2009年11月北京极端低温和强降水事件分析

2009年10月底到11月底,包括北京在内的华北地区连续出现2次较强冷空气过程,造成大范围的低温、雨雪天气。利用北京地区11个气象站近50年逐日气温、降水资料,对全市历年11月低温雨雪事件的演变特征进行了分析。结果表明,2009年11月全市月平均气温、月平均最低气温均突破了50年的最低记录,月平均最高气温位列1981年11月之后,接近历史极值;2009年11月降雪量也位列有记录以来第一位,冰冻日数历史排位第三;从气温和降水极端事件发生的频次来看,2009年11月日平均气温、日最高气温和日最低气温通过5%分位值标准的极端低温事件频次都明显偏多,在50年中居于第2位,降水量通过95%分位值标准的极端强事件频次在50年中居于第四位。2009年11月的严重低温雨雪事件出现在区域气温总体变暖、低温事件频率总体下降的气候趋势背景下,在一定程度上放大了负面影响。亚洲中高纬地区500hPa高度场经向度异常加大、冷暖气流交换活跃,是造成2009年11月极端低温和大雪的直接环流因子。     

山西省主汛期极端变化降水特征

利用环渤海地区60个测站1961～2008年逐日降水资料,采用L矩参数估计方法对各站超临界值日极端降水拟合广义帕雷托分布。结果表明,广义帕雷托分布能够很好地拟合环渤海地区日极端降水的概率分布,其尺度参数、形状参数与极端降水重现期的地理空间分布密切相关,重现期50、100年一遇的日极端降水空间分布基本一致,山东南部、河北西南部、辽宁西部与河北东北部等区域具有较高极端降水值。     

风切变对飞行的影响及其预报时效分析

利用NCEP再分析资料和AMDAR资料,对2008年11月1日首都机场冷锋过境前后风切变现象及其可预报时效进行分析。分析认为:在冷锋过境前后,首都机场存在多种形式的风切变,有高空槽前后的水平风切变、高层和中层急流轴引起的水平风切变、冷锋前逆温层顶上下的水平风切变和地面锋面过境时跑道面上的水平和侧风切变。对各种风切变的可预报时效进行了分析。     

平舆县48年来气温变化特征和突变分析

利用1959-2006年平舆县气温观测资料,分析了平舆县的年、季平均气温的变化特征,并用Mann-Kandell检验法对年平均气温的变化特征进行了突变检验.结果表明:48年来平舆县气温以增温为主;就各季节而言,除了夏季以降温趋势为主外,其他各季节均以增温趋势为主.特别是冬季,增温趋势十分显著.利用Mann-Kandell检验法对逐年平均气温突变检验结果显示,在1989年附近可能发生突变.     

Color dependence of clustering properties of Luminous Red Galaxies (LRGs)

From the approximately volume-limited Luminous Red Galaxy (LRG) sample of the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we construct three LRG samples with different g-r color, which have the nearly same number density, to investigate the color dependence of clustering properties of LRGs. It is found that the blue galaxies have a more filamentary distribution than red galaxies, and that the bluest LRGs preferentially inhabit the dense groups and clusters. But in three LRG samples with different u-g color, we do not observe the tendency for clustering properties of LRGs to significantly change with color. We preferentially conclude that the clustering properties of LRGs are not strongly correlated with colors.     

Flare-induced signals in polarization measurements during the X2.6 flare on 2005 January 15

Flare-induced signals in polarization measurements which were manifested as apparent polarity reversal in magnetograms have been reported since 1981. We are motivated to further quantify the phenomenon by asking two questions: can we distinguish the flare-induced signals from real magnetic changes during flares, and what we can learn about flare energy release from the flare-induced signals? We select the X2.6 flare that occurred on 2005 January 15, for further study. The flare took place in NOAA active re-gion (AR) 10720 at approximately the central meridian, which makes the interpretation of the vector magnetograms less ambiguous. We have identified that flare-induced signals during this flare appeared in six zones. The zones are located within an average distance of 5 Mm from their weight center to the main magnetic neutral line, have an average size of (0.6±0.4)×1017 cm2, duration of 13±4 min, and flux density change of 181±125 G in the area of reversed polarity. The following new facts have been revealed by this study: (1) the flare-induced signal is also seen in the transverse magnetograms but with smaller magnitude, e.g., about 50 G; (2) the flare-induced signal mainly manifests itself as apparent polarity reversal, but the signal starts and ends as a weakening of flux density; (3) The flare-induced signals appear in phase with the peaks of hard X-ray emission as observed by the Ramaty High Energy Solar Spectroscopic lmager (RHESSI), and mostly trace the position of RHESSI hard X-ray footpoint sources. (4) in four zones, it takes place cotemporally with real magnetic changes which persist after the flare. Only for the other two zones does the flux density recover to the pre-flare level immediately after the flare.The physical implications of the flare-induced signal are discussed in view of its relevance to the non-thermal electron precipitation and primary energy release in the flare.     

Measurements of spectral lines observed with Hinode/EIS as implications for coronal heating

We have measured the line widths and nonthermal velocities in 12 solar regions using high resolution EUV data taken by Hinode/EIS. We find that there exists a positive correlation between the intensity and nonthermal velocity for the Fe XII emission line as well as some other lines. The correlation coefficients decrease from the disk center to the limb. However, the nonthermal velocities of a particular spectral line do not vary much in different regions, so they are considered isotropic. In particular, we find that for a coronal loop structure, the largest widths and nonthermal velocities occur at the footpoints, where outflows appear. Based on these observational results, we discuss several physical processes responsible for coronal heating.     

混合式数字化博物馆设计与研究

数字化博物馆是一种结合前沿技术开发的区别传统实体博物馆的综合服务信息系统。本文对目前采用的基于图形和基于图像的两种数字化博物馆构建方法进行分析比较,提出了一种室外采用三维建模、室内采用360°全景图的混合式构建方法。探讨了混合式数字化博物馆在场景漫游和场景切换方面的关键技术,设计并实现了混合式数字化博物馆的框架结构与部分功能,是数字化博物馆建设的一种新的尝试。