliptical galaxies. In contrast to elliptical galaxies, central line strengths lie within the loci defining the range of 〈Fe〉 and Mg₂ achieved by Worthey's solar abundance ratio, single stellar populations (SSPs). The implication of solar abundance ratios indicates significant differences in the star formation histories of spiral bulges and elliptical galaxies. A 'single zone with infall' model of galactic chemical evolution, using Worthey's SSPs, is used to constrain the possible star formation histories of our sample. We show that the 〈Fe〉, Mg₂ and H β line strengths observed in these bulges cannot be reproduced using primordial collapse models of formation but can be reproduced by models with extended infall of gas and star formation (2–17 Gyr) in the region modelled. One galaxy (NGC 5689) shows a central population with a luminosity-weighted average age of ∼5 Gyr, supporting the idea of extended star formation. Kinematic substructure, possibly associated with a central spike in metallicity, is observed at the centre of the Sa galaxy NGC 3623.