A simple method to determine breaker height and depth for different deepwater wave height/length ratios and sea floor slopes     

J.P. Le Roux 《Coastal Engineering》2007

Existing, easily applicable methods to calculate the depth and height of breaking waves are hampered by two obstacles. First, the breaker depth is usually required to compute its height, and vice versa. Second, the equations take into account either the deepwater height to wavelength ratio or the sea floor slope, but not both. A simple iterative procedure is therefore proposed which incorporates both elements. For fully developed waves breaking over a nearly horizontal bottom, the breaker height and depth are also direct functions of the deepwater wavelength.  相似文献   

Effect of fluid column dynamics on longitudinal vibrations of an ultra deepwater riser covered by an orifice plug     

Vadim S. Tikhonov  Alexander I. Safronov 《Ocean Engineering》2002,29(1):99-112

The paper studies longitudinal vibrations of an ultra-deepwater drilling riser whose bottom end is disconnected from the sea floor and covered by a plug (a blind one or the one with a hole). An elastic shell is used as a model of a riser pipe. The fluid column motion in the riser is described by the Navier–Stokes equation for a compressible fluid. Losses of fluid pressure during its flowing through a hole in the plug are taken into account. Solution of the riser equations is carried out in the frequency domain. Analysis of the effect which the riser length, wave period and height, and the plug-hole diameter on the amplitude of the riser's tension vibrations is conducted. A riser manufactured of strong aluminium alloys, some of prospective materials for ultra deepwater drilling, was considered as a prototype. It has been shown that risers 2000–4000 m long, plug-hole, and a riser 6000 m long with plug-hole of 0.087 m in diameter can withstand wave height of >15 m throughout the frequency range.  相似文献   

Diagnostics of supernova remnant shock waves     

J. C. Raymond 《Astrophysics and Space Science》1995,233(1-2):231-237

Fairly simple models can explain the emission from non-radiative shock waves in supernova remnants. This talk reviews some of the more robust diagnostics of shock parameters and some of the implications for the physics of collisionless shock waves in interstellar gas. The Hopkins Ultraviolet Telescope observed several non-radiative shocks during the ASTRO-2 mission, and the spectra have interesting implications for the physics of collisionless shocks.  相似文献   

The observational study of Herbig-Haro shock waves     

Karl-Heinz Böhm 《Astrophysics and Space Science》1995,233(1-2):11-25

We review the basic shock properties and the origin and the geometry of Herbig-Haro (H-H) shock waves. We first discuss different aspects of “normal” H-H objects which are connected with working surfaces (including internal working surfaces) of jets from young stellar objects. The emphasis is on unsolved problems of the H-H shock waves and not on the problems of the jet. We study the line flux ratios of high excitation H-H objects (high velocity shocks) and low excitation HH objects (low velocity shocks) and carry out a comparison with theoretical predictions in both cases. We emphasize an unexplained deficit of higher ions (especially OIII and SIII, but also various other ions) in high excitation objects. This lets the line flux ratios of HH objects appear as if their shock velocities are almost never above 100 km s^?1, while other shock diagnostics (position-velocity diagrams, integrated line profiles, distributions of fluxes along the axis of the bow shock, etc.) definitely indicate higher shock velocities. Some aspects of the spectrum interpretation of the very low velocity shocks (like HH7) are explained quite well by the theory. A basic unsolved problem is, however, the explanation of the CI lines whose flux is up to a factor 10 times stronger than predicted for any model. Obviously we are very far from correctly predicting the ionization of C in shock models. In the last chapter we discuss, as one example of a very unusual HH-object, HH255 (Burnham's nebula). Detailed line fluxes in the immediate environment of T Tauri (the source of HH255) have shown that HH255 has a shock wave spectrum and is definitely an HH object. In the very narrow region between 3″ and 4″ S of T Tauri we find a sharp peak of the velocity dispersion, the centroid velocity, and N_e. In the same region there is an almost discontinous increase in ionization. Between 4″ and 10″ S (corresponding to 600-1600 a.u.) of T Tauri (the source of HH255) the ionization remains high but the centroid velocity is zero (with respect to T Tauri) and the velocity dispersion is very small. This result is completely surprising for a shock wave which according to the flux ratios must have ～90 km s^?1-1 shock velocity. Why should a cooling region of a shock have a centroid velocity of ～0 km s^?1 over a large range of distance from the stellar source? At present the geometry of the HH255 is enigmatic.  相似文献   

Identification of low frequency waves in the vicinity of the terrestrial bow shock     

