BCC大气环流模式对亚澳季风年际变率主导模态的模拟   总被引：8，自引：3，他引：5  

王璐  周天军  吴统文  吴波 《气象学报》2009,67(6):973-982

利用观测海温驱动下的北京气候中心大气环流模式(BCC-AGCM)1979-2000年的模拟数据,从亚澳季风(A-AM)年际变率的角度,对该模式的性能进行了分析.通过季节依赖的EOF分析方法(SEOF)得到观测第1模态,与ENSO从暖位相向冷位相的转变相联系,并伴随东南印度洋和西北太平洋的降水异常随季节变化.该模态具有准2a和4-6a周期的谱峰.分析结果显示,BCC模式可以很好地模拟出第1模态的时间变化特征,及其与ENSO位相的同步关系.但是,模式模拟的降水空间型与观测存在偏差,这主要是由于模式对环流场模拟的偏差造成的,具体表现在西北太平洋(WNP)反气旋和南印度洋(SIO)反气旋的季节锁相模拟偏差.前者与模式模拟的环流场整体偏东有关,后者是由于SIO反气旋的发展和衰亡过程受印度洋局地海气相瓦作用影响,而单独大气模式则无法合理地反映这一过程.另外,模式模拟的第一模态降水空间型在夏季效果较差,原因在于模式模拟的夏季平均降水量存在偏差,尤其是东南印度洋的降水量模拟偏少.进一步分析表明,这可能与对流参数化方案的选择有关.  相似文献   

地球系统10~(-1)年变化原因概述   总被引：4，自引：4，他引：0       下载免费PDF全文

汤懋苍  雍晓春  邓国卫  郭维栋 《高原气象》2009,28(6):1485-1489

我们曾论述了地球系统100～108年变化的原因[1], 唯对10-1年（月一年）的地球系统变化未指出其变化原因。经过近年的研究, 现在可以明确地指出, 地球内部有两类流体： 地外核和岩石圈裂隙中地下流体（地气）的活动是引发10-1年地球系统变化的原因。外核的上升运动会使其上部岩石圈产生上抬和压缩, 在地表层就出现3.2 m地温升高和降水减少的“干热异常”, 经过“孕震三步曲”最终引发构造地震。外核的下降运动会使其上部岩石圈产生下沉和拉张作用, 地表层表现为3.2 m地温降低, 同时降水增多的“湿冷异常”, 最终可导致发生陷落地震。外核的脉冲运动是引发岩石圈中形成地热（冷）涡的“源”。地气环流也是旋转地球上的一种流体运动, 其特征速度（地下风速）约为0.2 m/s, 据此可推得“自然气候周期”约为8个月。地气环流是使地气系统得以“流”的动力源。地热（冷）涡的“源”、 “流”相结合是使短期气候呈现纷繁复杂变化的原因。  相似文献   

南极洲低层两种位势高度再分析资料的比较     

施宁  王盘兴  徐海明  郭栋 《高原气象》2008,27(6)

比较NCEP/NCAR和ECMWF两种再分析资料南半球低层等压面(700 hPa及以下)的平均位势高度场,结果表明:两者在南极洲差异显著,除12月、1月(南半球夏季)外,NCEP/NCAR资料存在一个虚假的很强的极地高压,而ECMWF资料正常。分析表明该两种再分析资料的上述差异来源于南极洲地面以下虚拟气压场的产生过程;NCEP/NCAR资料较ECMWF少了一个对南极洲过低地面温度的修正。由此得到的NCEP/NCAR资料若用于南半球低层大气环流整体结构的分析,会导致严重的错误。  相似文献   

