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21.
采用TOGA/COARE国际合作考察期间(1992年10月─1993年2月)获得的267次定点(2°S,155°E)定时高空大气探测资料,进行计算分析,发现1992年12月─1993年2月低空存在一支西风急流,有两次分别持续半月之久,而1992年11月的两次赤道西风急流,因无赤道高空急流配合,仅持续2d便消失。本文还指出:(1)赤道低空西风急流是各种海-气指数产生ENSO异常的重要信息;(2)赤道高空急流有滞后赤道低空急流2d左右的响应关系;(3)赤道低空急流是纬向水汽输送的狭窄通道。 相似文献
22.
Wave induced excess flow of momentum(WIEFM)is the averaged flow of momentum over a wave period due to wave presence,which may also be called 3-D radiation stress.In this paper,the 3-D current equations with WIEFM are derived from the averaged Navier-Stokes equations over a wave period,in which the velocity is separated into the large-scale background velocity,the wave particle velocity and the turbulent fluctuation velocity.A concept of wave fluctuating layer(WFL)is put forward,which is the vertical column from the wave trough to wave ridge.The mathematical expressions of WIEFM in WFL and below WFL are given separately.The parameterized expressions of WIEFM are set up according to the linear wave theory.The integration of WIEFM in the vertical direction equals the traditional radiation stress(namely 2-D radiation stress)given by Longuet-Higgins and Stewart. 相似文献
23.
Phytoplankton variability on the Faroe Shelf 总被引:2,自引:2,他引:2
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好望角附近海域春季大风的几种主要形势分析 总被引:1,自引:1,他引:1
通过普查和分析,概括出了春季好望角附近海域三种主要大风出现时的模型图,并以一个月中逐日4次船舶测风报告为例,分析了好望角大风的某些主要特征。 相似文献
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Any calculation of seismic wave propagation comprising the seismic source, the travel path, and the receiver site in a single finite-difference (FD) model requires a considerable amount of computer time and memory. Moreover, the methods currently available for including point sources in the 2D FD calculations are far-field approximations only. Therefore we have developed a new hybrid method for treating the seismic wave fields at localized 2D near-surface structures embedded in a 1D background medium, and excited by a point source. The source radiation and propagation in the background model is solved by the discrete-wave number (DW) method, while the propagation in the local 2D structure is calculated by the FD method. The coupling between the two sets of calculations is performed on a rectangular excitation box surrounding the local structure. We show the usefulness of the method in ground-motion studies where both near-field source effects and local site effects are important. Technical problems connected with the inconsistency between the 3D source radiation and the 2D FD calculation are minor for the relatively distant in-plane point explosive sources, but are more serious for the in-plane dislocation sources. 相似文献
29.
为研究地铁建设对济南白泉泉群的影响,在综合分析白泉泉域地质、水文地质条件的基础上,假定研究区岩溶强径流带位置及水力性质,利用FEFLOW软件建立地下水流数值模型。以规划地铁M1号线为研究对象,分析了济南东站、梁王站、梁王东站分别施工及3个站同时施工4种情景下,采用施工降水或施工降水+人工回灌两种施工方式对白泉泉群流量的影响。结果表明:单独采用施工降水的施工方式使得白泉泉群流量衰减,其中3个站同时施工对泉流量的影响最大,泉流量最大衰减达5.48%;各站分别施工时,济南东站对泉流量影响最大,泉流量较未施工时减少了0.043×104 m3/d。采用施工降水+人工回灌的施工方式,能够有效缓解泉流量的衰减,各车站施工时的泉流量衰减由仅施工降水时的2.26%~5.48%降低至0.08%~1.21%。岩溶强径流带有利于地下水形成优势径流,促进白泉泉群补给,一定程度上缓解因地铁施工引起的泉流量衰减。 相似文献
30.
A. V. Krivov L. L. Sokolov V. V. Dikarev 《Celestial Mechanics and Dynamical Astronomy》1995,63(3-4):313-339
This paper deals with dynamics of impact ejecta from Phobos and Deimos initially on near-circular equatorial orbits around Mars. For particles emitted in a wide size regime of 1 micron and greater, and taking into account the typical particle lifetimes to be less than 100 years, the motion is governed by two perturbing forces: solar radiation pressure and influence of Mars' oblateness. The equations of motion of particles in Lagrangian non-singular elements are deduced and solved, both analytically and numerically, for different-sized ejecta. We state that the coupled effect of both forces above is essential so that on no account can the oblateness of Mars are be neglected. The dynamics of grains prove to be quite different for the ejecta of Phobos and Deimos. For Deimos, the qualitative results are relatively simple and imply oscillations of eccentricity and long-term variations of orbital inclination, with amplitudes and periods both depending on grain size. For Phobos, the dynamics are shown to be much more complicated, and we discuss it in detail. We have found an intriguous peculiar behavior of debris near 300 µm in size. Another finding is that almost all the Phobos ejecta with radii less than 30 µm (against the values of 5 to 20 µm adopted earlier by many authors) should be rapidly lost by collisions with martian surface. The results of the paper may be the base for constructing an improved model of dust belts that presumably exist around Mars. 相似文献