Turbulence fields in the lee of two‐dimensional transverse dunes simulated in a wind tunnel     

Zhibao Dong  Guangqiang Qinan  Ping Lu  Wanyin Luo  Hongtao Wang 《地球表面变化过程与地形》2009,34(2):204-216

The turbulence field of airflow in the lee of a dune has significant impacts on dune dynamics and related processes. We used particle image velocimetry in a wind tunnel simulation to obtain detailed velocity measurements in the lee of two‐dimensional transverse dune models, then used the results to analyse their turbulence fields. The dune models used in this study had a single lee angle of 30°, and a total of six stoss angles: 3°, 5°, 10°, 15°, 20° and 25°. We used vorticity, turbulence intensity, Reynolds stress and turbulent kinetic energy to characterize the turbulence fields. These parameters were functions of stoss angle, wind velocity, distance from the dune crest and height above the ground surface. The stoss angles could generally be divided into two groups based on the profiles of mean velocity, turbulence and Reynolds stress. Stoss angles of 3° and 5° usually had similar profiles, and angles of 15°, 20° and 25° formed a second group with similar profiles. The profiles for the stoss angle of 10° were usually transitional and were intermediate between the two groups. Vorticity, Reynolds stress and turbulent kinetic energy increased monotonically with increasing free‐stream wind velocity, but their variations with respect to the stoss angle were complex. The stoss angles of 15° and 20° had the maximum values of these three parameters, thus these angles may have special significance in dune development given the characteristics of the mean velocity fields and turbulence fields they produce within the lee airflow. It is the streamwise velocity component and its turbulence that determine the surface shear stress. Copyright © 2008 John Wiley and Sons, Ltd.  相似文献   

Meridional circulation in the radiation zones of rotating stars: Origins,behaviors and consequences on stellar evolution     

S. Mathis  T. Decressin  A. Palacios  P. Eggenberger  L. Siess  S. Talon  C. Charbonnel  S. Turck-Chièze  J.-P. Zahn 《Astronomische Nachrichten》2007,328(10):1062-1065

Stellar radiation zones are the seat of meridional currents. This circulation has a strong impact on the transport of angular momentum and the mixing of chemicals that modify the evolution of stars. First, we recall in details the dynamical processes that are taking place in differentially rotating stellar radiation zones and the assumptions which are adopted for their modelling in stellar evolution. Then, we present our new results of numerical simulations which allow us to follow in 2D the secular hydrodynamics of rotating stars, assuming that anisotropic turbulence enforces a shellular rotation law and taking into account the transport of angular momentum by internal gravity waves. The different behaviors of the meridional circulation in function of the type of stars which is studied are discussed with their physical origin and their consequences on the transport of angular momentum and of chemicals. Finally, we show how this work is leading to a dynamical vision of the evolution of rotating stars from their birth to their death. (© 2007 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

The angular momentum transport in rotating turbulent convection     

G. Rüdiger  P. Egorov  U. Ziegler 《Astronomische Nachrichten》2005,326(5):315-320

The angular momentum transport in rotating turbulent convection is simulated with the NIRVANA code for Taylor numbers up to 10⁶. The box consists of an unstable layer embedded in two stable overshoot layers. We find the expected anisotropies in the rotating anisotropic turbulence field: 〈u^′2_r〉 exceeds 〈u^′2_ϕ〉, and 〈u^′2_ϕ〉 exceeds 〈u^′2_θ〉. The resulting radial angular momentum transport is directed inwards and peaks in the middle of the convective layer. The resulting latitudinal angular momentum transport is equatorwards, peaks at the surface and is highly concentrated to the equatorial region. Apart from a factor of 2–3 the total amplitudes of the cross‐correlations are of the same order of magnitude. In the lower overshoot region (‘tachocline’) the cross‐correlations are negative. It is argued that the concentration of the latitudinal angular momentum transport towards the surface and towards the equator does not too strongly reduce its potential to produce rotation laws with accelerated equators. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

The structure and fluid mechanics of turbidity currents: a review of some recent studies and their geological implications   总被引：17，自引：1，他引：16  

Ben Kneller  Clare Buckee 《Sedimentology》2000,47(S1):62-94

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Turbulence Characteristics In The Surface Boundary Layer Over The South American Pampa     

