用红外和水汽两个通道的卫星测值指定云迹风的高度

提出了一种改进的用红外和水汽两个通道的测值指定云迹风高度的算法。利用红外水汽散点图和云迹风本身自动地将有低云的目标区、有半透明卷云的目标区、有密蔽高云的目标区分开。在有低云的目标区和有密蔽高云的目标区用红外一个通道指定云高。在有半透明卷云的目标区用红外和水汽两个通道指定云高。在用两个通道的测值指定云高时，假定卷云高度以上不存在水汽，以红外和水汽两个通道亮温相同这个方程与两个通道辐射测值线性相关的方程联立解出云的高度     

塔克拉玛干沙漠荒漠过渡带春季风沙活动特征——以肖塘为例

 通过对沙尘暴强化观测试验期间风速、跃移颗粒数、输沙量等资料的统计与计算,对塔克拉玛干沙漠北缘荒漠过渡带肖塘地区春季风沙活动进行了研究。结果表明,肖塘地区春季2 m高度1 s时距的起沙风速为4.9～5.0 m·s-1,1 min时距的起沙风速为4.4 m·s-1;起沙风速随着风速等级的增加,出现的频率相应减少,主要集中在4.4～8.4 m·s-1 之间;输沙势、输沙量的方位分布与起沙风相似,以ENE、E和ESE 3个方位为主,观测期间（1个月）总输沙势为80.8 VU,合成输沙势为13.7 VU,合成输沙势方向为241°;最大可能输沙总量为1 921.8 kg·m-1,合成输沙量为286.8 kg·m-1,合成输沙方向为235°,与输沙势的合成方向一致。     

影响生物土壤结皮在沙丘不同地貌部位分布的风因子讨论

 生物土壤结皮广泛分布于干旱和半干旱区,它的形成和发育对荒漠生态系统修复过程产生重要的影响。采用野外观测的方法,测定了固定沙丘纵断面表面气流和生物土壤结皮的发育特征。结果发现,近地表气流在迎风坡坡脚部位最低,丘顶最高,从坡脚到丘顶呈增加的趋势。近地表气流在背风坡中上部急剧下降,中下部位有所增加,到坡脚部位又呈减少的趋势,但后者均远低于丘顶的风速。各观测点不同高度风速放大率不尽相同。生物土壤结皮发育特征的测定结果显示,其厚度、抗剪强度和细颗粒物含量均从沙丘底部向中上部呈减少的趋势,表现出风速较高区域生物土壤结皮的发育程度较低,风速较低区域生物土壤结皮的发育程度较高的特点,说明生物土壤结皮在沙丘不同地貌部位的分布与由地形差异导致的气流变化之间具有密切的关系。     

美国风电产业政策演进:历程、特征与影响因素

论文分析了美国风电产业政策演进的历程、特征与影响因素,这对于推进中国风电产业政策升级和提升政策效果具有重要参考价值。在扼要刻画美国风电产业发展现状基础上,提出了美国风电产业的政策框架;考察了美国风电产业政策的演进历程并进行了阶段划分,探讨了风电产业萌芽示范期、缓慢发展期、快速增长期和优化增长期等阶段的政策背景、内容和绩效。基于对演进历程的系统回顾,提出了美国风电产业政策演进的四大特征,并揭示了政策演进的影响因素。     

东南印度洋海洋锋面处低空大气的垂向分布结构

本文利用中国第25次南极科学考察期间获取的现场观测数据研究了东南印度洋（弗里曼特尔至中山站间）海洋锋面附近的低空大气风场以及温度场垂向分布特征。结果表明：弗里曼特尔港至中山站之间的亚南极锋锋面暖水侧与冷水侧风速垂向分布结构不同,锋面暖水侧风速垂向梯度小,风速梯度最大值出现在500m高度附近,而锋面冷水侧低空风速梯度最大值出现在150m高度附近,揭示了中纬度海气相互作用机制在东南印度洋海洋锋面附近起重要作用。同时,本文还发现了亚南极锋锋面上空存在支一强的低空纬向急流,急流中心位于300m高度处;极锋上空低空风速强而高空风速弱。     

Geoeffectiveness of magnetic cloud, shock/sheath, interaction region, high-speed stream and their combined occurrence

A subset of CMEs, called interplanetary magnetic clouds (MCs), are observed to have systematic rotation [northward to southward (NS) or southward to northward (SN)] in their field structures. These MCs identified in the heliospheric plasma and field data at 1 AU may have different features associated with them. These structures (NS/SN) may be isolated MC moving with the ambient solar wind. MCs (NS/SN) may also be associated with shock/sheath region, formed due to compression of the ambient plasma/field ahead of them. A fraction from each of these four types of MCs have additional features, being ‘pushed’ by fast solar wind streams from coronal holes, forming interaction region (IR) between MCs and high-speed solar wind streams (HSS). Using these different sets of MCs, we have done a detailed study of the geoeffectiveness of NS and SN turning MCs and their associated features (shock/sheath, IR and HSS). To study the process that produces the geomagnetic disturbances and influences its amplitude/duration, we have utilized the interplanetary plasma and field parameters, namely, plasma velocity, density, temperature, pressure, field strength and its north-south component, during the passage of these structures with different associated properties. Differences in the geoeffectiveness of MCs with different structural and dynamical properties have been identified. The possible role of high-speed stream in influencing the recovery time (and hence duration) of geomagnetic disturbance has also been investigated. A best-fit equation representing the relation between level of the geomagnetic activity (due to MCs) and interplanetary plasma/field parameter has been obtained.     

