DIAGNOSTIC ANALYSIS OF ASYMMETRIC SPIRAL RAINBANDS AROUND THE LANDING OF TYPHOON HAITANG (2005)

By using WRF mesoscale model, this paper carries out a numerical simulation and diagnostic analysis of the structural characteristics of the asymmetric spiral rain bands around the landing of Typhoon Haitang during the period of July 19 to 20, 2005. The result indicated that the two rainbands associated with the precipitation centre was mainly located northeast of the typhoon centre. The movement and intensity of the southern rainband corresponded well with the 850-hPa positive vorticity band from 0200 to 1800 UTC July 19, 2005. Under the effect of cyclonic circulation, the positive vorticity band at 850 hPa connected with a southern rain band, leading to the intensification of rainfall in the southern centre of the precipitation. The southward rainband gradually moved toward and then merges with the northward one, strengthening the rainfall in the northern centre of the precipitation. Besides, the relationship between the heavy rainfall and the divergence field of vertical shear wind in the high altitude is analyzed. Finally, the relationship is revealed between the development of the vertical component of convective vorticity vector and the rainfall near the two centres of precipitation in the low altitude.     

Dust attenuation in starburst galaxies determined by measuring the dependence of the optical color indices on galaxy inclination

We use optical color indices (colors) from the SDSS database to study the effect of dust in starburst galaxies by mea‐suring the dependence of colors on galaxy inclination. Starburst galaxies with ongoing star formation, are rich with metals/dust and are, therefore, an excellent objects for studying the effect of dust in galaxies. They are selected using the [O III ]λ 5007/Hα vs. [N II ]λ 6584/Hβ diagram, that is, the BPT‐diagram. We use Kauffmann's empirical demarcation line in the BPT‐diagram to exclude galaxies with active galactic nuclei (AGN) from the sample because they have different physical and dust properties from normal galaxies. The sample is divided into bins according to galaxy stellar mass and 4000 Å break (which is a coarse measure of a galaxy star formation history; SFH) and the reddening with inclination is studied as a function of these two physical parameters. Assuming that the dust effect is negligible in the SDSS z ‐band, we derive the attenuation curves for these galaxies. We fit the attenuation curves with a simple power law and use power law index to interpret the relative distribution of dust and stars in the starburst galaxies (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Study of star formation in NGC 1084

We present UBVRI broad-band, Hα narrow-band photometry of the star-forming complexes in the infrared bright galaxy NGC 1084. Results of medium-resolution spectroscopy of some of the brighter complexes are also discussed. Spectroscopic data are used to better estimate the internal reddening within the galaxy which is found to be highly variable and to calculate metallicity which is close to the solar value. A diagnostic diagram identifies the shocked regions within this galaxy. The narrow-band Hα flux and its equivalent width are used to determine the star formation rates of the complexes and the distribution of ages. Star formation rates for a few of the complexes are found to be as high as  0.5 M_⊙ yr⁻¹  . The star-forming complexes lie in the age range 3 to 6.5 Myr. A U − B versus V − I colour–colour mixed population model created using the Starburst99 model colours is used to estimate the ages of the stellar populations present within these regions. Using this technique, it is found that the star formation in NGC 1084 has taken place in a series of short bursts over the last 40 Myr or so. It is proposed that the likely trigger for enhanced star formation is merger with a gas-rich dwarf galaxy.     

The AGNS and their host galaxies as seen in the mid-infrared

We present a new diagnostic diagram based on ISOCAMspectra (5-16 m) to distinguish the emission inducedby the active galactic nucleus (AGN) from that associated with thestar formation activity. This diagnostic based on the mid-IRcontinuum and the Unidentified Infrared Band (UIB) intensity allowsus to estimate the relative importance of the three components (HIIregions, diffuse/photo-dissociation regions (PDRs), and AGN) contained ingalaxy mid-infrared emission. In AGN spectra, we confirm the absenceof UIBs presumably photodissociated by the X-UV radiation field. Inaddition, a non-negligible continuum below 9 m commonlyassociated with emission from hot dust is present in AGNs. Adiagnostic diagram derived from these two results can be used fordetecting obscured AGNs embedded in a large concentration of dust.     

线路坐标计算的通用模型

介绍了一种适合电算的线路坐标计算通用模型.首先,引入了曲线元的概念,使线路的平面线形三要素(直线、圆曲线、缓和曲线)得到了统一.然后,以曲线元作为组成线路的最小单元,推导了线路坐标计算的通用数学模型.该模型形式简单,易于编程实现.不但能解算S型、卵型、复合型、C型等复杂组合线形的任意指定点的坐标,而且能将线路中桩、边桩以及与线路非正交交叉的特殊点位(如桥墩、电线杆等)的坐标解算统一了起来.     

大气涡旋的螺旋结构

利用速度场的分解,说明大气中常见的斑图.速度场可分为变形场和旋转场.若大气动力学方程中只有气压梯度力和科里奥利力平衡,此时速度场只有旋转场,地面天气图上气旋反气旋斑图是闭合的.若再加上摩擦力,则斑图为实际的气旋反气旋螺旋.对三维有水平辐散辐合的涡旋,其斑图为三维螺旋型式,常见是漏斗状.台风小口朝上,龙卷风大口朝上.     

线路坐标计算的通用模型

介绍了一种适合电算的线路坐标计算通用模型。首先,引入了曲线元的概念,使线路的平面线形三要素(直线、圆曲线、缓和曲线)得到了统一。然后,以曲线元作为组成线路的最小单元,推导了线路坐标计算的通用数学模型。该模型形式简单,易于编程实现。不但能解算S型、卵型、复合型、C型等复杂组合线形的任意指定点的坐标,而且能将线路中桩、边桩以及与线路非正交交叉的特殊点位(如桥墩、电线杆等)的坐标解算统一了起来。     

Weighing a galaxy bar in the lens Q2237 +=0305

In the gravitational lens system Q2237+0305 the cruciform quasar image geometry is twisted by 10c by the lens effect of a bar in the lensing galaxy. This effect can be used to measure the mass of the bar. We construct a new lensing model for this system with a power-law elliptical bulge and a Ferrers bar. The observed ellipticity of the optical isophotes of the galaxy leads to a nearly isothermal elliptical profile for the bulge, with a total quasar magnification of 16⁺⁵₋₄. We measure a bar mass of (7.5 ∼ 1.5) −10⁸ h ⁻¹₇₅ M⊙ in the region inside the quasar images.