热气候指数评价中国南方城市夏季舒适度

利用南方14个城市1981-2013年6-9月的逐日气象资料,根据生物环境特点,制定了基于通用热气候指数的新评价方法,对中国南方城市夏季舒适度进行评价研究。结果表明:中国南方城市的高温不舒适天数近33 a来以3.4 d/10a的速度增加,并有5 a震荡周期。舒适度排名显示,体感温度最高的4个城市分别为重庆、福州、南昌和长沙,杭州与重庆的体感舒适度下降速率较快。对比高温不舒适天数和高温日数发现,两者具有很好的一致性,证明了高温不舒适度与气温关系的密切性。同时,由于热气候指标计算要素的多重考虑,结果与高温日数存在一些差异,但其更具有一定参考和应用价值。     

地面自动气象观测设备运行状态信息检测技术

地面自动气象观测设备运行状态检测机制不足一直是困扰我国地面气象观测运行保障工作的一大难题。本研究从运行监控实际业务需求角度出发,在梳理现有业务运行地面自动气象观测设备结构基础上,结合部分研究成果,从数据采集模块、气压观测模块、温湿度观测模块、风观测模块、地温观测模块、雨量观测模块、供电系统模块、软件模块、能见度观测模块和称重降水观测模块共10个方面逐一细化了每一主要部件的状态检测点,并对其进行了分类和编码,同时参考现行业务运行设备长Z数据报文,制定了地面自动气象观测设备运行状态报文规范,最终研制了地面自动气象观测设备运行状态信息检测技术。通过统一规范、标准,研究结果可解决目前我国地面自动气象观测设备监控信息设计规范缺失的问题,可缓解当前厂家多、型号杂、设备不统一的不利局面,有利于推进地面自动气象观测设备运行监控技术规范化建设工作。     

Impact of the Vertical Velocity Field on Charging Processes and Charge Separation in a Simulated Thunderstorm

A three-dimensional(3D) charging-discharging cloud resolution model was used to investigate the impact of the vertical velocity field on the charging processes and the formation of charge structure in a strong thunderstorm. The distribution and evolution of ice particle content and charges on ice particles were analyzed in different vertical velocity fields. The results show that the ice particles in the vertical velocity range from 1 to 5 m s-1obtained the most charge through charging processes during the lifetime of the thunderstorm. The magnitude of the charges could reach 1014 n C. Before the beginning of lightning activity,the charges produced in updraft region 2(updraft speed 13 m s-1) and updraft region 1(updraft speed between 5 and 13 m s-1) were relatively significant. The magnitudes of charge reached 1013 n C, which clearly impacted upon the early lightning activity. The vertical velocity conditions in the quasi-steady region(updraft speed between –1 and 1 m s-1) were the most conducive for charge separation on ice particles on different scales. Accordingly, a net charge structure always appeared in the quasi-steady and adjacent regions. Based on the results, a conceptual model of ice particle charging, charge separation, and charge structure formation in the flow field was constructed. The model helps to explain observations of the"lightning hole" phenomenon.     

基于贝叶斯融合方法的高分辨率地面-卫星-雷达三源降水融合试验

为了探讨一种适用于区域性的地面、雷达、卫星等多源降水资料融合的方法,一种曾用于高分辨雷达、卫星土壤湿度产品反演的贝叶斯融合(Bayesian Merging)方法被尝试应用于江淮地区1 h-0.05°×0.05°经纬度高分辨率的雷达估测降水、卫星反演降水与地面站点观测降水3种资料的融合。在应用该方法时,通过2009年8月样本统计分别估计卫星和雷达反演降水的误差关系,通过曲线拟合建立误差方程,并以卫星资料作为背景场,但在融合时将雷达估测降水作为新的观测信息与地面观测降水同时引入。融合试验检验结果表明:贝叶斯融合方法能够有效实现雷达、地面、卫星3种不同来源资料的融合,该方法生成的多源融合产品的精度均优于任何单一来源的降水产品。     

HYSPLIT模式轨迹计算误差分析

基于NCEP 1°×1°再分析资料GDAS和NCEP2.5°×2.5°再分析资料GBL,利用美国NOAA 空气资源实验室ARL研发的一种用于计算和分析大气污染物输送、扩散轨迹的混合单粒子拉格朗日综合轨迹模式HYSPLIT,对2010年3月12日12时和田站距地100 m高度空气质点的3 d前向轨迹进行了模拟,分析了轨迹计算中的积分误差和分辨率误差.此次轨迹模拟试验中,积分误差对轨迹计算误差的贡献很小.随着积分时间的延长,积分误差略有增大.积分误差并未随着驱动数据分辨率的提高而减小.分辨率误差在积分的各个时刻并不相同,它与地形高度与天气系统有关.在轨迹模式中,轨迹计算基于风速在时间和空间上的线性插值,轨迹模拟的不确定性也与插值有关.使用不同分辨率的驱动数据对轨迹计算结果影响显著,分辨率误差对轨迹计算误差的贡献远大于积分过程中截断近似等带来的积分误差.     

