暴雨过程中积云对流反馈作用的诊断研究

根据各收支方程讨论，概述了各研究者采用直接和间接的方法，计算得出长江流域梅雨期暴雨过程中各源汇的空间分布特征。虽然个例，地区和资料不同，其结果各有差异，易比较，但次网格尺度运动对不尺度环境场的反馈作用均非常显著，因而在设计暴雨预报的数值模式时，参数化方案是必不可少的。     

海沟后退对地幔对流的影响

本文分析了有海底扩张无海沟后退、有海沟后退无海底扩张以及海底扩张与海沟后退共存等３种情况下，俯冲板片运动与海沟迁移的关系．用幂律流体有限元方法计算海沟后退对地幔对流的影响．地幔有效粘度除依赖应力偏张量的第二不变量以外，尚与温度、压力（含流体静压力和流动压力）有关．计算表明，对流环、高流动负压区以及低粘区的个数和位置，均受控于海沟是否后退以及海底是否扩张；温度场与海沟后退无明显关系．流动压力对形成洋中脊和弧后火山、驱动地幔对流以及维持板片的倾斜角度都具有重要意义．     

极隙区粒子和电流的观测和研究

处于高纬向日面的极隙区是太阳风能量、动量和质量可以直接进入地球磁场并到达地球的近地空间的区域。本文简要介绍了极隙区的观测和研究，综述了极隙区的粒子沉降、场向电流、等离子体对流和电离层电流的特征。     

莺－琼盆地YA13－1气田热流体活动与有机／无机成岩响应

根据钻井中途测试（ＤＳＴ）、重复地层测试（ＲＦＴ）、镜质体反射率（Ｒ０）、流体包裹体分析和粘土矿物Ｘ射线衍射全定量分析等综合研究发现，莺－琼盆地ＹＡ１３－１气田存在４期热流体活动；南侧的崖南地区和西侧的莺歌海盆地是其两个重要的热流体物质源和动力源；多期热流体活动在ＹＡ１３－１地区不仅造成热异常和物质迁移，而且还引起了不同的有机／无机成岩响应，如骨架颗粒的多期溶蚀作用、至少两期的次生加大作用、粘土矿物转化和有机质热成熟作用异常。第二、第三期热流体因出溶作用形成ＹＡ１３－１气田大规模的天然气聚集。     

地幔对流与岩石层板块的相互耦合及影响──（Ⅰ）球腔中的自由热对流

板块运动是地幔对流的主要证据之一．同时，作为地球动力系统中一个相对独立部分，板块自身的存在和运动对地幔内部物质的流动形态有巨大影响．地幔内部的流动由两部分组成：一是由内部非绝热温度差异造成的自由对流解；另一部分是由在地表运动的板块所激发．作为系列工作的第一部分，本文研究球腔中的自由热对流问题．得到了对地幔对流研究有实际意义的下边界为自由、上边界为刚性情况下的临界瑞利数值，不同的瑞利数时球腔内流场和温度场的分布形态等．     

A preliminary study of the effects of some flow parameters in the generation of poloidal and toroidal energies within a 3-D spherical thermal-convective system with variable viscosity

The effects of variable viscosity on flow dynamics within spherical shells are investigated using a finite-element thermal convection model, and preliminary result for cases with relatively low Rayleigh numbers and small viscosity contrasts are reported. These results demonstrate some general effects of viscosity variation on mantle dynamics, and, in particular, the generation of toroidal energy. Since lateral viscosity variations are necessary in the generation of toroidal motion in a thermally driven convective system, it is not surprising our results show that flows with greater viscosity contrasts produce greater amounts of toroidal energy. Our preliminary study further shows that solutions become more time-dependent as viscosity contrasts increase. Increasing the Rayleigh number is also found to increase the magnitude of toroidal energy. Internal heating, on the other hand, appears to lead to less toroidal energy compared wth bottom heating because it tends to produce a thermally more uniform interior and thus smaller viscosity variations.     

论浙江火山岩区金银矿床的成矿物质来源

稳定同位素和地质特征的研究,结果表明浙江火山岩区金银矿床的成矿物质系多元来源。金属和挥发性组分来源于岩石圈深部(下地壳或上地幔)和上地壳,成矿流体是大量大气水和少量岩浆水的混合溶液.金银矿化与板块运动及地热流体对流体系有关.     

A Note on the Mixing Length Theory and Massive Star Evolution

1 INTRODUCTIONThe mixing length theory (MLT) for stellar convection originally developed by Vitense(1953, 1958) has been the most popularly used local convection theory in the studies of stellarstructure and evolution. The theory was later modified and revised by many investigators,who suggested some different expressions. In fact, MLT is not a real hydrodynamic theory,rather, it is a simple "ballistic" theory which traces the motion of imaginary convective elements. In reality j stell…     

On determining the noon polar cap boundary from SuperDARN HF radar backscatter characteristics

Previous work has shown that ionospheric HF radar backscatter in the noon sector can be used to locate the footprint of the magnetospheric cusp particle precipitation. This has enabled the radar data to be used as a proxy for the location of the polar cap boundary, and hence measure the flow of plasma across it to derive the reconnection electric field in the ionosphere. This work used only single radar data sets with a field of view limited to 2 h of local time. In this case study using four of the SuperDARN radars, we examine the boundary determined over 6 h of magnetic local time around the noon sector and its relationship to the convection pattern. The variation with longitude of the latitude of the radar scatter with cusp characteristics shows a bay-like feature. It is shown that this feature is shaped by the variation with longitude of the poleward flow component of the ionospheric plasma and may be understood in terms of cusp ion time-of-flight effects. Using this interpretation, we derive the time-of-flight of the cusp ions and find that it is consistent with approximately 1 keV ions injected from a subsolar reconnection site. A method for deriving a more accurate estimate of the location of the open-closed field line boundary from HF radar data is described.