对流电场、场向电流和极光区电集流变化的地磁响应

对流电场、场向电流和极光区电集流是磁层一电离层耦合的主要物理过程．它们的演化发展时间分别为几分钟至半小时的量级．本文用１００°Ｅ和３００°Ｅ的两个地磁经度链附近各１１个台站的１ｍｉｎ均值地磁Ｈ和Ｚ分量资料,分析了１９９４年４月１６-１７日磁暴期间磁层耦合过程对极光区和中低纬区电离层扰动的地磁特征．强磁暴开始时,台站所处的地方时位置不同,则观测到的电离层和地磁响应也完全不同．这是磁层对流和一、二区场向电流共同作用的结果．一般说,扰时极光区的西向电集流变化更为强烈．随着耦合的发展,极光区范围会向南北扩展,电集流中心带则向低纬侧移动．在中低纬区,二区场向电流的建立能屏蔽一区场向电流所产生的扰动,并引起反向的电流及地磁变化．由此,中低纬区夜间有可能出现短时间的东向电场,又可通过ＥＸＢ的垂直向上漂移作用抬升Ｆ层等离子体,并发生同一经度链附近的多站电离层ｈ＇Ｆ同时突增现象．另一方面,磁赤道附近的台站则更多地受内磁层赤道环电流和电离层赤道电集流的影响．     

WRF模式对弱强迫系统中雷暴预报个例研究

用WRF2．2版本,针对2006年7月13日洛阳市区,发生在副高边缘偏东南暖湿气流中的雷暴进行了模拟预报,结果表明WRF模式能描述弱强迫天气尺度系统中的中小尺度对流系统,能捕捉到常规天气图上难以分辨出来的雷暴单体。模式输出的中尺度要素场可以确定雷暴发生的地点;模式探空的对流有效位能、抬升指数、沙瓦特指数、K指数随时间演变曲线的拐点,能指示雷暴发生的时间。个例分析表明WRF模式在预报弱强迫天气系统雷暴时具有较好的性能,用WRF模式来作雷暴的分析预报早一条可行的徐径。     

自由对流与稳定层结边界层风廓线的解析表达和边界层顶抽吸速度

基于近年来对自由对流和稳定边界层湍流交换特征的研究,求解边界层运动方程,得到这两种层结下边界层风的解析表达式.所得廓线与边界层特性参数符合观测特征.还求出了这二种层结下边界层顶抽吸速度的解析表达及其与某些参数的关系.结果表明,抽吸速度与层结有关,其特征可从物理上加以解释.     

青藏高原一次冰雹强对流天气过程的诊断及雷达回波特征分析

利用青藏高原第三次科学实验的C波段双偏振雷达（C-POL）的观测资料、ERA-Interim 0.125°（纬度）×0.125°（经度）气象再分析资料、常规气象探空资料,对2014年7月30日午后发生在西藏那曲地区的冰雹强对流天气过程进行了天气诊断及雷达回波特征分析。结果表明:1）此次冰雹强对流过程发生在有切变线伴随的高原低涡东移过程中,低涡尾部前倾的切变线为这次冰雹的发生提供了动力、水汽条件。2）强对流天气的水汽输送主要来自从孟加拉湾、印度及尼泊尔翻越喜马拉雅山脉的水汽,强对流发生前水汽输送显著增加,低层水汽集中在400 hPa以下,有明显的辐合及垂直输送。3）那曲400 hPa以下为假相当位温随高度递减区,也是水平辐合及垂直上升运动的重合区,有明显的对流不稳定能量集聚及动力抬升条件。4）雷达回波图上可看到,此次强对流天气主要由局地新生的多个中γ尺度孤立对流单体造成,其移动路径与切变线前西南气流一致。大部分单体水平尺度不大,生命史短,但仍有部分单体强度大,生命史较长。局地气流辐合扰动会导致新的单体产生,单体的发生、发展及维持离不开低层气流辐合提供的动力条件。5）在距离高度显示图上表现出了弱单体雹云特征,雹云云顶伸展至16 km,高于夏季平原地区普遍对流云高度,但未突破对流层顶,0℃层远低于平原地区,为深厚强对流降水;强降水中心位于云团下部,即有降雹也有降水,降雹以霰粒为主;垂直方向存在强烈的入流和上升气流,悬挂回波出现在入流上升气流之上,中层辐合区的气流下沉区对应降雹区;中层辐合区与上层的高空辐散区配合导致对流风暴的垂直增长和强烈发展。     

两种对流参数化方案对辐射能量收支的影响研究

利用中国科学院大气物理研究所大气科学和地球流体力学数值模拟国家重点实验室的格点大气环流模式(GAMIL)1.0版设计了两组数值模拟实验来研究两种不同的对流参数化方案对辐射能量收支的影响.这两种对流参数化方案分别是:Zhang and McFarlance/Hack方案(简称ZM)和Tiedtke/Nordeng方案(简称 TN).对应的数值模拟实验分别取名为EX-ZM和EX-TN.通过对实验结果的分析表明:在对流过程中,EX-ZM允许深对流和浅对流同时发生,因此两种对流同时在模式低层消耗了更多的水汽,释放了更多的潜热,引起了更大的增温;EX_TN每次只允许一种对流发生,也就避免了不同类型的对流在同一层同时消耗水汽的现象.因此对流过后,EX-ZM的环境空气相对湿度较小,而EX-TN周围空气的相对湿度较大,有利于低云云量的生成和大尺度的凝结,因此EX-TN模拟的低云云量偏多,低层的云水含量偏高,模式低层的云光学厚度偏大,这就使得EX_TN中更多的太阳短波辐射通量被云反射掉,严重低估了模式对短波波段的辐射通量的模拟.此外,不同的对流参数化方案通过改变云的长波发射率和降水,进而影响了模式对长波波段的辐射通量、感热和潜热通量的模拟.     

