大气中低频重力波指数与西南低涡发展及其暴雨的关系

采用低频重力波指数法，对西南低涡发展演变及其暴雨强度，落区进行了诊断分析和预测。结果指出：（１）低频重力波指数Ｃｐ，Ｃｉ对西南低涡的发展及其暴雨强度，落区都有一定的预测意义，其预见期可达２４小时以上；（２）低频重力波指数随时间变化与西南低涡发有较好的对应关系；（３）低频重力波指数的大小与西南低涡暴雨强度相联系；（４）西南低涡暴雨落区通常发生在Ｃｐ，Ｃｉ指数的最大负值区内和Ｃｐ等值线梯度最大的区域。     

亚洲夏季风系统水汽输送的季节平均和低频结构

应用欧洲中期预报中心１９８０－１９８６年５－９月的８５０ｈＰａ逐日资料，分析了亚洲夏季风系统水汽输送的平均结构和低频结构。研究指出，从季节平均结构来看，亚洲季风系统是一个完整的体系。从低频活动结构看，亚洲夏季风系统中存在着印度季风和东亚季风系统的相对独立性。     

1991年北半球夏季风及江淮流域降雨量的低频振荡

根据１９９１年５－８月江淮特大暴雨资料，使用功率谱和带通滤波结合的方法，研究了１９９１年夏季风和江淮梅雨的准周期振荡，探索季风对异常梅雨的影响。分析指出，１９９１年北半球夏季风活动，江淮流域湿度场和降雨量变化均存在显著的准２４天周期振荡，夏季风的周期振荡，主要表现在西南季风（东南季风不明显），它的位相比降雨量提前２－４左右，其振幅大小较好地反映了降雨量的大小。     

Low-latitude total ozone measurements in the Brazilian sector

Regular measurements of the atmospheric ozone in the Brazilian sector were started at Cachoeira Paulista (22.7°S, 45.0°W), and Natal (5.8°S, 35.2°W) in May 1974 and November 1978, respectively. The results of the total ozone measurements carried out at these two stations up to 1981 are presented in this communication and compared with other low-and mid-latitude stations. Although Natal is an equatorial station, it presents a prominent annual variation, and the average total ozone content is high compared to satellite measurements. During 1977–78, abnormally low values of total ozone were observed at Cachoeira Paulista. Some preliminary results about the QBO 9quasi-biennial oscillation) during 1974–81 are also presented.     

THE RELATIONSHIP BETWEEN THE MOVEMENT OF THE MEIYU/BAIU RAIN BELT AND THE PERIODIC NORTHWESTWARD PROPAGATION OF THE CONVECTIVE ACTIVITY FROM TROPICAL WEST PACIFIC

In order to investigate the effect of the factors in tower latitudes on Meiyu/Baiu front,adiagnostic analysis for the two cases during June to July of 1985 and 1986 was examined.We foundthat (1)when the tropical convective activity moves westward to 10.5-15.5′N/140°E from eastside of 10.5-15.5°N/160°E,the northward shifts of the Meiyu/Baiu rain belt occurs;(2)themain factor which results in the northward and southward shifts of Meiyu/Baiu rain belt is thoughtas the 8,18 and 30 day oscillations of the tropical convective activity around West Pacific.Meanwhile,the wave train propagating from Lake Baikal via Okhotsk Sea to the tropics couldsometimes shift Baiu rain belt southward;(3)the onsets of Meiyu in China of both cases tend totake place just when the convective activity around lower latitudes moves westward through about140°E with the 8,18 and 30 day oscillation periods firstly coming to June.     

V473 Lyrae: a Blazhko-effect Cepheid?

The amplitude spectra of the light curves of RR Lyrae Blazhko stars can often be typified by symmetrical triplets. It is shown that the same applies to V473 Lyr. Furthermore, the star is probably a radial pulsator – as is thought to be the case for the RR Lyrae stars – thus ruling out rotational splitting of a purely non-radial mode.     

The heating of the solar corona

The heating of the solar corona has been a fundamental astrophysical issue for over sixty years. Over the last decade in particular, space-based solar observatories (Yohkoh, SOHO and TRACE) have revealed the complex and often subtle magnetic-field and plasma interactions throughout the solar atmosphere in unprecedented detail. It is now established that any energy release mechanism is magnetic in origin - the challenge posed is to determine what specific heat input is dominating in a given coronal feature throughout the solar cycle. This review outlines a range of possible magnetohydrodynamic (MHD) coronal heating theories, including MHD wave dissipation and MHD reconnection as well as the accumulating observational evidence for quasi-periodic oscillations and small-scale energy bursts occurring in the corona. Also, we describe current attempts to interpret plasma temperature, density and velocity diagnostics in the light of specific localised energy release. The progress in these investigations expected from future solar missions (Solar-B, STEREO, SDO and Solar Orbiter) is also assessed.Received: 6 February 2003, Published online: 14 November 2003 Correspondence to: R. W. Walsh     

Mode Identification from Line Profiles using the Direct Fitting Technique

The method of moments and the direct fitting method are the onlyspectroscopic methods of mode identification which allow a determination ofall pulsational parameters. The pulsation parameters are required to predictthe light amplitude and phase which can be important discriminants in modeidentification. The direct fitting method has several advantages over themethod of moments. It is not restricted to low spherical harmonic degree or form of the eigenfunction and is not sensitive to the placement of the continuum. In the last few years the method has been applied to several different types of stars. We briefly describe the method and give someexamples of its application.