开敞水域中航槽流场的数值模拟   总被引：2，自引：0，他引：2       下载免费PDF全文

陆永军  赵连白 《水科学进展》1994,5(3):208-213

建立了一个模拟开敞水域中航槽流场的平面二维数学模型.利用该模型计算得到的流速分布与袁美琦、李安中等人试验值相吻合,并计算了相当于天然情况下(各种水深、挖深比及航槽与水流的不同交角)的流场,得到了各种航槽与水流交角、不同挖深比的航槽流速折减系数变化规律图,及各种航槽与水流交角、不同挖深比的航槽中流向与航槽轴线交角的变化规律图,为开敞水域中航槽选线设计提供了依据.  相似文献   

A kinematic model for evolution of island arc-trench systems   总被引：1，自引：0，他引：1  

Toshinori Sato  Mitsuhiro Matsu'ura 《Geophysical Journal International》1993,114(3):512-530

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东昆仑山南缘大型转换挤压构造带和斜向俯冲作用   总被引：28，自引：5，他引：23  

许志琴  李海兵等 《地质学报》2001,75(2):156-164

东昆仑地体和巴颜喀拉－－松潘甘孜地体之间的会聚边界是一条位于东昆仑南缘的大型转换挤压构造带。研究表明该带的东段（阿尼玛卿段）和西段（东－西大滩段）构造特征不同,阿尼玛卿段的构造以印支期具往南西造山极性的逆冲叠覆岩片和新生代脆性左行走滑构造为特征,东－西大滩段是由220Ma形成的EW向韧性左行走滑剪切带及两则伴生的挤压褶皱断裂带组成,韧性变形持续至20Ma,之后表现为脆性左行走滑构造再活动。因此,东昆仑南缘大型会聚带是一条由东段的“收缩挤压”为主向西段的“转换挤压”逐渐过度的特殊复杂的构造带,它的形成与巴颜喀拉－－松潘甘孜地体往NE方向斜向俯冲于东昆仑地体之下有关。  相似文献   

大陆动力学演化与成矿研究: 历史与现状   总被引：21，自引：8，他引：21  

毛景文  谢桂青  李晓峰  张作衡  王义天  王志良  赵财胜  杨富全  李厚民 《矿床地质》2005,24(3):193-205

地球动力学演化过程与成矿作用是当今矿床学研究的前沿。文章回顾了自20世纪60年代以来，有关大陆动力学演化与成矿的研究历史和当前的研究动向。综述了几个研究大阶段，即：海底喷流成矿作用、大陆边缘成矿作用、板内成矿作用及地质历史演化过程的大陆汇聚或增生与多期次成矿。同时，以华南地区为例，将大陆侧向和垂向增生作为切入点，阐述了华南世界级有色、稀有、贵金属成矿省在地质历史过程中的成矿作用，并提出在该成矿省进一步实现找矿突破的重要科学问题。  相似文献   

甘肃北山造山带类型及基本特征   总被引：30，自引：5，他引：30  

龚全胜  刘明强  李海林  梁明宏  代文军 《西北地质》2002,35(3):28-34

北山造山带经历多期次、多阶段的板块裂解－俯冲－碰撞－拼合的复杂地质演化历程，具多旋回复合造山的特色。通过对造山带构造单元的建立、古板块重建、原型盆地恢复、造山带结构、构造特征及造山机制和模式的研究，确定北山造山带类型为陆－增生弧碰撞造山带。  相似文献   

中国东南沿海及邻近海区一种独特的大陆增生方式——转换断层向俯冲体系的转变     

周祖翼 《上海国土资源》1992,(1)

闽东沿海构造带—东海陆架西缘断裂、钓鱼岛隆起带(台湾—宍道褶皱带)以及帛琉—九州洋脊在中生代期间先后经历了自转换断层向俯冲系统的转变,这种转变构成了中国东南及毗邻海区独特的大陆增生方式,它表明特提斯和古太平洋的演化对这一地区的中、新生代构造格局起着重要的制约作用。  相似文献   