On the use of X-ray and γ-ray telescopes for identifying the origin of electrons and positrons observed by ATIC, Fermi, and PAMELA

X-ray and γ-ray observations can help understand the origin of the electron and positron signals reported by ATIC, PAMELA, PPB-BETS, and Fermi. It remains unclear whether the observed high-energy electrons and positrons are produced by relic particles, or by some astrophysical sources. To distinguish between the two possibilities, one can compare the electron population in the local neighborhood with that in the dwarf spheroidal galaxies, which are not expected to host as many pulsars and other astrophysical sources. This can be accomplished using X-ray and γ-ray observations of dwarf spheroidal galaxies. Assuming the signal detected by Fermi and ATIC comes from dark matter and using the inferred dark matter profile of the Draco dwarf spheroidal galaxy as an example, we calculate the photon spectrum produced by electrons via inverse Compton scattering. Since little is known about the magnetic fields in dwarf spheroidal galaxies, we consider the propagation of charged particles with and without diffusion. Extending the analysis of Fermi collaboration for Draco, we find that for a halo mass ∼10⁹ M_⊙, even in the absence of diffusion, the γ-ray signal would be above the upper limits. This conclusion is subject to uncertainties associated with the halo mass. If dwarf spheroidal galaxies host local magnetic fields, the diffusion of the electrons can result in a signal detectable by future X-ray telescopes.     

Optimized running conditions and sensitivity for direction sensitive detectors of WIMP dark matter

Optimum fill pressures for direction-sensitive dark matter detectors based on tracking in gases are considered. Given the minimum resolvable track length and the gas fill, the Lindhard–Scharf stopping model leads to the existence of an optimum pressure which maximizes the specific event rate R (event rate per unit detector volume). In addition, maximizing the detectibility of the recoil nucleus diurnal asymmetry is considered. Optimum fill pressures are calculated for Ar, CF₄, CS₂ and Xe gas fills, as a function of the WIMP mass and the minimum resolvable track length. The associated minimum target volumes required to achieve currently competitive WIMP-nucleon cross-section sensitivity are also calculated. The standard isothermal sphere model of the galactic WIMP halo is used throughout, but the method could be extended to use any desired WIMP distribution function.     

Detection and Correction of AMSR-E Radio-Frequency Interference

Radio-frequency interference (RFI) affects greatly the quality of the data and retrieval products from space-borne microwave radiometry. Analysis of the Advanced Microwave Scanning Radiometer on the Earth Observing System (AMSR-E) Aqua satellite observations reveals very strong and widespread RFI contam- inations on the C- and X-band data. Fortunately, the strong and moderate RFI signals can be easily identified using an index on observed brightness temperature spectrum. It is the weak RFI that is diffi- cult to be separated from the nature surface emission. In this study, a new algorithm is proposed for RFI detection and correction. The simulated brightness temperature is used as a background signal (B) and a departure of the observation from the background (O-B) is utilized for detection of RFI. It is found that the O-B departure can result from either a natural event (e.g., precipitation or flooding) or an RFI signal. A separation between the nature event and RFI is further realized based on the scattering index (SI). A positive SI index and low brightness temperatures at high frequencies indicate precipitation. In the RFI correction, a relationship between AMSR-E measurements at 10.65 GHz and those at 18.7 or 6.925 GHz is first developed using the AMSR-E training data sets under RFI-free conditions. Contamination of AMSR-E measurements at 10.65 GHz is then predicted from the RFI-free measurements at 18.7 or 6.925 GHz using this relationship. It is shown that AMSR-E measurements with the RFI-correction algorithm have better agreement with simulations in a variety of surface conditions.     

European Solar Telescope: Progress status

In this paper, the present status of the development of the design of the European Solar Telescope is described. The telescope is devised to have the best possible angular resolution and polarimetric performance, maximizing the throughput of the whole system. To that aim, adaptive optics and multi‐conjugate adaptive optics are integrated in the optical path. The system will have the possibility to correct for the diurnal variation of the distance to the turbulence layers, by using several deformable mirrors, conjugated at different heights. The present optical design of the telescope distributes the optical elements along the optical path in such a way that the instrumental polarization induced by the telescope is minimized and independent of the solar elevation and azimuth. This property represents a large advantage for polarimetric measurements. The ensemble of instruments that are planned is also presented (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

A uvbyβ photometric analysis of the Monoceros star‐forming field

This investigation presents a new analysis of the spatial distribution of the bright early‐type stars in the field of Northern Monoceros. A database of all O–B9 stars with available uvbyβ photometry is collated and a homogeneous distance scale is established for the clusters and layers of field stars. We provide revised distances for NGC 2264 and NGC 2244 of 833±38 (s.e.) pc and 1585±60 (s.e.) pc, respectively. We present arguments that there might be substructures in the clusters projected along the line of sight. According to the present sample the classical Mon OB2 association at 1.6 kpc is represented by a relatively compact group at 1.26 kpc in the vicinity of NGC 2244 and a layer of massive stars located between 1.5 and 3 kpc (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)