STUDY ON THE CAUSE OF HEAVY RAIN 200506 （HR200506） IN GUANGDONG

A continuous heavy rain visited Guangdong province during June 18-25, 2005 (named Heavy Rain 200506, HR200506) and had resulted in enormous economic loss. The ageostropic Q vectors, θse,meridional circulation, computed from the NCEP reanalysis, and TBB are used to study the rainfall processes. The results indicated that a convective system moved northwards from the South China Sea (SCS)and stayed in Guangdong for several days, which was a direct cause of HR200506. The process is a result of the activity of the South China Sea summer monsoon. There were two rainbands of HR200506 in Guangdong. One laid in the north of Guangdong that produced frontal rainfall; another situated on the south of Guangdong which produced monsoon rainfall.     

2005年11月哈密暴雪天气 过程的诊断分析

2005年11月18日凌晨至20日，哈密出现罕见暴雪天气过程，此次降雪强度大，范围集中，南部大，北部小。利用NCEP1°×1°的6小时分析资料和非常规观测资料，对此次哈密地区的暴雪天气过程的环流背景、影响天气系统进行了动力和热力的诊断分析，并利用Q矢量及螺旋度方法作了天气动力学诊断分析。结果表明：（1）新疆西部高压脊东移发展，引导萨彦岭低涡东移南压，移入哈密地区，造成哈密暴雪天气。（2）萨彦岭低涡是一较深厚系统，是低层辐合高层辐散的垂直上升气旋性涡柱，为暴雪发生提供了有利的动力机制。（3）冷暖平流交汇，增强了斜压性，有助于低涡的发展加强。冷平流对锋生起到重要作用。（4）Q矢量辐合区及螺旋度正值区与低涡有较好的对应关系，对哈密降雪的预报有一定的指示作用。     

一次辽宁秋季暴雨天气的诊断分析

使用1.0°×1.0°NCEP再分析资料,对2006年10月21—22日深秋暴雨在天气形势分析的基础上,进行物理量诊断。结果表明:在有利的环境背景形势下,高位涡从对流层高层向低层伸展并形成湿位涡柱,引起气旋性环流与低涡环流叠加。对流层低层的湿斜压性增强,引起低层的锋区加强及垂直涡度发展,高空入侵干冷空气锲入底层,低层暖湿空气强迫抬升,使地面发展为气旋;高低空急流耦合产生上升气流,同时较强的补偿下沉运动激发上升运动加强,使次级环流加强,触发不稳定能量的释放;低空急流和超低空急流向辽宁输送暖湿空气及能量,对流层中低层形成湿柱并积聚高不稳定能量;中尺度气旋、高低空急流、湿位涡柱、次级环流上升支、地面高水汽含量湿区、高假相当位温出现的时间、强度、位置和结构决定了暴雨的时间和落区。     

阿拉斯加巴罗AB—67钻孔岩芯的沉积环境分析

巴罗ＡＢ－６７钻孔岩芯的４８个样品被进行了２５个项目的粒度分析和４４个项目的地球化学分析。本文对这些数据进行了Ｑ型因子分析,并得到了４个主因子。研究表明,这４个因子分别代表了沉积环境的四项指标,它们分别为沉积速率,降水,海平面和温度。从岩芯顶部５个样品与巴罗气象台观测记录研究了古温度和古降水的转换函数,从＾２１０Ｐｂ测年和几个环境事件确定了沉积速率的转换函数。     

Coda Q before and after the eruptions of 13 November 1985, and 1 September 1989, at Nevado del Ruiz Volcano, Colombia

 Coda Q^–1 was calculated at Nevado del Ruiz Volcano (NRV) before and after two phreatomagmatic eruptions (November 1985, September 1989) and for a period of stability (May 1987) using a functional form for coda derived from a single scattering model (Sato 1977). Substantial changes were found before and after the eruptions. The highest value of Q^–1 was found during the November 1985 eruption, an intermediate value for the September 1989 eruption, and the lowest value for May 1987. It seems that the changes in coda Q^–1 at NRV have a still-unknown relationship with the volume or magnitude of the eruption. A relatively strong frequency dependence was found for all periods. Also Q^–1 clearly changed with time, suggesting that the scattering was strong for the eruption of November 1985 and decreased for the eruption of September 1989, and that the intrinsic absorption probably increased. This suggests the possibility that crystallization is taking place in the NRV magma. The clear change of coda Q^–1 before and after the eruptions at NRV also suggests the possibility that coda Q^–1 is a premonitory tool of activity at this volcano. Received: 25 October 1996 / Accepted: 21 January 1998     

西昌地区地方震尾波衰减Q值

基于单次散射模型的尾波动功率谱分析法,利用西昌遥测台网地震波实时处理系统记录的２４个地震数字化波形资料,计算了西昌地区地球介质对应于１３个不同的ＱＣ值,在１．０－２０．０Ｈｚ频率范围内,以幂函数ＱＣ＝ＱＣｆ＾ｎ拟合ＱＣ值随的变化关系,其中Ｑ０值在４３．０－８２．４之间,ｎ值在０．２４－０．９４之间,平均值分别为６６．２和０．５３。     

双复杂介质条件下的反Q滤波偏移延拓算子研究

地下介质的非弹性吸收衰减效应造成地震资料中深层信号频带窄、能量弱、成像困难,因此需要对地层的非弹性吸收衰减进行补偿。在已有的补偿方法基础上,基于单程波方程,采用与品质因子和频率相关的复速度代替介质真实速度,将粘滞传播算子在频率—空间域采用连分式展开,得到相移项和补偿项,针对连分式的误差,在频率—波数域进行补偿校正,并用逐步累加法解决起伏地表问题。该方法提高了成像精度,有效补偿了由于地层非弹性吸收造成的振幅和频率损失。模型试算和实际资料处理表明,该方法具有一定的适应性和实用性。     

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Short time-scale fluctuations in the difference light curves of QSO 0957+561A,B: microlensing or noise?

From optical R -band data of the double quasar QSO 0957+561A,B, we made two new difference light curves (with an overlap of about 330 d between the time-shifted light curve for the A image and the magnitude-shifted light curve for the B image). We observed noisy behaviours around the zero line and no short time-scale events (with a duration of months), where the term 'event' refers to a prominent feature that may be a result of microlensing or another source of variability. Only one event lasting two weeks and rising −33 mmag was found . Measured constraints on the possible microlensing variability can be used to obtain information on the granularity of the dark matter in the main lensing galaxy and the size of the source. In addition, one can also test the ability of the observational noise to cause the rms averages and the local features of the difference signals. We focused on this last issue. The combined photometries were related to a process consisting of an intrinsic signal plus a Gaussian observational noise. The intrinsic signal has been assumed to be either a smooth function (polynomial), a smooth function plus a stationary noise process, or a correlated stationary process . Using these three pictures without microlensing, we derived some models totally consistent with the observations. We finally discussed the sensitivity of our telescope (at Teide Observatory) to several classes of microlensing variability.