SMIP2试验对亚洲夏季风的模拟能力及其可预报性的分析   总被引：4，自引：2，他引：2  

施洪波  周天军  万慧 《大气科学》2008,32(1):36-52

利用参加第二次季节预测模式比较计划（Phase 2 of the Seasonal Prediction Model Intercomparison Project,简称SMIP2）的五个大气环流模式的输出结果,比较了这些模式对亚洲夏季降水的模拟能力,并讨论了大气环流模式在季节尺度上对亚洲夏季风的可预报性。结果表明,各模式能够较好地模拟亚洲夏季降水的大尺度分布特征。除了模拟的东亚夏季降水异常经验正交函数分解第一模态（EOF1）的时间系数与观测之间的相关系数较低之外,多数模式可以大致再现东亚、南亚和西太平洋夏季降水异常EOF1及其对应的时间系数。分析表明,热带地区有很好的可预报性,北半球副热带地区的可预报性尽管也较好,但比热带地区要低,南半球热带以外地区的可预报性较差,陆地上的可预报性比海洋上低。在热带和北半球副热带地区,由海温强迫所产生的较大外部方差对此地高可预报性有很大的贡献。与正常年份相比,模式在强El Ni?o年和强La Ni?a年表现出较高的可预报性,在南亚和印度洋地区大多数模式在El Ni?o年比La Ni?a年产生了更好的可预报性,在中西太平洋区域El Ni?o年可预报性的高值中心较La Ni?a年位置偏西。  相似文献   

热带印度洋偶极子事件期间印度洋大气的变化——大气流函数场和势函数场的分析   总被引：1，自引：0，他引：1  

刘琳  于卫东  刁新源 《大气科学》2008,32(5):1083-1093

大气环流的变异是热带印度洋偶极子（IOD）事件研究中的一个重要问题。本文从风场旋度分量和散度分量角度出发,利用观测资料和大气环流模式,对IOD事件发生时热带印度洋海区上空的大气环流变化进行了分析,揭示出风场不同分量在IOD事件期间的变化特征。研究结果表明,热带印度洋大气环流系统在IOD事件期间,旋度分量和散度分量在垂直方向上呈现明显的一阶斜压形式,而在水平方向上呈现明显的对称分布特征。对低空（850 hPa）来说,无辐散流函数距平场在IOD事件正位相期间表现为关于赤道对称的一对反气旋式环流;无旋度分量在IOD事件正位相期间的响应表现为东印度洋辐散、西印度洋辐合;大气环流的两种分量场均可以在赤道印度洋地区产生距平意义下的纬向东风,正是这种形式的距平东风使得IOD事件依靠海气系统正反馈机制得以维持和发展。而高空（200 hPa）大气环流形式刚好与850 hPa相反。  相似文献   

谱模式SAMIL对南亚季风区大气季节内振荡向北传播的模拟     

贾小龙  李崇银  凌健 《大气科学》2008,32(5):1037-1050

基于与NCEP资料结果的比较,研究了中国科学院大气物理研究所大气科学和地球流体力学数值模拟国家重点实验室发展的大气环流模式SAMIL对夏季南亚季风区季节内振荡（ISO）向北传播特征的模拟,并结合目前对ISO北传机制的理解对模拟结果进行了分析讨论。SAMIL在夏季南亚地区模拟出相当强度的季节内振荡的活动,并且模拟的ISO也表现出与NCEP资料相似的从赤道向北传播的特征,但传播的速度要慢于NCEP资料的结果。模拟的北传ISO具有与NCEP资料相似的结构特征,涡度和水汽场明显的呈经向不对称,涡度和水汽的正异常位于ISO对流的北面,最大的上升运动和最强的行星边界层辐合也位于ISO对流的北面。ISO 结构的经向不对称性正是模式模拟的ISO具有向北传播特征的原因;而模式对夏季南亚季风区高低层风场和行星边界层水汽的合理模拟起了关键的作用。同时,根据关于ISO北传机理的已有研究,模式的结果也表明南亚地区夏季风场的垂直结构是那里ISO向北传播的重要机制。  相似文献   