M.A. BalikhinO.A. Pokhotelov  S.N. Walker  M. Andre 《Planetary and Space Science》2003,51(11):693-702

In this paper, methods for the determination of the wave mode for low frequency waves based on observed differences in phase are reviewed. Examples, using measurements made in the terrestrial foreshock and magnetosheath, are used to illustrate the application of these methods. The use of advance methods such as NARMAX modelling or genetic algorithms to identify the plasma wave mode is also discussed.  相似文献   

Photoionising shocks in SNRs and AGN     

Michael A. Dopita 《Astrophysics and Space Science》1995,233(1-2):215-230

A high velocity radiative shock, or one moving into high-metallicity gas, provides an efficient means to generate a strong local UV photon field. The optical emission from the shock and precursor region is dominated by the photoionised gas, rather than by the cooling region, and the total optical + UV emission scales as the mechanical energy flux through the shock. In this paper, such models are applied to oxygen-rich supernova remnants and AGN. For AGN, the degree of magnetic support in the post-shock gas is an important parameter. LINER and cooling flow spectra can be understood as resulting from high velocity shocks without precursors, while Seyfert 1.5–2 galaxy emission line ratios result from high velocity shocks with their photoionised precursor HII regions. This model explains the problem of the high electron temperatures observed in both classes of object.  相似文献   

The deflection of jets by clouds     

Steve Higgins  Tim O'Brien  James Dunlop 《Astrophysics and Space Science》1995,233(1-2):311-315

The role of collisions between extragalactic jets and dense clouds in determining the appearance of high-redshift radio galaxies is discussed and investigated through numerical hydrodynamic simulations in three dimensions. The code has the facility to track jet material separately from ambient material. This allows us to use simplifying assumptions to calculate synthetic radio images. The results indicate that the most powerful radio sources are likely to be observed during or shortly after an interaction, and that such interactions can explain both the radio structures and the spatial association between optical and radio light found in powerful radio galaxies. In some cases such a scenario may provide an alternative explanation of jet properties to mechanisms based on variations in the source or fluid-dynamical instabilities.This author is supported by a PPARC research studentship  相似文献   

台湾岛邻近海域台风浪模拟分析   总被引：10，自引：0，他引：10       下载免费PDF全文

陈希  闵锦忠  李妍  沙文钰 《气象科学》2003,23(1):46-54

本文概略介绍了目前国际上较为先进的第三代近岸海浪数值模式SWAN（SimulationWavesNearshore）及风生浪、底摩擦、白帽耗散、深度诱导波破碎、非线性波－波相互作用等物理过程；在此基础上，以较高的分辨率对袭击台湾岛邻近海域的9015、8616号台风浪过程进行了模拟分析；台风浪高模拟值与实际台风浪资料相符较好，可以为该海域台风浪的模拟提供较好的参考。  相似文献   

Modélisation du courant sagittal induit par les vagues au-dessus des systèmes barre/baïne de la côte aquitaine (France)     

Bruno Castelle  Philippe Bonneton 《Comptes Rendus Geoscience》2006,338(10):711-717

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Effects of waves on the initiation of headland-associated sandbanks     

Nicolas Guillou  Georges Chapalain 《Continental Shelf Research》2011,31(11):1202-1213

Linear sandbanks appear in the lee of coastal headlands where the hydrodynamics are dominated by strong tidal currents and the seabed is characterized by an abundance of sands. They may develop as symmetrical sandbanks on either sides of the headland or as an unique banner bank. The present study numerically investigates the combined effects of waves and tide on the initial development of headland-associated sandbanks. A morphological model based on the coupling of the wave propagation module SWAN (Simulating WAves Nearshore) with the three-dimensional circulation module COHERENS (COupled Hydrodynamical-Ecological model for REgioNal and Shelf seas) is applied to an idealized Gaussian shaped headland for waves conditions varying in heights and directions at the offshore boundary. The coupling considers the effects of the interactions between the wave and current bottom boundary layers, namely the enhanced levels of turbulence near the bottom and the increase of the total bottom shear stress. Waves substantially modify the initial development of sandbanks formed by suspension narrowing their width and reorienting them along the side of the headland. They weakly impact the morphogenesis of sandbanks by bedload favoring on a short-time scale the growth of symmetric circular-shaped features and a central depositional spit prolonging the headland tip. Waves of transverse directions toward the tip of the headland contribute to the initiation by suspension of a well-developed feature in the headland side of low energy limiting the seabed evolution in the exposed area.  相似文献