现代水下技术在我国水运工程建设中的应用与前景

自本世纪８０年代中期以来，世界水下工程技术随着各国科学水平的提高而得以迅速发展。本文从水下工程技术的专业范畴及特征着手，分析了现代水下技术在水运工程建设中的应用；介绍了国外现代水下技术的基本进展及趋势；评价了国内水下工程技术及装备水平，同时展示了我院近十年来在现代水下技术与装备和开发、应用方面所做的工作与实力；最后分析了国内水运工程建设发展对水下技术的挑战，以及发展我国现代水下技术装备开发研究所面     

卵形鲳鲹早期卵子发生显微及超微结构的研究

本文研究了卵形鲳鲹早期卵子发生的显微与超微结构特点。研究结果表明在1～2龄鱼卵巢中卵原细胞进入首次成熟分裂前期的结构特点，3～4龄鱼才开始进入小生长期，文中讨论了此鱼性腺成熟的年龄以及如何加速性腺发育，为人工繁殖提供科学依据。     

黑潮延伸区的海平面异常和中尺度涡的统计分析

利用1993～2004年卫星高度计TP/Jason-1和 ERS/ENVISAT提供的海平面异常(SLA)融合数据,分析了黑潮延伸区12年来的平均海平面异常的变化特征及中尺度涡的分布规律.研究表明,在黑潮延伸区海平面异常(SLA)呈递增趋势,年平均上升率为8.89mm/a,显著性周期是1年、0.5年和6年;黑潮延伸区的海平面异常和海表面温度异常的低频分量与Nino3指数具有较高的相关性.这说明,黑潮延伸区的海平面变化和海表面温度与厄尔尼诺事件密切相关,都受到黑潮变化的密切影响.在日本东部的黑潮延伸区,中尺度涡自东向西移动,寿命约为1年,移动速度大约是10经度/年.气旋涡和反气旋涡的面积呈现几乎同步增减的规律,均呈年周期变化,上半年少,下半年多.在1997～1998年,黑潮延伸区内中尺度涡的面积显著减小,并且正好对应于Nino3指数极大值出现的年份.因此,黑潮延伸区内中尺度涡的数量和强度也与厄尔尼诺事件密切相关.     

厦门港岩石岸潮间带软体动物的生态

本文根据１９８２年２月至１９８３年２月在厦门港岩石岩潮间带采集的软体动物，论述了其种类组成，数量分布，生活型及影响软件动物分布的主要环境因子，厦门港岩石岸潮间带共发现软动物５４种。其中，多板类６种，腹足类３３种，双壳类１５种，优势种有僧帽牡蛎，黑荞麦蛤，复瓦小蛇螺，粗糙滨螺等。与６０年代初调查结果比较得出，厦门港岩石岸潮间带的软体动物群落是相对稳定的，潮汐是决定河口结果比较得出，厦门港岩石岩潮间带     

福鼎山后尖玄武岩筒地质特征及其形成机制探讨

福鼎山后尖玄武岩位于福鼎一福清北东向断裂带北东段,呈岩筒状产于石帽山群下组下段火山沉积岩中,属钠质碱性玄武岩系列,由玄武质火山角砾岩、碧玄岩、橄榄辉长一玄武岩组合,经历火山爆发、喷溢、次火山侵入3个阶段而形成。     

鄂尔多斯盆地靖边气田马五_(1+2)气藏储集单元研究

综合地震、地质、测井等信息,考虑沉积、成岩、地貌、生产动态等多因素,在沟槽识别和致密带研究基础上,通过井间干扰、油层压力变化和试井边界响应分析,按照局部、就近原则对靖边气田马五1+2气藏进行了储集单元划分。共划分出111个储集单元,其中独立型69个,复合型42个。这些储集单元的面积多介于10～50km2之间,单个储集单元的井数一般少于6口。在对气藏储层特征综合认识的基础上,确定流动单元划分思路与流程,并认为关键环节包括古沟槽识别、致密带研究、动静结合确定储集单元等3个方面。储集单元一方面受控于被致密岩相包围的有利成岩相带,宏观上与弱—中等充填泥粉晶白云岩相对应性好;另一方面又受各级古沟槽夹持,在两个一级古沟槽之间往往共生多个储集单元,而这些储集单元边界又严格地受二级或三级沟槽切割控制。     

Low frequency flickering of TT arietis: Hard and soft X-ray emission region

Using archival ASCA observations of TT Arietis, X-ray energy spectra and power spectra of the intensity time series are presented for the first time. The energy spectra are well-fitted by a two continuum plasma emission model with temperatures 1 keV and 10 keV. A coherent feature at 0.643 mHz appeared in the power spectra during the observation.     

The contact binary system YY Eri

Relatively new and unanalysed photometric data-sets of the contact binary system YY Eri are presented. The light curves have been analysed using information limit optimization techniques, and the Binary Maker program of Bradstreet (1992).Comparison of the results allows insight into determinacy questions affecting the W UMa type of light curve, which relates to our general understanding of contact binaries. A limiting contact configuration cannot be ruled out on the basis of empirical data-analysis alone.Very careful analysis of the photospheric flux distribution over the surface of the Sun may help establish appropriate values of the gravity brightening parameter for cool dwarf stars. At present, however, empirical photometric information on contact binaries is non-discriminatory: i.e. alternative cosmogonies can find alternative support from available evidence. The implication is then for more and better observational data to allow better real independent parameter determination.     

Solar models with strong turbulence

A series of evolutionary models for the Sun were constructed using the strong turbulence model of the variable mixing-length theory (AMLT) of Canuto (1990). The present values of the solar model were obtained by an initial compositionX = 0.754,Z = 0.019, and(x) = 1.1. The physical variables which were obtained by applying the strong turbulence case of AMLT were similar to those of weak turbulence model (Kzlolu and Civelek, 1992) if we focused on the fitting of present solar radius and luminosity.     

Structure of the expanding atmosphere of P Cygni

With the aid of the spectra taken in the years 1959–1968, a physical analysis of the atmosphere of P Cygni has been carried out and the motions of the atmosphere have been studied. The variations of radial velocities, the velocity progressions of Balmer and Hei lines, the high rate of mass loss (2×10^–5 M yr^–1), the features of the observed line profiles, especially that of H-K lines of Caii andD ₁-D ₂ lines of Nai confirm the conclusion of Van Blerkom (1978), concerning the assumption of an accelerating atmosphere for P Cygni. The electron density variation with the radius seems to ben _e r ^–5/2, with an average value of 7×10¹¹cm^–3 at the lower boundary of the atmosphere.In order to explain the two absorption components of observed lines, an atmospheric model based on the assumption of three envelopes, two of which accelerate gradually with two different velocity laws (up to 11.2r _c ), and the third of which accelerates rapidly with a standard velocity law (beyond 11.2r _c ) has been developed. From this model and the observed profiles, the geometrical thicknesses of the line-forming regions of H, H, H, and H are derived.The observations were obtained at Haute Provence Observatory (CNRS).