Three-dimensional variational data assimilation of WindSat ocean surface winds for the genesis and forecasting of tropical storm Henri   总被引：2，自引：1，他引：1  

Zheng Weizhong  Zou Chengzhi 《气象科学》2010,30(5):615-620

With available high-resolution ocean surface wind vectors retrieved from the U.S. Naval Research Laboratorys WindSat on Coriolis, the impact of these data on genesis and forecasting of tropical storm Henri is examined using the non-hydrostatic, fifth-generation mesoscale model (MM5) of Pennsylvania State University-National Center for Atmospheric Research plus its newly released three-dimensional variational data assimilation (3DVAR) system. It is shown that the assimilation of the WindSat-retrieved ocean surface wind vectors in the 3DVAR system improves the model initialization fields by introducing a stronger vortex in the lower troposphere. As a result, the model reproduces the storm formation and track reasonably close to the observations. Compared to the experiment without the WindSat surface winds, the WindSat assimilation reduced an error between the model simulated track and observations of more than 80 km and also improved the storm intensity by nearly 2 hPa. It suggests that these data could provide early detection and prediction of tropical storms or hurricanes.  相似文献   

2008年奥运会期间北京地区大气O3浓度模拟分析     

高怡  张美根  朱凌云  唐贵谦 《气候与环境研究》2010,15(5):643-651

利用空气质量模式系统RAMS-CMAQ模拟分析了2008年8月北京及周边地区近地面O3浓度的时空变化。分析结果表明,模式系统可以较好地模拟污染物以及气象要素的变化特征和区域分布情况;奥运会期间的污染控制对O3浓度的降低有明显的作用,但是在一些有利的气象条件下,O3易达到较高浓度:8月2日、24日14时(北京时间)左右O3浓度都在0.22mg.m-3以上,其中2日北京地区处于辐合的弱风场中,风速为1.5～2.5m.s-1,24日则是处于自南向北的有输送作用的风场中,风速为3.5～6.5m.s-1;污染控制对北京周边地区的效果要好于北京市区。  相似文献   

多普勒激光雷达风场反演方法研究   总被引：3，自引：0，他引：3  

王改利  刘黎平  邱崇践 《大气科学》2010,34(1):143-153

采用三维变分同化反演(3DVAR)、 四维变分同化反演(4DVAR) 对多普勒激光雷达资料反演风场的方法进行了研究, 利用车载多普勒激光雷达在2008年残奥会测试赛期间外场试验取得的数据, 反演了海面10 m高度处的风场, 并将风场反演结果与浮标资料进行了对比分析, 结果表明: 3DVAR、4DVAR风场反演方法均能实现近海面风的精细化风场反演, 并能反映出风向的变化, 反演风场与浮标数据基本一致, 在风速较大的天气情况, 3DVAR与4DVAR反演风场的一致性要好于风速较小的天气情况; 4DVAR反演方法中以浮标资料作为背景场, 使得其与浮标的符合程度要好于3DVAR方法反演风场; 反演风场的风向与浮标风向具有很好的相关关系, 反演风场的风速与浮标风速具有一定的相关关系, 反演风场的风向、风速与浮标的风向、风速之间平均均方根误差和平均绝对误差表明, 这两序列之间具有一定差别, 在风速较小的天气情况下使用时需要注意。  相似文献   

