The morphology of galactic rings exterior to evolving bars: test-particle simulations

The morphology of the outer rings of early-type spiral galaxies is compared to integrations of massless collisionless particles initially in nearly circular orbits. Particles are perturbed by a quadrupolar gravitational potential corresponding to a growing and secularly evolving bar. We find that outer rings with R1R2 morphology and pseudo-rings are exhibited by the simulations even though they lack gaseous dissipation. Simulations with stronger bars form pseudo-rings earlier and more quickly than those with weaker bars. We find that the R1 ring, perpendicular to the bar, is fragile and dissolves after a few bar rotation periods if the bar pattern speed increases by more than ∼8 per cent, bar strength increases (by ≳140 per cent) after bar growth or the bar is too strong  ( Q_T > 0.3)  . If the bar slows down after formation, pseudo-ring morphology persists and the R2 ring perpendicular to the bar is populated due to resonance capture. The R2 ring remains misaligned with the bar and increases in ellipticity as the bar slows down. The R2 ring becomes scalloped and does not resemble any ringed galaxies if the bar slows down more than 3.5 per cent suggesting that bars decrease in strength before they slow down this much. We compare the morphology of our simulations to B -band images of nine ringed galaxies from the Ohio State University Bright Spiral Galaxy Survey, and we find a reasonable match in morphologies to R1R2' pseudo-rings seen within a few bar rotation periods of bar formation. Some of the features previously interpreted in terms of dissipative models may be due to transient structure associated with recent bar growth and evolution.     

The Color-Magnitude Relations of Late-type Spiral Galaxies and Their Disks

The 395 late-type spiral galaxies brighter than 15^m in r-band are selected from the Data Release 2 of Sloan Digital Sky Survey and the colormagnitude relations of these galaxies and their disks are investigated. It is found that the colors g − r, r − z and g − z of these galaxies and their disks are strongly correlated with the r-band absolute magnitudes, i.e., the more luminous galaxies (or disks) have the redder colors than the less luminous galaxies (or disks). And the correlation of galaxies is stronger than that of their disks.     

山东省一次冰雹云过程的数值模拟

利用中国气象科学研究院的三维对流云模式,对发生在山东省的一次强降雹天气过程进行了数值模拟,并将模拟结果与雷达观测资料进行了检验.分析了风暴各发展阶段的流场结构和回波结构特征及微观物理量的分布及其演变.结果表明:雹胚源区出现在主上升气流前侧上升气流向辐散下沉气流的转向处,在垂直方向上位于最大上升速度上方;冰晶碰并过冷水形成霰和冰雹,冰雹粒子在气流循环处生长.研究结果对实际防雹业务有一定参考意义.     

Inertia and diurnal oscillations of Ekman layers in atmosphere and ocean

A 1D model, including a time variation of eddy viscosity and mixed layer depth, is applied to study Ekman spirals. It simulates a weak velocity in the atmosphere but a jet in the upper oceanic mixed layer during daytime; and a strong velocity in the atmosphere but a weak, uniform velocity in the ocean at night. The mean spirals in both atmosphere and ocean are close to the average spirals at midday and midnight, they are not flat as suggested by previous studies but consistent with the observations of Polton et al (2013). Our results also show shorter length scale for magnitude decay than for rotation of mean velocity as observed in the ocean, which comes from the combined effects of the diurnal variation of PBL and the Coriolis force. The latter becomes more important away from the surface. In the upper oceanic mixed layer, the mean velocity mainly comes from the strong jets in the late afternoon and early evening. Near and below the depth of Ekman depth, the weak velocities change with time and cancel out each other if averaged timing is longer than the inertia period. It results in diminishing of magnitude of the mean velocity, but the amplitude of individual parcel oscillating can still be quite large near the Ekman depth. Meanwhile, the change of velocity angle from the surface is near or less than 90 degree. Hence, shorter length scale for magnitude decay than for rotation of the mean velocity is not controlled by viscosity alone. Meanwhile, the model does not need two viscosities as suggested previously.The results also show that either the diurnal variation of surface stress or eddy viscosity alone can create a diurnal oscillation of velocity in the ocean. The interactions between PBL force and the Coriolis force can create a weak instability in the atmosphere and ocean at 30° and 90°. This weak instability may explain the observed nocturnal LLJ near 30 °N on the lee of the Rocky Mountains and the intensification of mesoscale circulation simulated by Sun and Wu (1992).     

一种转阀换向的液压双缸单作用往复泵设计

为解决往复泵恒压力恒流量输出问题,设计了一种液压双缸单作用泵。其液压系统由双油泵供油,采用带单向机构的转阀与普通换向阀相结合的油量分配方式,转阀动作由活塞行程控制,转阀动作精度不受主油泵变量的影响,系统控制可靠。该泵在实际应用中取得了良好的效果。     

几种岛状硅酸盐矿物的形貌学研究

测量研究了锆石、黄石、石榴石、羟硅铍石和符山石的形态和微形貌，并分别列出了这些晶体的化学成分和其它鉴定参数，观察到的生长和溶蚀螺纹证实螺旋生长机制在硅酸盐矿物晶体生长中具有重要意义。     

一次路径偏北南折的秋季江淮气旋成因分析

2015年11月5—8日发生的一次江淮气旋具有与以往过程不同的特征,发生时间晚、路径偏北东移、途经山东半岛后又南折,导致山东半岛连续降水36 h,降水时段内累积降水量最大接近50 mm。为揭示上述特点的成因,利用FNL（Final Analysis Data of Global Forecast System）再分析数据进行了天气形势分析,结果表明：副热带高压位置偏北且强度较强是导致气旋过程发生时间偏晚、路径偏北东移的重要原因,而副热带高压的异常变化与2015年强厄尔尼诺事件有很强的关联性。借助WRF（Weather Research and Forecasting）数值试验探究了气旋过程路径偏北又南折的原因,发现：1）黄海的高海温有利于海面水汽通量向上输送,积云对流加强,潜热释放促进江淮气旋增强发展;高空西南气流对增强气旋的控制较弱,导致气旋没有一直向北移动,中途发生南折。2）黄海南部海温较北部偏高约4 ℃,低空大气南、北部之间形成的能量锋区对江淮气旋的南折有指向作用;同时对流层低层偏北风的存在以及副热带高压的短时南撤为气旋的南折提供了动力环境。