北京奥运会开幕式期间的中尺度天气系统研究

利用北京地区稠密的地面观测网资料以及北京市观象台、海淀、上甸子3部风廓线仪的观测资料,通过分析2008年8月8日北京奥运会开幕式期间发生在北京地区的降水过程,讨论了此次过程中在环境风场、地形和城市热岛作用下,中尺度系统发展或减弱的可能机制及对城区降水的影响。结果表明:城市热岛和地形作用形成的次级环流圈对城区南北两侧的影响不同,在城区南侧,次级环流圈使南风减弱,同时受次级环流圈下沉气流影响,中尺度系统北上时会减弱;在城区北侧,次级环流圈使南风加强,中尺度系统南下时会使气流辐合增强,有利于中尺度系统发展。当环境风场是较弱的偏南风时,城市热岛-地形次级环流圈在城区1500 m以下形成辐合,以上辐散,在3000 m左右辐散最强,不利于北上的中尺度系统向城区发展形成降水。     

Effects of vertical wind shear on convective development during a landfall of severe tropical storm Bilis (2006)

Effects of vertical wind shear on convective development during the landfall of tropical storm Bilis (2006) are investigated with a pair of sensitivity experiments using a two-dimensional cloud-resolving model. The validated simulation data from Wang et al. [Wang, D., Li, X., Tao, W.-K., Liu, Y., Zhou, H., 2009: Torrential rainfall processes associated with a landfall of severe tropical storm Bilis (2006): A two-dimensional cloud-resolving modeling study. Atmos. Res., 91, 94–104.] are used as the control experiment. The difference between the control and sensitivity experiments is that vertically varying zonal winds in the control experiment are replaced by their mass-weighted means in the sensitivity experiment. The imposed vertical velocity with ascending motion in the upper troposphere and descending motion in the lower troposphere is responsible for dominant stratiform rainfall on 15 July. The vertical wind shear does not have important impacts on development of stratiform rainfall. One day later, imposed upward motion extends to the lower troposphere. The inclusion of negative vertical wind shear produces well-organized convection and strong convective rainfall because it causes kinetic energy transfer from large-scale forcing to perturbation circulations.     

达坂城1961—2008年来风的气候特征及风能现状分析

分析了达坂城气象站1961--2008年风的气候特征及48a来风速最小年2008年的风能参数。结果表明：达坂城一日之中17—18时风速最大,07-08时最小;一年之中4—5月风速最大,9—10月最小;风速变化分4个阶段,其中1986--2008年风速呈减小趋势,特别是2000年以来风速明显偏小,2008年出现了近48a来的最低值;一年之中以4-9月风速减小最为显著。2008年的风能参数达到了“风能较丰富”的指标,近期为风能资源偏少时期,特别是夏半年风能偏弱。     

Viscous flow properties in the transport of solar wind momentum to the Venus upper ionosphere

A comparative study of the viscous transport of solar wind momentum to the upper layers of the Venus ionosphere with that occurring within the trans-terminator flow leads to estimates of the ratio of the viscosity coefficients that are applicable to both cases. Support for viscous forces between the solar wind and the ionospheric plasma in the trans-terminator flow derives from the momentum flux balance between the momentum flux in the latter flow and the deficiency of solar wind momentum along the flanks of the ionosheath. By comparing the relative width of the viscous boundary layer in the Venus ionosheath and the width of the trans-terminator flow we find that the transport of momentum within the upper ionosphere proceeds at a rate similar to that at which momentum is delivered to the upper ionosphere from the solar wind. Comparable values are obtained for the viscosity coefficient of the solar wind that streams over the ionosphere and that implied from momentum transport within the ionospheric trans-terminator flow. It is further suggested that despite the different nature of the processes that give place to the viscous transport of the solar wind momentum to the upper ionosphere (wave-particle interactions) and those responsible for its distribution within the ionosphere (through coulombian collisions) there is a similar response in the behavior of both plasmas to momentum transport. Calculations show that with comparable values of the viscosity coefficient in the ionosheath and in the upper ionospheric plasma the mean free path suitable to wave-particle interactions in the ionosheath is of the same order of magnitude as the mean free path of the planetary O⁺ ions that interact through coulombian collisions in the upper ionosphere. The effects of this similarity are considered in the discussion.     