海平面升降变化对贵州紫云礁体生长的控制   总被引：1，自引：0，他引：1  

陆永潮  李思田  叶洪波 《地球科学》1999,24(6):585-589

以贵州紫晚二叠世碳酸盐台地边缘礁为例,运用高频层序地层学原理和方法,精细地划分了紫云礁层序的各级单元,并对其内部沉积构成进行了详细研究,探讨海平面和变化对礁体生长的控制,研究结果表明,晚二叠世紫云礁 合体为发育在台地边缘坡折带的一个三级层序,由１３个准层序组成,并可识别出低位、海侵、高位３个体系域,低位期的下切谷 边缘坡折带碳酸盐台地的暴露、海侵期和高位期礁的３种生长方式的增生及每种生长方式的特定  相似文献   

The fraction of galaxies that contain active nuclei and their accretion rates     

M.J. Page 《Monthly notices of the Royal Astronomical Society》2001,328(3):925-930

We investigate the relationship between the present-day optical luminosity function of galaxies and the X-ray luminosity function of Seyfert 1s to determine the fraction of galaxies that host Seyfert 1 nuclei and their Eddington ratios. The local type 1 active galactic nuclei (AGN) X-ray luminosity function is well reproduced if ∼1 per cent of all galaxies are type 1 Seyferts which have Eddington ratios of ∼10⁻³. However, in such a model the X-ray luminosity function is completely dominated by AGN in E and S0 galaxies, contrary to the observed mix of Seyfert host galaxies. To obtain a plausible mix of AGN host galaxy morphologies requires that the most massive black holes in E and S0 galaxies accrete with lower Eddington ratios, or have a lower incidence of Seyfert activity, than the central black holes of later-type galaxies.  相似文献   

Peculiarities of the UV continuum energy distribution for T Tauri stars     

A. S. Kravtsova  S. A. Lamzin 《Astronomy Letters》2003,29(9):612-620

In the UV spectra of BP Tau, GW Ori, T Tau, and RY Tau obtained with the Hubble Space Telescope, we detected an inflection near 2000 Å in the F _λ ^c (λ) curve that describes the continuum energy distribution. The inflection probably stems from the fact that the UV continuum in these stars consists of two components: the emission from an optically thick gas with T<8000 K and the emission from a gas with a much higher temperature. The total luminosity of the hot component is much lower than that of the cool component, but the hot-gas radiation dominates at λ<1800 Å. Previously, other authors have drawn a similar conclusion for several young stars from low-resolution IUE spectra. However, we show that the short-wavelength continuum is determined from these spectra with large errors. We also show that, for three of the stars studied (BP Tau, GW Ori, and T Tau), the accretion-shock radiation cannot account for the observed dependence F _λ ^c (λ) in the ultraviolet. We argue that more than 90% of the emission continuum in BP Tau at λ>2000 Å originates not in the accretion shock but in the inner accretion disk. Previously, a similar conclusion was reached for six more classical T Tau stars. Therefore, we believe that the high-temperature continuum can be associated with the radiation from the disk chromosphere. However, it may well be that the stellar chromosphere is its source.  相似文献   

X-ray emission from accretion disks in active galactic nuclei     

V. F. Suleimanov  K. K. Ghosh  R. A. Austin  B. D. Ramsey 《Astronomy Letters》2002,28(11):745-754

We constructed a grid of relativistic models for standard high-relative-luminosity accretion α-disks around supermassive Kerr black holes (BHs) and computed X-ray spectra for their hot, effectively optically thin inner parts by taking into account general-relativity effects. They are known to be heated to high (～10⁶–10⁹ K) temperatures and to cool down through the Comptonization of intrinsic thermal radiation. Their spectra are power laws with an exponential cutoff at high energies; i.e., they have the same shape as those observed in active galactic nuclei (AGNs). Fitting the observed X-ray spectra of AGNs with computed spectra allowed us to estimate the fundamental parameters of BHs (their mass and Kerr parameter) and accretion disks (luminosity and inclination to the line of sight) in 28 AGNs. We show that the Kerr parameter for BHs in AGNs is close to unity and that the disk inclination correlates with the Seyfert type of AGN, in accordance with the unification model of activity. The estimated BH masses M_x are compared with the masses M_rev determined by the reverberation mapping technique. For AGNs with luminosities close to the Eddington limit, these masses agree and the model under consideration may be valid for them. For low-relative-luminosity AGNs, the differences in masses increase with decreasing relative luminosity and their X-ray emission cannot be explained by this model.  相似文献