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.     

冬季台风“南玛都”结构性质的初步研究

利用1982～2001年NCEP/NCAR再分析的周平均SST场、逐日表面热通量场及近地层10米高度风场资料,分析了南海地区季风爆发前后几周南海多年平均SST随时间的变化和空间分布特征及其影响因子.结果表明,南海季风爆发前,SST急剧升高,季风爆发后,SST的变化呈现比较明显的空间差异,南海北部SST继续上升,而南部SST持续下降.南海季风爆发前,海面净得热,这是季风爆发前南海SST上升的主要原因.季风爆发后几周,海面净得热减少,此时的海表净热通量收支与SST无显著相关.而季风爆发期和爆发后几周,南海SST变化的不均匀性与西南气流具有很好的相关性,南海的降温区呈东北-西南走向,与低层西南气流的方向一致.因而,在季风爆发后的一段时间内,近地层风场导致的海洋表面及内部动力过程是影响南海SST变化的另一重要因子.     

热带太平洋地区风场异常和与El Ni?o有关的年际变化

利用1964～1993年NCEP/NCAR再分析风应力资料和中国科学院大气物理研究所发展的14层热带太平洋环流模式(OGCM),对热带太平洋与El Ni?o有关的年际变化进行了研究.首先,分析了西太平洋暖池次表层海温异常(SOTA)与Ni?o3区海表温度异常(SSTA)的年际变化关系,发现在El Ni?o事件之前,暖池的次表层海温都有明显正异常出现,它的东传导致了El Ni?o的发生,并且SOTA的传播随纬度变化,沿赤道东传,在赤道外西传.然后,选取了20世纪70年代和80年代两次最强的El Ni?o事件讨论了引起这种机制的可能原因--西风异常的作用.最后,对1964～1993所有的El Ni?o年的风场、次表层海温和海表温度的异常进行了综合分析.     

风能资源观测数据省级传输系统

风能资源观测数据省级传输系统是国家风能资源数据库建设项目的一个重要组成系统,是全国风能及其相关数据和产品服务的基础,并已实现了观测数据的业务化传输。该系统由数据收集、收集处理、数据分发、传输监视等4个功能模块组成。数据收集模块功能由Linux下的socket编程实现,可收集实时和历史数据、备份数据、删除过时数据;收集处理模块功能由Linux下的C语言编程实现,可对数据的唯一性、正确性及格式进行检查;数据分发模块功能由Linux下的socket编程实现,可实时分发、失败重发、分发日志记录;传输监视模块具有监视、统计、信息查询和显示等功能。     

珠峰北坡绒布河谷大气二氧化碳浓度低值观测

In the summers of 2006 and 2007, the atmospheric CO2 concentration and the wind speed in the Rongbuk Valley on the northern slope of Mt. Everest were measured by an ultrasonic anemometer with an Li-7500 CO2/H2O gas analyzer. The average CO2 concentration was 370.23±0.59 and 367.45±1.91 ppm in June of 2006 and 2007, respectively. The values are much lower than those at sites with similar latitudes and altitudes worldwide. The observed atmospheric CO2 concentration in Rongbuk Valley can be affected by the transportation of prevailing down-valley winds from the up-valley direction to the observation site. Our results suggest that the Mt. Everest region could be ideal for background atmospheric and environmental studies.