Identification method of weak seismic phases on the basis of wavelet packet transform   总被引：1，自引：0，他引：1  

Xi-Qiang Liui  Hui-Lan Zhou  Zhi-Zhen Zheng  Ping Shen  Xuan-Hui Yang  Yan-Lu Ma 《地震学报(英文版)》1998,11(4):431-439

This paper describes a sort of new method identifying seismic phase by the name of wavelet packet transform. Perfectness and development of the wavelet packet transform is based upon the idea of its multiscale analysis. The method of wavelet packet transform can depict the anomalous changes information of transient spectra of seismic wave onset, and come true the target of identifying seismic phase especially weak seismic phase. Then this paper presents discriminating examples of simulating digital signals and actual seismic phase. Compared with conventional seismic phase discrimination, studied results show that the wavelet packet transform method is an available tool of weak signal analyses, and have unexampled merits and attractive application foreground. This research gets hold of Higher School Doctor Scientific Research Foundation (No. 157 WJ0704 9435611) and supported by the National Natural Science Foundation (No. 49474211).  相似文献   

弱流场调制下的海面微波散射模拟研究          下载免费PDF全文

吕伟艳  赵朝方  杜涛 《海洋科学》2008,32(7):57-61

根据海面微波散射的多尺度模型以及波流相互作用理论，对一维弱流场调制下的海面微波散射截面进行了数值模拟。结果表明，利用数值方法直接求解波作用量方程获得的海浪调制谱并结合多尺度模型可以较好地模拟弱流场引起的雷达散射截面的变化。内波等海洋现象调制了海浪谱，使得雷达散射截面反映出这些海洋特征，整个调制过程的模拟对于分析这些海洋现象并更好地利用其雷达数据具有重要意义。  相似文献   

Simulations for multi-object spectrograph planet surveys     

Stephen R. Kane  Donald P. Schneider  Jian Ge 《Monthly notices of the Royal Astronomical Society》2007,377(4):1610-1622

Radial velocity surveys for extrasolar planets generally require substantial amounts of large telescope time in order to monitor a sufficient number of stars. Two of the aspects which can limit such surveys are the single-object capabilities of the spectrograph, and an inefficient observing strategy for a given observing window. In addition, the detection rate of extrasolar planets using the radial velocity method has thus far been relatively linear with time. With the development of various multi-object Doppler survey instruments, there is growing potential to dramatically increase the detection rate using the Doppler method. Several of these instruments have already begun usage in large-scale surveys for extrasolar planets, such as Fibre Large Array Multi Element Spectrograph (FLAMES) on the Very Large Telescope (VLT) and Keck Exoplanet Tracker (ET) on the Sloan 2.5-m wide-field telescope.
In order to plan an effective observing strategy for such a program, one must examine the expected results based on a given observing window and target selection. We present simulations of the expected results from a generic multi-object survey based on calculated noise models and sensitivity for the instrument and the known distribution of exoplanetary system parameters. We have developed code for automatically sifting and fitting the planet candidates produced by the survey to allow for fast follow-up observations to be conducted. The techniques presented here may be applied to a wide range of multi-object planet surveys.  相似文献   

A Bayesian periodogram finds evidence for three planets in HD 11964     

P. C. Gregory † 《Monthly notices of the Royal Astronomical Society》2007,381(4):1607-1616

A Bayesian multiplanet Kepler periodogram has been developed for the analysis of precision radial velocity data. The periodogram employs a parallel tempering Markov chain Monte Carlo algorithm. The HD 11964 data have been re-analysed using 1, 2, 3 and 4 planet models. Assuming that all the models are equally probable a priori, the three planet model is found to be ≥600 times more probable than the next most probable model which is a two planet model. The most probable model exhibits three periods of  38.02^+0.06_−0.05, 360⁺⁴₋₄ and 1924⁺⁴⁴₋₄₃ d  , and eccentricities of  0.22^+0.11_−0.22, 0.63^+0.34_−0.17 and 0.05^+0.03_−0.05  , respectively. Assuming the three signals (each one consistent with a Keplerian orbit) are caused by planets, the corresponding limits on planetary mass ( M sin  i ) and semimajor axis are     respectively. The small difference (1.3σ) between the 360-d period and one year suggests that it might be worth investigating the barycentric correction for the HD 11964 data.  相似文献   

WASP-1b and WASP-2b: two new transiting exoplanets detected with SuperWASP and SOPHIE   总被引：1，自引：0，他引：1  

A. Collier Cameron  F. Bouchy  G. Hébrard  P. Maxted  D. Pollacco  F. Pont  I. Skillen  B. Smalley  R. A. Street  R. G. West  D. M. Wilson  S. Aigrain  D. J. Christian  W. I. Clarkson  B. Enoch  A. Evans  A. Fitzsimmons  M. Fleenor  M. Gillon  C. A. Haswell  L. Hebb  C. Hellier  S. T. Hodgkin  K. Horne  J. Irwin  S. R. Kane  F. P. Keenan  B. Loeillet  T. A. Lister  M. Mayor  C. Moutou  A. J. Norton  J. Osborne  N. Parley  D. Queloz  R. Ryans  A. H. M. J. Triaud  S. Udry  P. J. Wheatley 《Monthly notices of the Royal Astronomical Society》2007,375(3):951-957