中国新一代极轨气象卫星——风云三号   总被引：18，自引：2，他引：16  

杨军  董超华  卢乃锰  杨忠东  施进明  张鹏  刘玉洁  蔡斌 《气象学报》2009,67(4):501-509

风云三号(简称FY-3)是中国第2代极地轨道气象卫星系列.它的第1颗星--风云三号A星(FY-3A)于2008年5月27日上午11时02分33秒在山西太原卫星发射中心发射升空.新一代极轨气象卫星主要是实现伞球、全天候、三维、定量、多光谱遥感,以满足现代气象业务,特别是数值天气预报业务的发展,同时监测大范围气象及其衍生自然灾害和生态环境变化,为研究全球气候变化规律,进行气候诊断和预测提供地球物理参数,为农、林、交通、海洋、水文等多领域提供服务.FY-3A携带11个对地观测仪器,其观测数据通过星地链路进入地面接收站,并在数据处理和服务中心(国家卫星气象中心大楼内)汇集.在强大的计算机和网络支撑下,利用科学算法对仪器遥感数据进行处理,生成各类产品,提供给用户使用.FY-3A发射后,经过半年的在轨测试和试运行,于2009年初正式投入业务运行,卫星和地面系统状态稳定,工作正常.文中较系统全面地介绍了卫星轨道、数传、仪器、数据接收、处理和产品等,尤其分析了星载仪器的主要技术特征,并给出了部分产品应用实例.  相似文献   

CAM3模式海气湍流通量参数化的改进及其应用   总被引：1，自引：0，他引：1  

李忠贤  孙照渤  陈海山  倪东鸿 《气象学报》2009,67(6):1101-1112

通过对流性阵风参数化方法,在CAM3原有海气湍流通量参数化方案(CAM3方案)中引入边界层自由对流和降水深对流对海表湍流通量的贡献,改进了CAM3模式的海气湍流通量参数化方案(CAM3 ME方案).在此基础上,利用观测海温积分改进的CAM3模式,分析改进模式对冬(DJF)、夏季(JJA)大气环流异常的模拟性能.结果表明,采用改进的海气湍流通量参数化方案,模式对冬(DJF)、夏季(JJA)大气环流异常年际变化的模拟能力有了很大提高,尤其是冬季(DJF)北太平洋和北美大陆地区以及夏季(JJA)南半球海洋上空.  相似文献   

GIS技术在决策气象服务系统建设中的应用   总被引：21，自引：5，他引：16       下载免费PDF全文

吴焕萍  罗兵  王维国  段延娥 《应用气象学报》2008,19(3):380-384

该文介绍了基于组件式GIS技术的决策气象服务系统建设的总体框架, 并阐述了系统的建设内容, 主要包括电子地图建设、气象制图输出、实时与历史资料检索、灾情分析、台风预警与损失评估以及参数化制图等功能; 同时对GIS应用于决策气象服务系统的若干关键技术问题进行了深入讨论与分析, 如数据共享与转换、气象要素插值算法、空间信息检索方法、基于插件技术的模型评估方法、三维可视化技术; 最后给出了相关结论, 并指出该系统将为全国综合性决策服务系统提供一个良好的建设思路。  相似文献   

TOPEX/Poseidon高度计资料在全球海洋环流模式中的同化及分析   总被引：1，自引：0，他引：1  

刘娟  王斌  俞永强  刘海龙 《气候与环境研究》2008,13(6):697-707

利用一个新的四维变分海洋资料同化系统LICOM-3DVM对TOPEX／Poseidon高度计资料进行了同化。该同化系统是在LASG／IAP气候海洋模式LICOM1．0的基础上建立起来的,所用的同化方法为三维变分映射资料同化方法3DVM。高度计观测资料是采取间接的方式进行同化,即先建立起二维海面高度距平场与三维温度场的统计关系,并由此通过观测的海面高度距平信息反演出“观测”的三维温度场,然后利用LICOM-3DVM四维变分同化系统将此反演的温度场同化到海洋模式中。作者设计了两组试验并对结果进行了比较分析,积分时间从1993年1月至2001年12月共9年时间。结果表明,由于上混合层相关系数较小,因此同化后海温没有改进;而在温跃层以及更深层次,同化后的海温均有很大程度的改善。从对赤道太平洋地区海温的气候态、季节变化和年际变化以及Nino3区的Nino指数的模拟情况来看,由于同化时将海面高度异常和海温异常之间的相关参数取为常数,没有考虑其季节和年际变化,因此,同化后对于赤道太平洋的年际变化没有改善。对于黑潮地区,由于模式的分辨率较低,同化之前没有很好地模拟出温度锋面,温度和盐度梯度都偏小,流速也偏弱;而同化后使得温度锋面和盐度梯度与WOA01更加吻合,流速增强。  相似文献   