Osvaldo L. L. Moraes 《Boundary-Layer Meteorology》2000,96(3):317-335

This paper presents results of turbulence measurementsmade in the south of Brazil in the Pampa region.Data collected at 1Hz are used to calculatestandard deviations of temperature and velocities. Onthe other hand data collected at 10Hz areused to study the behaviour of spectra and cospectraof turbulence in the surface layer. Dimensionless dissipation rates of turbulent kinetic energy and temperature variance are also presented. The frameworkof Monin–Obukhov Similarity theory is used and allresults are compared with other experimentalstudies.  相似文献   

On the spectrum of mid-latitude sporadic-E irregularities     

Yu. V. Kyzyurov 《Annales Geophysicae》2000,18(10):1283-1292

We discuss the creation of mid-latitude sporadic-E plasma irregularities (with length-scales smaller than sporadic layer thickness) by the neutral atmosphere turbulence. Using fluid equations, the relation between plasma density fluctuations and the velocity field of neutrals is derived. After a brief discussion of the relevant neutral turbulence, the analytical expression for the power spectrum of plasma irregularities is obtained. This expression allows a power-law type of experimental irregularity spectra (the spectral index depends on sporadic-E characteristics) and possible departures in detail of the irregularity spectra from the power-law form to be explained. In addition, it allows us to make estimates of length-scales at which such departures must occur.  相似文献   

Study on horizontal relative diffusion in the troposphere and lower stratosphere     

Zheng Yi 《大气科学进展》2000,17(1):93-102

The behaviour of relative diffusion theory and Gifford’s random-force theory for long-range atmospheric diffusion is examined. When a puff scale is smaller than the Lagrangian length scale, 2KTL, an accelerative relative diffusion region exists, i.e., σy∝t3/2. While the puff diffusion enters a two-dimensional turbulence region, in which the diffusion scale is larger than 500 km, or time scale is larger than 1 day, divergence and convergence are main cause of horizontal diffusion. Between the two above-mentioned regimes, diffusion deviation is given byσy=2KTL. The large-scale horizontal relative diffusion parameters were obtained by analyzing the data of radioactive cloud width collected in air nuclear tests.  相似文献   

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

Charles F. Gammie  Jeremy Goodman  Gordon I. Ogilvie 《Monthly notices of the Royal Astronomical Society》2000,318(4):1005-1016

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.  相似文献   

Energetic particle acceleration in a three-dimensional magnetic field reconnection model: the role of magnetohydrodynamic turbulence     

T. Kobak  M. Ostrowski 《Monthly notices of the Royal Astronomical Society》2000,317(4):973-978

The role of magnetohydrodynamic (MHD) turbulence in the cosmic ray acceleration process in a volume with a reconnecting magnetic field is studied by means of Monte Carlo simulations. We performed modelling of proton acceleration, with the three-dimensional analytic model of stationary reconnection of Craig et al. providing the unperturbed background conditions. Perturbations of particle trajectories resulting from a turbulent magnetic field component were simulated using small-amplitude pitch-angle momentum scattering, enabling modelling of both small- and large-amplitude turbulence in a wide wavevector range. Within the approach, no second-order Fermi acceleration process is allowed. Comparison of the acceleration process in models involving particle trajectory perturbations with the unperturbed model reveals that the turbulence can substantially increase the acceleration efficiency, enabling much higher final particle energies and flat particle spectra.  相似文献   

海洋湍流观测技术   总被引：3，自引：0，他引：3  

康建军  邬海强  杨庆轩  付红丽 《海洋技术学报》2007,26(3):19-23

湍流在海洋能量和水体的交换演化中起着非常重要的作用。海洋湍流研究的发展和海洋湍流观测仪器的研发密切相关。世界上湍流观测仪器的研发起步于上世纪50年代,但是我国在湍流观测设备方面到目前为止仅仅处于起步和引进国外设备阶段。针对我国的情况,文中对海洋湍流观测的平台、探头测量原理及其数据修正、资料后处理等关键技术做一个总结性的介绍,为我国使用引进的海洋湍流设备和自主开发海洋湍流测量设备提供参考。  相似文献