We have detected low-amplitude radial-velocity variations in two stars, USNO-B1.0 1219–0005465 (GSC  02265–00107 = WASP–1  ) and USNO-B1.0 0964–0543604 (GSC  00522–01199 = WASP–2  ). Both stars were identified as being likely host stars of transiting exoplanets in the 2004 SuperWASP wide-field transit survey. Using the newly commissioned radial-velocity spectrograph SOPHIE at the Observatoire de Haute-Provence, we found that both objects exhibit reflex orbital radial-velocity variations with amplitudes characteristic of planetary-mass companions and in-phase with the photometric orbits. Line-bisector studies rule out faint blended binaries as the cause of either the radial-velocity variations or the transits. We perform preliminary spectral analyses of the host stars, which together with their radial-velocity variations and fits to the transit light curves yield estimates of the planetary masses and radii. WASP-1b and WASP-2b have orbital periods of 2.52 and 2.15 d, respectively. Given mass estimates for their F7V and K1V primaries, we derive planet masses 0.80–0.98 and 0.81–0.95 times that of Jupiter, respectively. WASP-1b appears to have an inflated radius of at least 1.33 R _Jup, whereas WASP-2b has a radius in the range 0.65–1.26 R _Jup.  相似文献   

新一代天气雷达(CINRAD)体扫模式起始仰角探讨     

卢兴来  邵伟军 《成都信息工程学院学报》2007,22(5):633-636

CINRAD所采用的各种体扫模式(VCP)均以仰角0.5°为起始进行扫描,通过分析雷达发射波束宽度、地物杂波对产品影响、雷达测量低仰角回波的重要性等因素,提出了CINRAD在低仰角观测时选取低仰角的原则,以及低仰角观测时应注意的问题.  相似文献   

南黄海辐射沙脊群西洋水道污水输移扩散研究   总被引：1，自引：0，他引：1  

周智鹏  陶建峰  张长宽  徐凡  姚静 《海洋通报》2015,34(1):65-71

采用沿深平均二维数值模型对南黄海辐射沙脊群西洋海域的潮流场和物质扩散场进行了模拟,计算和分析了大潮情况下海域5 m、7 m和10 m 3种水深(理论基准面下)排放位置处达标污水输移扩散的范围及分布规律。结果表明,污水排入海后,会很快被稀释,各排放位置200和500稀释度等值线包络面积均较小,且包络面积随水深增加有明显变小的规律。拟合了不同污水排放量对应的200和500稀释倍数包络面积,发现两者呈良好的幂级数关系。  相似文献   

条子泥一期工程对条子泥发育影响及工程防护措施   总被引：2，自引：0，他引：2  

陈才俊  徐向红 《海洋工程》2015,33(5):105-112

通过历史和现场观测资料并结合遥感卫片资料,对条子泥匡围一期工程两年多的建设过程中,由工程所引起对条子沙洲西大港、东大港、条鱼港等主要的潮沟,及相应的潮盆系统和二分水的剧烈变化进行了分析研究,总结了潮沟摆动治理经验。治理方法主要为丁坝群结合砼连锁块镇压排布防护技术等。  相似文献   

2013年7月1日河北宁晋极端短时强降水成因研究     

王丛梅  俞小鼎 《湖北气象》2015,(2):105-116

2013年7月1日午后至夜间,华北出现一次区域性暴雨和局地大暴雨过程。局地极端降水出现在河北省邢台市宁晋县四芝兰镇,过程雨量409 mm,其中当日17—19时连续2 h雨量超过100 mm。利用常规高空和地面观测资料、NCEP再分析资料和石家庄新一代天气雷达资料,探讨了宁晋极端短时强降水的形成原因。主要结论是:(1)低槽、冷锋、副热带高压及其外围低涡切变线为其主要影响系统,海南附近台风远距离影响加强了水汽自南向北的输送,半定常的地面辐合切变线对新生对流的触发和已有对流的维持及加强起到重要作用;(2)宁晋最强降水期间,其上空具有较强的垂直风切变,有利于高度组织化的对流系统发展;(3)对流系统的后向传播使回波主体移动缓慢、持续时间长,而回波强度大和雨强很强,则导致四芝兰镇极端强降水,此外,具有弱中气旋的超级单体相对较长时间的影响使其对四芝兰镇强降水具有重要贡献;(4)产生极端降水的对流系统属于高质心发展强烈的大陆强对流型,而非更易导致强降水的低质心系统。同时,针对众多学者研究北京"7.21"特大暴雨得到的一些结论进行了进一步探讨和验证。  相似文献   

重庆“5.6”强风雹天气过程成因分析   总被引：8，自引：4，他引：8  

陈贵川  谌芸  乔林  刘德  李强  张亚萍  王文芳  张焱 《气象》2011,37(7):871-879

利用常规观测、NCEP分析场及雷达、自动站等资料对重庆＂5.6＂强风雹天气的成因进行了分析,结果表明：冷锋和副热带高空急流在风雹发生地近乎重叠的配置结构促进了次级环流的形成并有利于上升运动的强烈发展;风暴天气发生前,下垫面强烈加热、低层增温增湿、中高层干冷对大气对流不稳定性增强的作用显著;对流有效位能（CAPE）、K指数、SI指数高值区边缘的强指数梯度区、对流抑制（CIN）的小值区以及较强的垂直风切变对大风冰雹的预报有重要的指示意义;雷达回波显示多单体风暴具有三体散射、弱回波区等冰雹回波特征,中层径向辐合和反射率因子核心的反复上升下降也是形成地面大风和冰雹的重要特征;四川盆地东部东北西南向山脉对冷空气的移动有阻挡作用,山脉之间的槽状地形为多单体风暴的持续发展保留了较大的空间,明月山南麓的地形起到了强迫抬升和触发的作用,由于地形的阻挡形成狭管效应,加强了下击暴流形成的地面大风,是形成11级大风的重要因素。  相似文献