利用卫星遥感数据监测莱州湾海冰

主要介绍了利用NOAA和EOS卫星遥感监测莱州湾海冰的方法,简要分析了海冰对不同光谱的反应及海冰和水体在可见光、近红外通道反射率的差异等,对2008年莱州湾海面结冰状况进行了监测,利用国家卫星气象中心提供的海冰厚度计算经验模式,估算了海冰厚度分布及面积。为了使海冰分布更加清晰,对NOAA卫星监测海冰图像进行了彩色增强处理。     

一次罕见的秋季暴雨天气成因分析

利用数值预报、常规天气图、各种物理量场、卫星云图、E（Energy）指数等对2007年9月18-20日一场历史罕见的区域性秋季暴雨天气过程进行了综合分析。该过程是在西风槽、副热带高压边缘的暖湿气流和13号台风韦怕减弱后的低气压共同作用下产生的;欧洲中心数值预报在预报西太平洋副高位置上明显优于T213数值预报;T213、日本和德国三家预报的降水中心位置均有一定的偏差,中心量级偏大,但对强降水出现的时间和落区预报都具有一定的指示意义;E指数作为一个反映降水强弱和落区的辅助工具,对本次降水过程做出了准确预报。     

三维城市地表反射率计算模式

地表反射率是控制地表能量平衡的一个重要参数。城市建筑物的分布具有较大的不均一性,这不仅给地基观测城市地表反射率带来了很大困难,数值模拟城市地表反射率也是非常困难的。作者开发了一个三维城市地表反射率模式city_photo,该方法结合了蒙特卡洛方法和几何光学方法的优点,具有较高的精度和较快的计算速度。通过引入城市地图的概念,该模式能够计算具有不同结构的城市的地表反射率。2002至2004年晴空MODIS（MODerate Resolution Imaging Spectroradiometer,中分辨率成像光谱辐射计）1~7通道可见光和近红外通道地表反射率资料被用来检验模式的有效性,位于北京朝阳区的中国科学院大气物理研究所的AERONET站点观测得到气溶胶光学特性和水汽资料,6S（Second Simulation of Satellite Signal in the Solar Spectrum）大气辐射传输模式被用来对其进行大气订正。模式计算的北京城市地表反射率个例与MODIS 7个通道地表反射率观测结果具有很高的相关性,相关系数在0.80~0.93之间,说明模式能够较好地模拟城市地表反射率随太阳和观测角度的变化情况。最后讨论了城市结构对城市地表反射率的影响。     

基于机载多光谱遥感数据的溢油信息提取方法

为研究应用紫外-可见光-近红外-热红外遥感数据识别海上溢油的方法,利用机载多光谱溢油监测设备获取了舟山海域多光谱遥感数据,并利用野外地物光谱仪获取了水体和油膜的反射光谱。通过提取并分析机载多光谱遥感图像上多目标的影像特征和光谱响应特征,利用决策树分类法对海上油膜相对厚度的分布进行分类和制图。研究表明,基于机载多光谱遥感数据的溢油信息提取方法总体分类精度达93.7%,能够准确区分薄油膜和厚油膜,可有效提取海洋溢油污染信息,完全能够满足海洋溢油污染遥感监测需求。     

Old stellar population synthesis： new age and mass estimates for Mayall Ⅱ = G1

Mayall Ⅱ = G1 is one of the most luminous globular clusters （GCs） in M31. Here, we determine its age and mass by comparing multicolor photometry with theoretical stellar population synthesis models. Based on far- and near-ultraviolet GALEX photometry, broad-band UBVRI, and infrared JHKs 2MASS data, we construct the most extensive spectral energy distribution of G 1 to date, spanning the wavelength range from 1538 to 20 000A. A quantitative comparison with a variety of simple stellar population （SSP） models yields a mean age which is consistent with G1 being among the oldest building blocks of M31 and having formed within ～1.7 Gyr after the Big Bang. Irrespective of the SSP model or stellar initial mass function adopted, the resulting mass estimates （of order 10^7M⊙） indicate that GI is one of the most massive GCs in the Local Group. However, we speculate that the cluster＇s exceptionally high mass suggests that it may not be a genuine GC. Our results also suggest that G1 may contain, on average, （1.65±0.63） × 10^2L⊙ far-ultraviolet-bright, hot, extreme horizontal-branch stars, depending on the adopted SSP model. In addition, we demonstrate that extensive multi-passband photometry coupled with SSP analysis enables one to obtain age estimates for old SSPs that have similar accuracies as those from integrated spectroscopy or resolved stellar photometry, provided that some of the free parameters can be constrained independently.     

An infrared study of Be stars based on ISO SWS01 spectra

The Infrared Space Observatory （ISO） Short-Wavelength Spectrometer （SWS） spectra of 10 Be stars are presented. It can be seen that the Be stars show a diversity in their ISO SWS01 spectral classifications by Kraemer et al., from naked stars, stars associated with dust, stars with warm dust shells, stars with cool dust shells to very red sources. In addition, the Brα/HI（14-6） line flux ratio derived for the sample stars is compared with that of P Cyg, and it is found that the line ratio of Be stars which were investigated show not only lower values as suggested by Waters et al., but also larger values. Therefore, the line ratio cannot be used to judge whether a star is a Be star or not.     

一次朝圣的旅途——参观LAMOST望远镜

首次获悉我国正在筹建全球最大的大视场光纤光谱望远镜（LAMOST）已是几年前的事情了,这一在世界上领先的项目立即引起了我的关注。随后,通过网络、《天文爱好者》杂志等渠道,逐步加深了对它的了解。这一次,我非常荣幸地参加了由“北京市青少年科技俱乐部”组织的参观LAMOST望远镜的活动,得以第一时间目睹它的风采。     

High resolution spectroscopy of two young active late type stars within 20 parsecs of the Sun

We present high-resolution optical echell spectroscopy of HIP 544 and HIP 46843, two nearby solar like stars. The discovery of these young stars at such a close distance to the Sun is really a surprising phenomenon. It will help us to have a better understanding of the structure and evolutionary history of the Milky Way. The radial ve-locities (RV) of HIP 544 and HIP 46843 are measured to be -6.88±0.13km s-1 and 8.30±0.16km s-1, respectively, which are more accurate than before. The equivalent widths (EW) of the Li I 6707.8 A absorption line of HIP 544 and HIP 46843 are mea-sured to be 110±5mA and 195±5mA respectively. Based on these properties, HIP 544 is estimated to be 100-800Myr old and HIP 46843 30-100Myr old using three relatively creditable methods.     

An unusual timing and spectral state of a black hole microquasar XTE J1550-564

An unusual timing and spectral state of a black hole microquasar XTE J1550-564 observed with RXTE is analyzed. Millisecond variabilities are found, which are significantly shorter than the minimum possible time scale in the light curves of black hole binaries, as suggested by Sunyaev & Revnivtsev (2000). The X-ray spectral fitting result indicates that there is an unusual soft component in the spectrum, which may be responsible for the millisecond variabilities. The millisecond variabilities as well as the unusual soft spectral component should be produced from some small, but independent active regions in the accretion disk.