用瑞利面波资料反演中国大陆东部地壳上地幔横波速度的三维构造

利用中国大陆东部21个台站的43条面波大圆路径上瑞利面波记录的双台资料,计算出双台间地震面波相速度频散,采用Tarantola概率反演的方法求得相速度频散曲线的分布,并由各处相速度频散曲线反演得到地壳上地幔的三维横波波速图像,进而得到中国东部地壳上地幔的S波速度结构.结果表明:我国大陆东部地壳厚度总体上呈东薄西厚的趋势,以105°E为界向西地壳厚度逐渐加深到55 km以上,其中有一个北东向的h形地壳厚度的坡度带.豫西及晋南地区为相对薄地壳的地区.大别山地区和泰山附近地区地壳变厚,但秦岭地区地壳不变厚.上地幔低速层上界面的深度在华北地区较浅,为80-90km,在鄂尔多斯、四川东部以及黔湘地区为120-130km.扬子地块东部及华南褶皱系中、东部上地幔顶部速度偏低使低速层的速度反差不明显.滇黔褶皱系的西部在200 km以内的上地幔中未出现低速层.     

Interpolation of wave heights

Remote sensing of waves often necessitates presentation of data in the form of wave height values grouped over large time intervals. This restricts their use to long-term applications only. This paper describes how such data can be made suitable for short-term usage in the field. Weekly mean significant wave heights were derived from their monthly mean observations with the help of different alternative techniques. These include model-free neural network schemes as well as model-based statistical and numerical methods. Superiority of neural networks was noted when the estimations were compared with corresponding observations. The network was trained using three different training algorithms, viz., error back propagation, conjugate gradient and cascade correlation. The technique of cascade correlation took minimum training time and showed better coefficient of correlation between observations and network output.     

Relativistic anisotropic pair plasmas

The properties of waves able to propagate in a relativistic pair plasma are at the basis of the interpretation of several astrophysical observations. For instance, they are invoked in relation to radio emission processes in pulsar magnetospheres and to radiation mechanisms for relativistic radio jets. In such physical environments, pair plasma particles probably have relativistic, or even ultrarelativistic, temperatures. Besides, the presence of an extremely strong magnetic field in the emission region constrains the particles to one-dimensional motion: all the charged particles strictly move along magnetic field lines.
We take anisotropic effects and relativistic effects into account by choosing one-dimensional relativistic Jűttner–Synge distribution functions to characterize the distribution of electrons and/or positrons in a relativistic, anisotropic pair plasma. The dielectric tensor, from which the dispersion relation associated with plane wave perturbations of such a pair plasma is derived, involves specific coefficients that depend on the distribution function of particles. A precise determination of these coefficients, using the relativistic one-dimensional Jűttner–Synge distribution function, allows us to obtain the appropriate dispersion relation. The properties of waves able to propagate in anisotropic relativistic pair plasmas are deduced from this dispersion relation. The conditions in which a beam and a plasma, both ultrarelativistic, may interact and trigger off a two-stream instability are obtained from this same dispersion relation. Two astrophysical applications are discussed.     

Linear and non-linear theory of a parametric instability of hydrodynamic warps in Keplerian discs

We consider the stability of warping modes in Keplerian discs. We find them to be parametrically unstable using two lines of attack, one based on three-mode couplings and the other on Floquet theory. We confirm the existence of the instability and investigate its non-linear development in three dimensions, via numerical experiment. The most rapidly growing non-axisymmetric disturbances are the most nearly axisymmetric (low- m ) ones. Finally, we offer a simple, somewhat speculative model for the interaction of the parametric instability with the warp. We apply this model to the masing disc in NGC 4258 and show that, provided the warp is not forced too strongly, parametric instability can fix the amplitude of the warp.     

Non-linear amplification of a magnetic field driven by cosmic ray streaming

One-, two- and three-dimensional numerical results of the non-linear interaction between cosmic rays and a magnetic field are presented. These show that cosmic ray streaming drives large-amplitude Alfvénic waves. The cosmic ray streaming energy is very efficiently transferred to the perturbed magnetic field of the Alfvén waves, and the non-linear time-scale of the growth of the waves is found to be very rapid, of the order of the gyro-period of the cosmic ray. Thus, a magnetic field of interstellar values, assumed in models of supernova remnant blast wave acceleration, would not be appropriate in the region of the shock. The increased magnetic field reduces the cosmic ray acceleration time and so increases the maximum cosmic ray energy, which may provide a simple and elegant resolution to the highest energy Galactic cosmic ray problem, where the cosmic rays themselves provide the fields necessary for their acceleration.     

