我国西南地区一次暴雨过程特征及成因

利用卫星云图、多普勒天气雷达资料和高空风等各种天气学资料,对2009年6月8—9日广西、贵州、以及和湖南交界地带的一次暴雨过程进行了综合分析。结果表明,暴雨是由中尺度对流复合体东移、β中尺度强对流云团发展、以及二者合并造成的;地面α中尺度低压带配合α中尺度纬向切变线的生成,为中尺度对流复合体（mesoscale convective complex,MCC）的东移发展、β中尺度强对流云团的发展、以及二者的合并创造了有利条件;地面能量比低值舌的活动是MCC和β中尺度强对流云团生成和发展的触发机制之一;在多普勒雷达径向速度图上,MCC的生成和发展,伴随西南低空急流的建立和维持,大范围的逆风区的生成;MCC的消亡,伴随西南低空急流的减弱和消失,对应西北气流建立和东扩。MCC发展期和β中尺度强对流云团发展期、MCC消散期和β中尺度强对流云团消散期的涡度收支以及视热源和视水汽汇有很大的不同。     

Near-Infrared Observations of the Massive Star Forming Region IRAS 23151＋5912

Near-infrared images and K-band spectroscopy of the massive star-forming region IRAS 23151+5912 are presented. The JHK' images reveal an embed-ded infrared cluster associated with infrared nebula, and the H_2 (2.12μm) narrow-band image provides for the first time evidence of outflow activity associated withthe cluster. That the cluster is young can be shown by the high percentage ofinfrared excess sources and the outflow activity. We suggest an age of the clus-ter of ～ 10~6yr. Eight young stars are found in the bright nebular core aroundIRAS 23151+5912. By the color-magnitude diagrams of the cluster, we found fivehigh--mass YSOs and four intermediate-mass YSOs in the cluster. Eight H_2 emissionfeatures are discovered in the region with a scattered and non-axisymmetric distri-bution, indicating the existence of multiple outflows driven by the cluster. DiffuseH_2 emission detected to the north and to the west of the cluster may result fromUV leakage of the cluster. Brγ, H_2, and CIV emission lines are     

天文选址相机的研制

详细介绍了天文选址用CCD相机的开发研制．系统探测器选用具有累进扫描模式的ICX098ALCCD芯片，采用相关双采样信号读出电路、USB通讯接口实现数据与命令的传输．对系统工作性能进行了详细的测试：12℃条件下暗流约为52adu／see，系统增益(system gain)为2.2e／adu，读出噪声(readout noise)为30e．最后给出了在日本冈山天体物理观测所对大气宁静度的实测结果，该结果与冈山已有仪器测量值吻合．     

我国古代记录的特殊流星现象与现代印证

中国古代有着大量的对于流星和流星雨的观测记录，最早可以追溯到3000多年以前。在这些珍贵的记录中，不仅有对于流星的一般描述，而且还有一些至今不能完全理解的特殊流星现象的记录。基于现代对电声变换流星声、流星体的螺旋线形运动、流星的颜色变化和流星的分裂等等的研究，列出在中国古代文献中可以查找到的有关记录。这些记录，不仅是世界文化宝库的一部分，而且对于今天的研究仍有实用价值。对电声变换流星声的报道，只是近20年来，才确立了的并非是观测者的臆想。流星的现代彩色照相观测，更真实地记录和展现了其他的特殊流星现象和它们的发生与演变。这些古代记录与现代的流星观测的对比，可以起到相互印证的作用。     

Chandler Wobble Period and Q Derived by Wavelet Transform

We apply complex Morlet wavelet transform to three polar motion dataseries, and derive quasi-instantaneous periods of the Chandler and annual wobbleby differencing the wavelet transform results versus the scale factor, and then findtheir zero points. The results show that the mean periods of the Chandler (annual)wobble are 430.71±1.07 (365.24±0.11) and 432.71±0.42 (365.23±0.18) mean solardays for the data sets of 1900-2001 and 1940-2001, respectively. The maximumrelative variation of the quasi-instantaneous period to the mean of the Chandlerwobble is less than 1.5% during 1900-2001 (3%--5% during 1920-1940), and thatof the annual wobble is less than 1.6% during 1900--2001. Quasi-instantaneous andmean values of Q are also derived by using the energy density-period profile of theChandler wobble. An asymptotic value of Q = 36.7 is obtained by fitting polynomialof exponential of σ~(-2) to the relationship between Q and σ during 1940--2001.     

非圆轨道GPS/LEO掩星反演地球大气参数的算法及讨论

在非圆轨道GPS和LEO卫星条件下，给出一种较为直接的GPS／LEO掩星反演地球大气参数技术中弯曲角序列的迭代算法，并在理论上对该迭代法的收敛性进行了严格的数学证明．利用GPS掩星反演模拟程序，定量估算了卫星圆轨道假设对GPS／LEO掩星反演地球大气参数的影响，并验证了在非圆轨道条件下各种迭代法的一致性．指出了文献中给出的级数展开迭代算法的不足之处．     

Atmospheric and Oceanic Excitations to LOD Change on Quasi-biennial Tune Scales

We use wavelet transform to study the time series of the Earth's rotation rate (length-of-day, LOD), the axial components of atmospheric angular momentum (AAM) and oceanic angular momentum (OAM) in the period 1962-2005, and discuss the quasi-biennial oscillations (QBO) of LOD change. The results show that the QBO of LOD change varies remarkably in amplitude and phase. It was weak before 1978, then became much stronger and reached maximum values during the strong El Nino events in around 1983 and 1997. Results from analyzing the axial AAM indicate that the QBO signals in axial AAM are extremely consistent with the QBOs of LOD change. During 1963-2003, the QBO variance in the axial AAM can explain about 99.0% of that of the LOD, in other words, all QBO signals of LOD change are almost excited by the axial AAM, while the weak QBO signals of the axial OAM are quite different from those of the LOD and the axial AAM in both time-dependent characteristics and magnitudes. The combined effects of the axial AAM and OAM can explain about 99.1% of the variance of QBO in LOD change during this period.     

The Lembang's Photographic Observations on Sirius

1　ＩｎｔｒｏｄｕｃｔｉｏｎＳｉｒｉｕｓ (α2 0 0 0 =6 ｈ45 ｍ2 ,δ2 0 0 0 =- 1 6°41′) ,ｔｈｅｂｒｉｇｈｔｅｓｔｓｔａｒｉｎｔｈｅｓｋｙ ,ｉｓａｄｏｕｂｌｅｓｔａｒｓｙｓｔｅｍｗｉｔｈｌａｒｇｅｍａｇｎｉｔｕｄｅｄｉｆｆｅｒｅｎｃｅｂｅｔｗｅｅｎｔｈｅｔｗｏｃｏｍｐｏｎｅｎｔｓ (Ｖ =- 1 5 8ｆｏｒｔｈｅｂｒｉｇｈｔｅｒｓｔａｒａｎｄ 8 44ｆｏｒｔｈｅｓｅｃｏｎｄａｒｙ) .Ｔｈｉｓｙｉｅｌｄｓｖｉｓｕａｌｏｂｓｅｒｖａｔｉｏｎｓｔｏｂｅｍａｄｅｏｎｌｙｗｈｅｎｔｈｅｓｅｐａｒａｔｉｏｎｓａｒｅｌａ…     

丽江高美古的天文观测条件

综述对丽江高美古的视宁度、天光亮度、消光系数进行观测的原理、仪器、观测方法和结果．结果表明,高美古是我国南方的优良光学天文台址,视宁度达到世界优良台址的水平