Intermediate‐term variations in solar radius during solar cycle 23     

H. Kili  O. Golbasi  F. Chollet 《Astronomische Nachrichten》2009,330(4):351-357

In this study, we look for the mid‐term variations in the daily average data of solar radius measurements made at the Solar Astrolabe Station of TUBITAK National Observatory (TUG) during solar cycle 23 for a time interval from 2000 February 26 to 2006 November 15. Due to the weather conditions and seasonal effect dependent on the latitude, the data series has the temporal gaps. For spectral analysis of the data series, thus, we use the Date Compensated Discrete Fourier Transform (DCDFT) and the CLEANest algorithm, which are powerful methods for irregularly spaced data. The CLEANest spectra of the solar radius data exhibit several significant mid‐term periodicities at 393.2, 338.9, 206.5, 195.2, 172.3 and 125.4 days which are consistent with periods detected in several solar time series by several authors during different solar cycles. The knowledge relating to the origin of solar radius variations is not yet present. To see whether these variations will repeat in next cycles and to understand how the amplitudes of such variations change with different phases of the solar cycles, we need more systematic efforts and the long‐term homogeneous data. Since most of the periodicities detected in the present study are frequently seen in solar activity indicators, it is thought that the physical mechanisms driving the periodicities of solar activity may also be effective in solar radius variations (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

A survey for satellites of Venus     

Scott S. Sheppard  Chadwick A. Trujillo 《Icarus》2009,202(1):12-16

We present a systematic survey for satellites of Venus using the Baade-Magellan 6.5 m telescope and IMACS wide-field CCD imager at Las Campanas observatory in Chile. In the outer portions of the Hill sphere the search was sensitive to a limiting red magnitude of about 20.4, which corresponds to satellites with radii of a few hundred meters when assuming an albedo of 0.1. In the very inner portions of the Hill sphere scattered light from Venus limited the detection to satellites of about a kilometer or larger. Although several main belt asteroids were found, no satellites (moons) of Venus were detected.  相似文献   

Optical properties of dust from Jupiter family comets     

E. Hadamcik 《Planetary and Space Science》2009,57(10):1118-1132

To try to define specific physical properties of the dust of Jupiter-family comets (JFCs), we compare the light scattered by them. Amongst the more than 1000 JFCs, less than 200 are numbered, 40 of them being rather bright. In the present work we use data from the latter. In situ observations of three nuclei show low albedo surfaces. The albedo of the dust particles in the coma is low, with generally a red colour. The A(α)fρ product is a measure of cometary activity and secular changes. Images of different regions (jets and fans) give indications on the nucleus rotation and position of the emitting areas, as compared to the position of the rotation axis. Differences in physical properties between the particles in different regions are pointed out by differences in the linear polarization of the scattered light and by spectral variations in brightness and polarization. Jupiter family comets are considered as dust-poor comets. Tails and trails’ studies give an estimation of the size distribution of the particles. However the dust production rates depend on the largest particles (up to centimetre size), which are mainly observed in the trails where large dark compact particles are found. These dark particles are also responsible for the high polarization in the inner most coma of some comets. The meaning, in terms of physical properties, of the linear polarization is discussed through different examples such as 2P/Encke, 9P/Tempel 1 or the fragments of 73P/Schwassmann-Wachmann 3. Cometary outbursts and splitting events show that the properties of the dust ejected from the interior of the nucleus are similar to the ones of more active comets (new or with larger semi-major axis).  相似文献   

Repeating microlensing events in the OGLE data     

J. Skowron  &#;. Wyrzykowski  S. Mao  M. Jaroszy&#;ski 《Monthly notices of the Royal Astronomical Society》2009,393(3):999-1009

Microlensing events are usually selected among single-peaked non-repeating light curves in order to avoid confusion with variable stars. However, a microlensing event may exhibit a second microlensing brightening episode when the source or/and the lens is a binary system. A careful analysis of these repeating events provides an independent way to study the statistics of wide binary stars and to detect extrasolar planets. Previous theoretical studies predicted that 0.5–2 per cent of events should repeat due to wide binary lenses. We present a systematic search for such events in about 4000 light curves of microlensing candidates detected by the Optical Gravitational Lensing Experiment (OGLE) towards the Galactic bulge from 1992 to 2007. The search reveals a total of 19 repeating candidates, with six clearly due to a wide binary lens. As a by-product, we find that 64 events (∼2 per cent of the total OGLE-III sample) have been misclassified as microlensing; these misclassified events are mostly nova or other types of eruptive stars. The number and importance of repeating events will increase considerably when the next-generation wide-field microlensing experiments become fully operational in the future.  相似文献