Nonlinear and 3D effects in leaky infragravity waves

In this paper, infragravity (IG) waves, forced by normally and obliquely incident wave groups, are studied using the quasi-3D (Q3D) nearshore circulation model SHORECIRC [Van Dongeren, A.R., I.A. Svendsen, 1997b. Quasi 3-D modeling of nearshore hydrodynamics. Research report CACR-97-04. Center for Applied Coastal Research, University of Delaware, Newark, 243 pp.], which includes the Q3D effects. The governing equations that form the basis of the model, as well as the numerical model and the boundary conditions, are described. The model is applied to the case of leaky IG waves. It is shown that the Q3D terms have a significant effect on the cross-shore variation of the surface elevation envelope, especially around the breakpoint and in the inner surf zone. The effect of wave groupiness on the temporal and spatial variation of all Q3D terms is shown after which their contribution to the momentum equations is analyzed. This reveals that only those Q3D coefficients, which appear in combination with the largest horizontal velocity shears make a significant contribution to the momentum equations. As a result of the calculation of the Q3D coefficients, the IG wave velocity profiles can be determined. This shows that in the surf zone, the velocity profiles exhibit a large curvature and time variation in the cross-shore direction, and a small — but essential — depth variation in the longshore direction.     

Experiments on Transformation and Run-Up of Wave Trains

—This paper details experiments undertaken in the UK Coastal Research Facility(CRF)at Hy-draulics Research(HR).Wallingford.on transformation and run-up of wave trains.The purpose of theseexperiments is to provide verification data for numerical models of wave transformation in shoaling.surfand swash zones.This is the kind of data that flume experiments are unable to provide.and is collected inthe highly controlled environment of CRF where extrinsic factors present in the field are not an issue.Theexperiments concerning wave trains are undertaken by use of existing wave generation software.and therun-up measurements are made with large experimental run-up gauges.     

Vortex Patterns and Roll Damping on Various Cross Sections of Ships

A numerical study is presented on roll damping of ships by solving Navier-Stokes equation.Two-Dimensional unsteady incompressible viscous flow around the rolling cylinders of various ship-likecross sections are numerically simulated by use of the computational scheme previously developed by theauthors.The numerical results show that the location of the vortices is very similar to the existing experi-mental result.For comparison of vortex patterns and roll damping on various ship-like cross sections,vari-ous distributions of shear stress and pressure on the rolling ship hull surface are presented in this paper.Itis found that there are two vortices around the midship-like section and there is one vortex around the foreor stern section.Based on these simulation results.the roll damping of a ship including viscous effects iscalculated.The contribution of pressure to the roll moment is larger than the contribution of frictionalshear stress.     

Quasi-harmonic faraday-rotation fluctuations of radio waves when sounding the outer solar corona

A statistical analysis of the Faraday-rotation fluctuations (FRFs) of linearly polarized radio signals from the Helios 1 and Helios 2 spacecraft shows that the FRF time power spectra can be of three types. Spectra of the first type are well fitted by a single power law in the range of fluctuation frequencies 1–10 mHz. Spectra of the second type are a superposition of a power law and two quasi-harmonic components with fluctuation frequencies of about v₁=4 mHz (fundamental frequency) and v₂=8 mHz (second harmonic). Spectra of the third type exhibit only one of the two quasi-harmonic components against the background of a power law. The spectral density of the quasi-harmonic components can be represented by a resonance curve with a fairly broad [Δυ ≈ (0.5–1.3)υ_1,2] distribution relative to the v=v_{1, 2} peak. The intensity of the quasi-harmonic FRF has a radial dependence that roughly matches the radial dependence for the background FRF, while their period at the fundamental frequency is approximately equal to the period of the wellknown 5-min oscillations observed in the lower solar atmosphere. The fluctuations with 5-min periods in FRF records can be explained by the presence in the outer corona of isolated trains of Alfvén waves generated at the base of the chromosphere-corona transition layer and by acoustic waves coming from deeper layers.     

Shock waves with large energy losses by direct radiation from the front

Highly nonadiabatic shock waves are formed at an early stage of a supernova explosion inside a stellar wind because of the large energy losses by direct radiation from the front. The properties of such waves are considered for velocities of (5?25)×10³km s^?1 and gas densities of 10^?17?10^?10 g cm^?3. A critical energy flux going to “infinity” that separates two modes is shown to exist. If the flux is lower than the critical one, then energy losses cause even an increase in the post-shock temperature. An excess of the flux over its critical value results in an abrupt cooling and in a strong compression of the gas. For the flux equal to the critical one, the post-shock gas velocity matches the isothermal speed of sound. Approximate formulas are given for estimating the degree of gas compression and the post-shock radiation-to-gas pressure ratio at energy losses equal to the critical ones and for the limiting compression.