Mercury’s magnetosphere-solar wind interaction for northward and southward interplanetary magnetic field: Hybrid simulation results

Analysis of global hybrid simulations of Mercury’s magnetosphere-solar wind interaction is presented for northward and southward interplanetary magnetic field (IMF) orientations in the context of MESSENGER’s first two encounters with Mercury. The global kinetic simulations reveal the basic structure of this interaction, including a bow shock, ion foreshock, magnetosheath, cusp regions, magnetopause, and a closed ion ring belt formed around the planet within the magnetosphere. The two different IMF orientations induce different locations of ion foreshock and different magnetospheric properties: the dayside magnetosphere is smaller and cusps are at lower latitudes for southward IMF compared to northward IMF whereas for southward IMF the nightside magnetosphere is larger and exhibits a thin current sheet with signatures of magnetic reconnection and plasmoid formation. For the two IMF orientations the ion foreshock and quasi-parallel magnetosheath manifest ion-beam-driven large-amplitude oscillations, whereas the quasi-perpendicular magnetosheath shows ion-temperature-anisotropy-driven wave activity. The ions in Mercury’s belt remain quasi-trapped for a limited time before they are either absorbed by Mercury’s surface or escape from the magnetosphere. The simulation results are compared with MESSENGER’s observations.     

Observations of interplanetary scintillation with a single-station mode at Urumqi

The Sun affects physical phenomena on Earth in multiple ways.In particular,the material in interplanetary space comes from coronal expansion in the form of inhomogeneous plasma flow (solar wind),which is the primary source of the interplanetary medium.Ground-based Interplanetary Scintillation (IPS) observations are an important and effective method for measuring solar wind speed and the structures of small diameter radio sources.We discuss one mode of ground-based single-station observations: Single-Station Single-Frequency (SSSF) mode.To study the SSSF mode,a new system has been established at Urumqi Astronomical Observatory (UAO),China,and a series of experimental observations were successfully carried out from May to December,2008.     

行星际闪烁单站单频数据处理

太阳风是日地空间的主要物质来源,太阳风的观测对日地空间环境及地球物理的研究具有重要意义。地基行星际闪烁观测是监测太阳风风速,测量太阳风等离子体不规则结构,研究遥远致密射电源角径的重要且有效的方法。介绍了行星际闪烁地基观测的单站单频模式的基本理论,针对单站单频模式观测的数据处理及自编软件。本文的工作是为行星际闪烁单站双频系统数据分析处理作前期准备。     

一次中尺度雷暴大风过程的闪电特征分析

2005年6月21日山东北部出现了一次中尺度对流系统,并伴有地面灾害性大风。作者综合闪电定位资料、雷达和卫星资料详细分析了这次中尺度对流系统的闪电活动特征,结果表明,在系统初始发展阶段地闪频数快速增加.成熟阶段地闪频数一直较高,且都在20次/5 min以上,在减弱消散阶段,正地闪比例超过负地闪。负地闪多发生在对流降水区,而正地闪则对应于稳定的层状云降水区。逐小时地闪次数峰值滞后于云顶最低温度峰值,小于-50℃的冷云覆盖面积峰值滞后于地闪次数峰值。这次地面大风主要是较强下沉气流底部外流造成的,利用WINDEX计算的地面最大风速潜势与观测的阵风值非常接近。地面大风阶段对应着剧烈的闪电活动,地闪频数的跃增略提前于地面强风发生时间,这对灾害性天气过程的监测预警具有一定的参考价值。     

Covariation of the Indonesian Throughflow and South China Sea Throughflow Associated with the 1976/77 Regime Shift

Changes in the Indonesian Throughflow(ITF) and the South China Sea throughflow—measured by the Luzon Strait Transport(LST)—associated with the 1976/77 regime shift are analyzed using the Island Rule theory and the Simple Ocean Data Assimilation dataset.Results show that LST increased but ITF transport decreased after 1975.Such changes were induced by variations in wind stress associated with the regime shift.The strengthening of the easterly wind anomaly east of the Luzon Strait played an important role in ...     

应用泊松耿贝尔分布估算海上极端风速

采用泊松耿贝尔分布，基于中国气象局发布的《CMA-STI热带气旋最佳路径数据集》资料来估算海上极端风速，并以上川岛气象站多年实测资料通过概率评估来加以验证。结果表明，采用泊松耿贝尔分布可以得到较为保守的海上极值风速取值。对于海上的小面积区域的重现期风速估算，采用50 km半径区域进行评估，可以得到较为合理的估算结果，当评估区域较大时，则需考虑适当扩大评估半径。