New magnetic field measurements of β Cephei stars and slowly pulsating B stars     

S. Hubrig  M. Briquet  P. De Cat  M. Schller  T. Morel  I. Ilyin 《Astronomische Nachrichten》2009,330(4):317-329

We present the results of the continuation of our magnetic survey with FORS 1 at the VLT of a sample of B‐type stars consisting of confirmed or candidate β Cephei stars and Slowly Pulsating B (hereafter SPB) stars, along with a small number of normal B‐type stars. A weak mean longitudinal magnetic field of the order of a few hundred Gauss was detected in three β Cephei stars and two stars suspected to be β Cephei stars, in five SPB stars and eight stars suspected to be SPB stars. Additionally, a longitudinal magnetic field at a level larger than 3σ has been diagnosed in two normal B‐type stars, the nitrogen‐rich early B‐type star HD 52089 and in the B5 IV star HD 153716. Roughly one third of β Cephei stars have detected magnetic fields: Out of 13 β Cephei stars studied to date with FORS 1, four stars possess weak magnetic fields, and out of the sample of six suspected β Cephei stars two show a weak magnetic field. The fraction of magnetic SPBs and candidate SPBs is found to be higher: Roughly half of the 34 SPB stars have been found to be magnetic and among the 16 candidate SPBs eight stars possess magnetic fields. In an attempt to understand why only a fraction of pulsating stars exhibit magnetic fields, we studied the position of magnetic and non‐magnetic pulsating stars in the H‐R diagram. We find that their domains in the H‐R diagram largely overlap, and no clear picture emerges as to the possible evolution of the magnetic field across the main sequence. It is possible that stronger fields tend to be found in stars with lower pulsating frequencies and smaller pulsating amplitudes. A somewhat similar trend is found if we consider a correlation between the field strength and the v sin i ‐values, i.e. stronger magnetic fields tend to be found in more slowly rotating stars (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

The aperiodic broad-band X-ray variability of Cygnus X-3     

Magnus Axelsson  Stefan Larsson  Linnea Hjalmarsdotter 《Monthly notices of the Royal Astronomical Society》2009,394(3):1544-1550

We study the soft X-ray variability of Cygnus X-3. By combining data from the All-Sky Monitor and Proportional Counter Array instruments on the RXTE satellite with EXOSAT /Medium Energy (ME) detector observations, we are able to analyse the power density spectrum (PDS) of the source from 10⁻⁹ to 0.1 Hz, thus covering time-scales from seconds to years. As the data on the longer time-scales are unevenly sampled, we combine traditional power spectral techniques with simulations to analyse the variability in this range. The PDS at higher frequencies  (≳10⁻³ Hz)  are for the first time compared for all states of this source. We find that it is for all states well described by a power law, with index  ∼−2  in the soft states and a tendency for a less steep power law in the hard state. At longer time-scales, we study the effect of the state transitions on the PDS, and find that the variability below  ∼10⁻⁷ Hz  is dominated by the transitions. Furthermore, we find no correlation between the length of a high/soft-state episode and the time since the previous high/soft state. On intermediate time-scales, we find evidence for a break in the PDS at time-scales of the order of the orbital period. This may be interpreted as evidence for the existence of a tidal resonance in the accretion disc around the compact object, and constraining the mass ratio to   M ₂/ M ₁≲ 0.3  .  相似文献   

Spectral variability in Cygnus X-3     

L. Hjalmarsdotter  A. A. Zdziarski  A. Szostek  D. C. Hannikainen 《Monthly notices of the Royal Astronomical Society》2009,392(1):251-263

We model the broad-band X-ray spectrum of Cyg X-3 in all states displayed by this source as observed by the Rossi X-ray Timing Explorer . From our models, we derive for the first time unabsorbed spectral shapes and luminosities for the full range of spectral states. We interpret the unabsorbed spectra in terms of Comptonization by a hybrid electron distribution and strong Compton reflection. We study the spectral evolution and compare with other black hole as well as neutron star sources. We show that a neutron star accretor is not consistent with the spectral evolution as a function of L _E and especially not with the transition to a hard state. Our results point to the compact object in Cyg X-3 being a massive,  ∼30 M_⊙  black hole.  相似文献