Additional effects of resonance in Hilda-asteroid orbits by the combined action of Jupiter and Saturn     

J. Schubart 《Icarus》2007,188(1):189-194

Inside the 3/2 mean motion resonance some Hilda-type orbits show effects of a three-body resonance that includes the frequency of the libration due to the 3/2 resonance. A graphical method presents numerical results for such orbits and demonstrates in 6 cases a process of temporary libration, that is ruled by the additional resonance together with the secular period of the eccentricities of Jupiter and Saturn.  相似文献   

GNSS海面散射信号的海面风场遥感     

王迎强  严卫  张锐 《海洋技术学报》2008,27(2):72-77

首先介绍了GNSS-R海洋遥感的发展过程,简要叙述了利用GNSS信号进行海洋动力学遥感测量的基本原理;然后分析了接收机天线的部分参数对GNSS信号可见数量的影响;最后详细阐述了GNSS海面散射信号的理论模型,该模型是利用几何光学限制的基尔霍夫近似建立起来的,并根据理论模型进行了数值仿真试验。结果证实了通过散射信号功率波形来反演海面风场理论上的可行性。  相似文献   

A comparative analysis of metiers and catch profiles for some French demersal and pelagic fleets     

Marchal  Paul 《ICES Journal of Marine Science》2008,65(4):674-686

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A real-time, event-triggered storm surge forecasting system for the state of North Carolina   总被引：3，自引：0，他引：3  

Craig Mattocks  Cristina Forbes   《Ocean Modelling》2008,25(3-4):95-119

A new real-time, event-triggered storm surge prediction system has been developed for the State of North Carolina to assist emergency managers, policy-makers and other government officials with evacuation planning, decision-making and resource deployment during tropical storm landfall and flood inundation events. The North Carolina Forecast System (NCFS) was designed and built to provide a rapid response assessment of hurricane threat, accomplished by driving a high-resolution, two-dimensional, depth-integrated version of the ADCIRC (Advanced Circulation) coastal ocean model with winds from a synthetic asymmetric gradient wind vortex. These parametric winds, calculated at exact finite-element mesh node locations and directly coupled to the ocean model at every time step, are generated from National Hurricane Center (NHC) forecast advisories the moment they are inserted into the real-time weather data stream, maximizing the number of hours of forecast utility. Tidal harmonic constituents are prescribed at the open water boundaries and applied as tidal potentials in the interior of the ocean model domain. A directional surface roughness parameterization that modulates the wind speed at a given location based on the types of land cover encountered upwind, a forest canopy sheltering effect, and a spatially varying distribution of Manning’s–n friction coefficient used for computing the bottom/channel bed friction are also included in the storm surge model. Comparisons of the simulated wind speeds and phases against their real meteorological counterparts, of model elevations against actual sea surface elevations measured by NOAA tide gauges along the NC coast, and of simulated depth-averaged current velocities against Acoustic Doppler Current Profiler (ADCP) data, indicate that this new system produces remarkably realistic predictions of winds and storm surge.  相似文献   

Stability of an immersed tunnel in offshore conditions under deep water wave impact     

T. Kasper  J.S. Steenfelt  L.M. Pedersen  P.G. Jackson  R.W.M.G. Heijmans 《Coastal Engineering》2008

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Multidimensional treatment of photon emission from accretion discs around black holes     

Kazunori Kohri  Ken Ohsuga  Ramesh Narayan 《Monthly notices of the Royal Astronomical Society》2007,381(3):1267-1274

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Structure and clumping in the fast wind of NGC 6543     

R. K. Prinja  S. E. Hodges  D. L. Massa  A. W. Fullerton  A. W. Burnley 《Monthly notices of the Royal Astronomical Society》2007,382(1):299-307

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Particle distributions and X-ray spectra in single or multiple solar current sheets     

C. Gontikakis  A. Anastasiadis  C. Efthymiopoulos 《Monthly notices of the Royal Astronomical Society》2007,378(3):1019-1030

The acceleration of charged particles in a site of magnetic reconnection is analysed by detailed numerical simulations. Single or multiple encounters of the particles with Harris-type reconnecting current sheets (RCSs) are modelled as an overall stochastic process taking place within an active region. RCS physical parameters are selected in a parameter space relevant to solar flares. Initially, the charged particles form a thermal (Maxwellian) distribution corresponding to coronal temperature  ≃2 × 10⁶ K  . Our main goal is to investigate how the acceleration process changes the shape of the particles' kinetic energy distribution. The evolution of the kinetic energy distribution, calculated numerically after one encounter of the particles with a single RCS, is found to be in good agreement with our previously published analytical formulae. In the case of consecutive encounters, we find that the kinetic distribution tends to converge to a practically invariant form after a relatively small number of encounters. We construct a discrete stochastic process that reproduces the numerical distributions and we provide a theoretical interpretation of the asymptotic convergence of the energy distribution. We finally compute the theoretical X-ray spectra that would be emitted by the simulated particles in a thick target model of radiation.  相似文献   

Progressive Transformation of a Flux Rope to an ICME     

S. Dasso  M. S. Nakwacki  P. Démoulin  C. H. Mandrini 《Solar physics》2007,244(1-2):115-137

The solar wind conditions at one astronomical unit (AU) can be strongly disturbed by interplanetary coronal mass ejections (ICMEs). A subset, called magnetic clouds (MCs), is formed by twisted flux ropes that transport an important amount of magnetic flux and helicity, which is released in CMEs. At 1 AU from the Sun, the magnetic structure of MCs is generally modeled by neglecting their expansion during the spacecraft crossing. However, in some cases, MCs present a significant expansion. We present here an analysis of the huge and significantly expanding MC observed by the Wind spacecraft during 9 – 10 November 2004. This MC was embedded in an ICME. After determining an approximate orientation for the flux rope using the minimum variance method, we obtain a precise orientation of the cloud axis by relating its front and rear magnetic discontinuities using a direct method. This method takes into account the conservation of the azimuthal magnetic flux between the inbound and outbound branches and is valid for a finite impact parameter (i.e., not necessarily a small distance between the spacecraft trajectory and the cloud axis). The MC is also studied using dynamic models with isotropic expansion. We have found (6.2±1.5)×10²⁰ Mx for the axial flux and (78±18)×10²⁰ Mx for the azimuthal flux. Moreover, using the direct method, we find that the ICME is formed by a flux rope (MC) followed by an extended coherent magnetic region. These observations are interpreted by considering the existence of a previously larger flux rope, which partially reconnected with its environment in the front. We estimate that the reconnection process started close to the Sun. These findings imply that the ejected flux rope is progressively peeled by reconnection and transformed to the observed ICME (with a remnant flux rope in the front part).  相似文献   

Ultraviolet dust attenuation in spiral galaxies: the role of age-dependent extinction and the initial mass function     

P. Panuzzo  G. L. Granato  V. Buat  A. K. Inoue  L. Silva  J. Iglesias-Páramo  A. Bressan 《Monthly notices of the Royal Astronomical Society》2007,375(2):640-648

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