A new efficient 3D non-hydrostatic free-surface flow model for simulating water wave motions

A new three-dimensional, non-hydrostatic free surface flow model is presented. For simulating water wave motions over uneven bottoms, the model employs an explicit project method on a Cartesian the staggered gird system to solve the complete three-dimensional Navier–Stokes equations. A bi-conjugated gradient method with a pre-conditioning procedure is used to solve the resulting matrix system. The model is capable of resolving non-hydrostatic pressure by incorporating the integral method of the top-layer pressure treatment, and predicting wave propagation and interaction over irregular bottom by including a partial bottom-cell treatment. Four examples of surface wave propagation are used to demonstrate the capability of the model. Using a small of vertical layers (e.g. 2–3 layers), it is shown that the model could effectively and accurately resolve wave shoaling, non-linearity, dispersion, fission, refraction, and diffraction phenomena.     

西湖凹陷西斜坡平湖组储层特征及致密化过程分析

综合应用铸体薄片、扫描电镜、阴极发光、恒速压汞、流体包裹体和X衍射等分析技术,对储层岩石学、孔喉结构和成岩作用类型及特征进行深入研究,探讨储层致密化过程和物性演化。结果表明：平湖组储层砂岩类型主要为长石岩屑质石英砂岩,以细—中粒结构为主,分选性中到好;孔隙类型以溶蚀粒间孔为主,孔隙半径主要集中于130～190 μm,喉道半径主要集中于0.2～10 μm;埋藏压实是导致平湖组储层低渗-特低渗的主因,埋深、粒度及泥质决定了压实作用的强弱,而后期次生溶蚀及胶结作用的差异加剧了储层的非均值性。中成岩A期平湖组储层次生溶蚀规模受限于流体环境,细粒沉积不利于后期溶蚀是造成储层致密化的主因;进入中成岩B期,成岩环境呈碱性且逐渐封闭,大量含铁碳酸盐、呈丝状或弯曲片状伊利石等富集堵塞喉道,致使储层大规模致密。     

The effects of immobilization on physiology and ultrastructure of unicellular alga Platymonas subcordiformis

ＴｈｅｅｆｆｅｃｔｓｏｆｉｍｍｏｂｉｌｉｚａｔｉｏｎｏｎｐｈｙｓｉｏｌｏｇｙａｎｄｕｌｔｒａｓｔｒｕｃｔｕｒｅｏｆｕｎｉｃｅｌｌｕｌａｒａｌｇａＰｌａｔｙｍｏｎａｓｓｕｂｃｏｒｄｉｆｏｒｍｉｓ￥ＺｈａｎｇＸｕｅｃｈｅｎｇ；ＷｕＸｉａｏｎａｎａｎｄＬｉ...     

胶州湾底栖生物动态的研究

胶州湾底栖生物组成复杂,数量丰富,其中有些种为捕捞对象,如菲律宾蛤仔等开发潜力很大,有些种为鱼、虾类天然饵料,如多毛类的长吻沙蚕、索沙蚕,软体动物的金星碟铰蛤等。底栖生物对渔业资源的补充和开发利用以及增、养殖和海洋生态学的研究都具有重要意义。早在30年代,张玺教授等(1936)就对胶州湾的底栖生物进行了系统的研究。解放后,中国科学院海洋研究所在胶州湾进行了大量的调査研究(E.Φ.古丽娅诺娃、吴宝铃,1963),特别是刘瑞玉教授领导的底栖生物组在1980-1990年对胶州湾进行了长期的、连续的调査,积累了许多宝贵的资料,发表了很多文章(刘瑞玉等,1992a;刘瑞玉等,1992b;孙滨等,1992;孙道元,1990;吴耀泉等,1992),基本掌握了胶州湾底栖生物的全貌。作者自1991年5月至1994年2月在原来调查的基础上,在胶州湾6个不同底栖生物群落的分布区范围内设立了10个底栖生物监测取样站(图5),进行了3年调査。每年分春(5月)、夏(8月)、秋(11月)、冬(2月)四季在各站以取样面积为0.1㎡的表层采泥器取样2次,对胶州湾底梄生物的种类组成、数量变化及群落结构进行了研究。     