Mountain Waves Launched By Convective Activity Within The Boundary Layer Above Mountains

Mountain waves are observed in the free atmosphere, even when the mountainboundary layer (the source region of these waves) is neutral or convectivelyunstable, and filled with convective rolls, revealed by cloud streets. This paperinvestigates if mountain waves are caused not simply by air flow over mountainridges, but also by flow over boundary-layer convective activity, similar toconvection waves above plains and oceans. Disturbance of stable air flow abovemountains by convective activity, mechanical and convective turbulence and rotors,near the ground, could move the effective mountain-wave launching height to higherthan the mountain peaks.     

苏南5市区雷暴预报方法的研究

对2001-2010年4-9月苏南5市区雷暴天气的对流参数进行了分析、研究.经过对对流参数箱线图统计、计算点双序列相关系数、值域多次分级试验和级间整合调整等优化处理后,最终选取大气可降水量、杰弗逊指数、肖沃特指数、全总指数、风暴强度指数、抬升凝结高度层温度、上下层温差共7个对流参数作为预报因子,建立苏南5市区雷暴的双级逻辑预报方程.利用预报方程,对2001-2009年4-9月的8230个样本进行拟合结果分析:临界成功指数的平均值为61.0％;对2010年4-9月的样本进行试报,苏南5市区7、8月份的临界成功指数分别为75.0％和66.7％,预报效果较好.     

The Influence of the Prandtl Number on the Style of Vigorous Thermal Convection

The effect of the Prandtl number on convection in a planar three-dimensional geometry is investigated in this study. We have employed a numerical scheme to integrate the governing equations. Differently from previous studies we have chosen stress-free boundaries. Experiments have been performed at a Rayleigh number of Ra = 10 6 for Prandtl numbers (Pr) ranging from 0.025 to 100. We have further conducted one experiment in the limiting case of infinite Prandtl number. Despite the differences in the geometry and the boundary conditions, as compared to other studies, we find a similar transition in the dynamics of the flow when the Prandtl number is increased. While the velocity and the temperature structure show diffusive character at low Pr, sharp thermal boundary layers form at high Pr. The heat transport efficiency increases with Pr until a transition value is reached, from there on Nu behaves almost asymptotically. The transition can not be caused by a change in hierarchies between velocity and thermal boundary layers, as suggested in other studies. Due to the stress-free boundaries, a velocity boundary layer does not exist. We observe that the toroidal part of the flow is strong at low Pr and looses its strength with increasing Pr, thus it is likely to be responsible for the transition. In a further chapter we demonstrate that due to the neglect of the toroidal part in two-dimensional calculations at low Pr results are obtained which are misleading, even in a qualitative sense. Infinite Pr results from 2D calculations closely resemble the dynamics of fully 3D flows.     

Linear Magnetoconvection in Rotating Fluid Spheres Permeated by a Uniform Axial Magnetic Field

A linear analysis of thermally driven magnetoconvection is carried out with emphasis on its application to convection in the Earth's core. We consider a rotating and self-gravitating fluid sphere (or spherical shell) permeated by a uniform magnetic field parallel to the spin axis. In rapidly rotating cases, we find that five different convective modes appear as the uniform field is increased; namely, geostrophic, polar convective, magneto-geostrophic, fast magnetostrophic and slow magnetostrophic modes. The polar convective (P) and magneto-geostrophic (E) modes seem to be of geophysical interest. The P mode is characterized by such an axisymmetric meridional circulation that the fluid penetrates the equatorial plane, suggesting that generation of quadrapole from dipole fields could be explained by a linear process. The E mode is characterized by a few axially aligned columnar rolls which are almost two-dimensional due to a modified Proudman-Taylor theorem.     

The effect of time-dependent γ-pumping on buoyant magnetic structures

ABSTRACT

In this paper, we explore for the first time the interactions of the net downward, time-dependent, γ-pumping overlying an imposed layer of magnetic fluid, in a polytropic atmosphere. Our calculations show that an equipartition of energy, between the magnetic and kinetic components, must be reached for buoyancy-driven magnetic structures to rise into the pumping region. However, structures do not rise unhindered, as in a previous investigation. We show that the evolution and other features of the emerging magnetic flux structures are significantly affected by the temporal variation of the γ-pumping. The rate of emerging structures, the strength of magnetic concentrations and the extent to how far magnetic field can travel were all found to depend on the timescale of the γ-pumping.