2005/2006年度莱州湾东部的海冰灾害及其影响

莱州湾是水深较浅的半封闭海湾,与外海海水的交换缓慢,受黄河等十几条入海河流汇入的淡水影响使海水的盐度较低.受寒潮影响莱州湾内海冰灾害发生频繁.莱州湾的海冰灾害分5个冰情等级.在冬季气温偏高的年份,莱州湾内形成Ⅰ、Ⅱ级海冰,沿岸一般没有固定冰形成;一般年份形成Ⅲ级海冰,西岸和南岸冰情较严重,有固定冰形成;在冬季气温偏低的年份,形成Ⅳ级或Ⅴ级海冰,南岸、西岸的固定冰宽度较大,有时整个莱州湾海面都分布流冰.2005年末～2006年初在莱州湾东岸形成了一次较严重的海冰灾害,莱州市近海海湾扇贝养殖的经济损失达400万元以上.为减轻未来海冰灾害带来的损失提出了加强海冰灾害的监测和预报技术研究,严格管理近海养殖生产作业,莱州湾沿岸地方政府应制定<海冰灾害应急预案>,建设和完善海冰灾害应急防御体系等防御海冰灾害的对策.     

Limits on the 2.2-μm contrast ratio of the close-orbiting planet HD 189733b

We obtained 238 spectra of the close-orbiting extrasolar giant planet HD 189733b with resolution   R ∼ 15 000  during one night of observations with the Near-Infrared High-Resolution Spectrograph (NIRSPEC), at the Keck II Telescope. We have searched for planetary absorption signatures in the  2.0–2.4 μm  region where H₂O and CO are expected to be the dominant atmospheric opacities. We employ a phase-dependent orbital model and tomographic techniques to search for the planetary absorption signatures in the combined stellar and planetary spectra. Because potential absorption signatures are hidden in the noise of each single exposure, we use a model list of lines to apply a spectral deconvolution. The resulting mean profile possesses a signal-to-noise ratio (S/N) that is 20 times greater than that found in individual lines. Our spectral time series thus yields spectral signatures with a mean S/N = 2720. We are unable to detect a planetary signature at a contrast ratio of  log₁₀( F _p/ F _*) =−3.40  , with 63.8 per cent confidence. Our findings are not consistent with model predictions which nevertheless give a good fit to mid-infrared observations of HD 189733b. The 1σ result is a factor of 1.7 times less than the predicted 2.185-μm planet/star flux ratio of  log₁₀( F _p/ F _*) ∼−3.16  .     

关于正确处理对流－弥散方程和渗流方程中源汇项的若干问题

对流─弥散方程和渗流基本微分方程中的源汇项，分别是决定含水层中任一内点上水质量和溶质质量时变率的重要因素之一。而关于源汇项不适当的乃至是错误的表述，在文献中却不乏其见，其影响之大是显而易见的．本文深入分析了某些表述的不当或错误之处，给出了正确的处理与表述方法。     

TPS测设道路填挖边线方法探讨

道路建设中,测设填挖线是经常遇到的问题,就此提出了TPS(全站仪)在任意控制点设站、测定辅助点和填挖点的放样方法。该方法的关键之处是,利用曲线要素推算各放样点的坐标,然后在道路施工现场附近选择一视野开阔的控制点安置TPS,一次性放样出全视野内的辅助点和填挖点,并连接填挖点组成填挖边线。为保证各阶削坡的精度,应注意保护各辅助点的平面位置,正确地削出最上阶平台,以控制以下各阶削坡。而以往的放样方法是抬竿法,需要在逐个横断面多次设站,用定向、量距、抬高的方法放样填挖点。这种方法的缺点是:效率低下,作业难度大,累计误差大。显然,用TPS一次设站,放样若干横断面填挖点的方法,提高了施工效率,降低了作业难度,且提高了放样点的精度。     

Extragalactic Astronomy with the VLTI: a new window on the Universe

Interferometry in the optical and near infrared has so far played a marginal role in Extragalactic Astronomy. Active Galactic Nuclei are the brightest and most compact extragalactic sources, nonetheless only a very limited number could be studied with speckle interferometry and none with long baseline interferometry. The VLTI will allow the study of moderately faint extragalactic objects with very high spatial resolution thus opening a new window on the universe. With this paper we focus on three scientific cases to show how AMBER and MIDI can be used to tackle open issues in extragalactic astronomy. This revised version was published online in July 2006 with corrections to the Cover Date.