Statistical Analysis of the Relationships among Coronal Holes,Corotating Interaction Regions,and Geomagnetic Storms

We have examined the relationships among coronal holes (CHs), corotating interaction regions (CIRs), and geomagnetic storms in the period 1996?–?2003. We have identified 123 CIRs with forward and reverse shock or wave features in ACE and Wind data and have linked them to coronal holes shown in National Solar Observatory/Kitt Peak (NSO/KP) daily He i 10?830 Å maps considering the Sun?–?Earth transit time of the solar wind with the observed wind speed. A sample of 107 CH?–?CIR pairs is thus identified. We have examined the magnetic polarity, location, and area of the CHs as well as their association with geomagnetic storms (Dst≤?50 nT). For all pairs, the magnetic polarity of the CHs is found to be consistent with the sunward (or earthward) direction of the interplanetary magnetic fields (IMFs), which confirms the linkage between the CHs and the CIRs in the sample. Our statistical analysis shows that (1) the mean longitude of the center of CHs is about 8°E, (2) 74% of the CHs are located between 30°S and 30°N (i.e., mostly in the equatorial regions), (3) 46% of the CIRs are associated with geomagnetic storms, (4) the area of geoeffective coronal holes is found to be larger than 0.12% of the solar hemisphere area, and (5) the maximum convective electric field E _y in the solar wind is much more highly correlated with the Dst index than any other solar or interplanetary parameter. In addition, we found that there is also a semiannual variation of CIR-associated geomagnetic storms and discovered new tendencies as follows: For negative-polarity coronal holes, the percentage (59%; 16 out of 27 events) of CIRs associated with geomagnetic storms in the first half of the year is much larger than that (25%; 6 out of 24 events) in the second half of the year and the occurrence percentage (63%; 15 out of 24 events) of CIR-associated storms in the southern hemisphere is significantly larger than that (26%; 7 out of 27 events) in the northern hemisphere. Positive-polarity coronal holes exhibit an opposite tendency.     

Why Do Temperature and Velocity Have Different Relationships in the Solar Wind and in Interplanetary Coronal Mass Ejections?

In-situ observations of the solar wind (SW) show temperature increasing with the wind speed, whereas such a dependence is not observed in interplanetary coronal mass ejections (ICMEs). The aim of this paper is to understand the main origin of this correlation in the SW and its absence in ICMEs. For that purpose both the internal-energy and momentum equations are solved analytically with various approximations. The internal-energy equation does not provide a strong link between temperature and velocity, but the momentum equation does. Indeed, the observed correlation in the open magnetic-field configuration of the SW is the result of its acceleration and heating close to the Sun. In contrast, the magnetic configuration of ICMEs is closed, and moreover the momentum equation is dominated by magnetic forces. This implies no significant correlation between temperature and velocity, as observed.     

On the manifestation of Richtmyer-Meshkov instability in an inhomogeneous interstellar medium with radiative cooling

We numerically simulate the evolution of the plane two-dimensional deformations of a contact discontinuity that is impulsively accelerated by a shock wave. We take into account the effects of radiative cooling and perturbation scale lengths on the dynamics and shape of the forming density inhomogeneities. For moderately intense shocks in a stellar wind and for strong shocks from a supernova, we show that the radiative cooling processes do not affect significantly the growth rate of the initial perturbations and the total mass of the forming condensations. However, the density of the matter compressed by the transmitted shock wave increases dramatically. At the same time, the contribution from long-wavelength perturbations to the deformation of the contact surface decreases significantly. In the case of shock propagation from a supernova, the initial conditions have been found to be a factor that can affect the morphology of the shocked interstellar medium.     

北京盛夏一次罕见的大雹事件分析

分析了1969年8月29日出现在北京的罕见大雹事件.冰雹发生在蒙古低涡低槽大尺度环流背景下,500hPa的冷空气叠置在低层暖空气上,为冰雹等强对流天气的出现提供了有利的条件.分析表明,华北东部的降雹区位于高能带中,北京在高能带的中心并且对流有效位能(CAPE)和抬升指数(LI)均达到了一个较高的水平,特别是在-10～-30℃层内有高的CAPE值,使大冰雹的出现成为可能.此外,对流层中下层较强的环境风垂直切变有利于多单体风暴或超级单体等强风暴云的发展,从而增加了冰雹出现的几率.而且,合适的冻结层高度以及冷暖云厚度比也为降雹创造了条件.