On the intrinsic shape of the gamma-ray spectrum for Fermi blazars

The curvature of the γ-ray spectrum in blazars may reflect the intrinsic distribution of emitting electrons, which will further give some information on the possible acceleration and cooling processes in the emitting region. The γ-ray spectra of Fermi blazars are normally fitted either by a single power-law(PL) or a log-normal(call Logarithmic Parabola, LP) form. The possible reason for this difference is not clear. We statistically explore this issue based on the different observational properties of 1419 Fermi blazars in the 3 LAC Clean Sample. We find that the γ-ray flux(100 Me V–100 Ge V) and variability index follow bimodal distributions for PL and LP blazars, where the γ-ray flux and variability index show a positive correlation. However, the distributions of γ-ray luminosity and redshift follow a unimodal distribution. Our results suggest that the bimodal distribution of γ-ray fluxes for LP and PL blazars may not be intrinsic and all blazars may have an intrinsically curved γ-ray spectrum, and the PL spectrum is just caused by the fitting effect due to less photons.     

银河系中球状星团的空间运动

球状星团是银河系中最古老的天体类型之一,其累积光度很大,是银晕中重要的示踪天体。已以发现的银河系球状星团有１４０多个,其中１２０个银心距Ｒ〈４０Ｋｐｃ的星团已被准确地测定了视向速度。根据结数据以及球状星团金属度的统计分析,可以把球状星团次系再进一步分成某些不同的族群。目前已经测定过绝对自行的球状星团只有３８个,尽管这些自行的精度比视向速度和距离的精度差很多,然而,由此可以得出三维的空间速度,在统计     

An Emulation Research on the Radio Occultation Exploration of Martian Ionosphere

The technical system of the Sino-Russian joint satellite-to-satellite Mars ionosphere occultation is analyzed and introduced. The analogue computation of the observed values of the radio waves of the ionosphere occultation event is carried out by adopting the three-dimensional ray tracking method and the electron density profile inversion is conducted by means of the simulated occultation observational data, with the result showing that the emulation algorithm is reliable. By taking advantage of the emulation method the case computation and analysis of the inversion errors caused by the observational error of the occultation radio wave phase and the satellite orbital error are respectively carried out, and it is obtained from the result that the effect of the phase measuring error of the 5% circle on the result of the daytime ionosphere occultation exploration may be neglected, while the absolute error of the night electron density measurement is less than 4 × 108 m^?3, and the main effect of the satellite orbital error on the occultation leads to the lifting or falling of the ionospheric height. The result shows that the technical system of the Sino-Russian joint Mars ionosphere occultation exploration is advanced. It can be expected that the high accuracy electron density profile is obtained and the technical system can be applied to the exploration of the lunar ionospheric environment.     

A new interpretation of zero Lyapunov exponents in BKL time for Mixmaster cosmology

A global relation ship between cosmological time and Belinskii-Khalatnikov-Lifshitz(BKL)time during the entire evolution of the Mixmaster Bianchi Ⅸ universe is used to explain why all the Lyapunov exponents are zero at the BKL time.The actual reason is that the domain of the cosmological time is finite as the BKL time runs from minus infinity to infinity.     

Star forming activities in W75N and DR21 – Are the two regions in collision?

We have observed the massive star formation region W75N in ¹²CO J = 3 ? 2 with KOSMA. The profile of ¹²CO J = 3 ? 2 indicated that besides the 9 km s^?1 component, there is another component of ?3 km s^?1, which is associated with another star formation region, DR21N, located to the north of DR21. We derived the physical and dynamical parameters of the core and high velocity gas associated with the two components separately. Star forming activities were investigated, including outflows and infall analysis. The two regions overlap in space and are not connected in velocity. We found that the cloud–cloud collision scenario may not apply for the DR21/W75N case.     

大气模式动态测定的研究

利用12万组大气阻力资料，对DTM－1994模式进行改造，获得了一个新的大气模式，该模式的特点是：1．利用2阶周日峰效应，代替了原来模式中的复杂的周日效应表达式，减少了模式参数（少于50个），并使模式参数均具有明确的物理意义，2．分清了模式的主要参数和次要参数，在主要参数中，又分清了利用了阻力资料可以改进的参数和可能改不好的参数．3．与MSIS－1990和DTM－1994模式相比，其互差可以被接受，说明使用卫星阻力资料可以进行大气模式动态改正，不仅能测定大气总密度，并且能测定大气的分密度，4．与卫星轨道相比较，改进有显优于MSIS－1990模式，在120km轨道附近，改进模式密度比MSIS－1990模式大10％，同时我们在卫星陨落期预报中发现，MSIS－1990模式密度比实际大气密度小9％，这说明改进模式的密度与实际大气的密度基本接近。