地形地表的不规则起伏对雷电电磁场传输的影响   总被引：2，自引：0，他引：2  

张其林  张源源  李东帅  樊艳峰  高金阁 《气象学报》2013,71(2):357-365

为了研究地形地表的不规则起伏(简称粗糙地表)对雷电电磁场传播的影响,首先利用二维分形方法模拟了粗糙地表,然后利用Barrick表面阻抗理论和Wait近似算法研究了粗糙地表对雷电电磁场传播的影响。结果表明,粗糙地表对地闪首次回击垂直电场的影响较小,但对继后回击存在明显的影响。随着粗糙度的增加,继后回击垂直电场峰值的衰减程度明显增加,且时域脉冲波形上升沿时间增大。如继后回击电磁场传播100 km,均方高为30 m的粗糙地表(电导率σ=0.1 S/m)引起时域电磁场波形上升沿时间额外增约1.5μs,电场峰值额外减小约12%,且其影响随着地面电导率的减小而增大。因此,在实际工作中应考虑复杂地形地表对闪电定位系统探测精度和效率的可能影响。  相似文献   

基于DDS技术的Loran—C信号源的杂散信号抑制的分析与实现     

皇甫江  华宇  李实锋 《时间频率学报》2014,(1):41-48

采用直接数字频率合成（DDS）技术设计的Loran—C信号源,具有输出杂散多且难以预测的缺点。基于对DDS基本原理的研究分析,针对DDS输出信号存在的相位舍位杂散问题,对其关键部位的相位累加模块进行优化设计,并基于FPGA技术,在QuartusII环境下完成了对Loran．C信号源的实现与仿真验证。结果表明,通过优化的设计算法能够产生失真小,稳定度好的输出波形,从而验证了该方法抑制杂散的有效性与可行性。  相似文献   

PSF-fitting techniques for crowded field 3D spectroscopy     

Martin M. Roth 《New Astronomy Reviews》2006,49(10-12):573

From a historical point of view, it was only through the advent of the CCD as a linear, high dynamic range panoramic detector that it became possible to overcome the source confusion problem for stellar photometry, e.g., in star clusters or nearby galaxies. The ability of accurately sampling the point-spread-function (PSF) in two dimensions and to use it as a template for fitting severely overlapping stellar images is of fundamental importance for crowded-field photometry, and has thus become the foundation for the determination of accurate color-magnitude diagrams of globular clusters and the study of resolved stellar populations in nearby galaxies. Analogous to CCDs, the introduction of integral field spectrographs has opened a new avenue for crowded-field 3D spectroscopy, which benefits in the same way from PSF-fitting techniques as CCD photometry does. This paper presents first experience with sampling the PSF in 3D spectroscopy, reviews the effects of atmospheric refraction, discusses background subtraction problems, and presents several science applications as obtained from observations with the PMAS instrument at Calar Alto Observatory.  相似文献   

Libration Points in Schwarzschild's Circular Restricted Three-Body Problem     

Roman Rodica  Mioc Vasile 《Astrophysics and Space Science》2006,304(1-4):101-103

The restricted three-body problem in Schwarzschild's gravitational field is analyzed. The existen- ce of the equilibrium points in the orbital plane is discussed and the corresponding positions are established. There are three collinear libration points, and, if they exist, two triangular libration points (situated in the orbital plane of the primaries). If triangular points exist, they may not form equilateral triangles; the triangles are isosceles for equal masses of the primaries, and scalene else.  相似文献   

东昆仑三维重力异常解释方法研究     

胡宁 《青海国土经略》1996,(2)

小波变换是一种广泛应用的信号处理技术,它具有良好的时—频局部化特性。本文探讨了小波变换在分解重力异常中的应用。同时,利用计算机对重力资料的三维定量解释,进行了初步试算。通过东昆仑地区实际资料处理,认为这二种方法在重力资料处理解释中,具有快速、简捷的特点。  相似文献   

NUMERICAL SIMULATION OF INTERANNUAL AND INTERDECADAL VARIABILITY OF SURFACE WIND OVER THE TROPICAL PACIFIC   总被引：2，自引：0，他引：2  

吴爱明  赵永平  白学志  胡敦欣 《中国海洋湖沼学报》2002,20(1):1-8

A global atmospheric general circulation model (L9R15 AGCMs) forced by COADS SST was integrated from 1945 to 1993. Interannual and interdecadal variability of the simulated surface wind over the tropical Pacific was analyzed and shown to agree vey well with observation. Simulation of surface wind over the central-western equatorial Pacific was more successful than that over the eastern Pacific. Zonal propagating feature of interannual variability of the tropical Pacific wind anomalies and its decadal difference were also simulated successfully. The close agreement between simulation and observation on the existence of obvious interdecadal variability of tropical Pacific surface wind attested to the high simulation capability of AGCM.  相似文献   

A model of Jupiter's magnetospheric magnetic field with variable magnetopause flaring     

E.S. Belenkaya  S.Y. Bobrovnikov  V.V. Kalegaev 《Planetary and Space Science》2005,53(9):863-872

We present a new model of the jovian magnetosphere in which the flaring of the magnetopause boundary can be varied. Magnetopause flaring is expected to vary due to changing conditions in the upstream interplanetary medium, related both to the dynamic pressure of the solar wind, and to changes in the direction of the interplanetary magnetic field. The model includes a tilted dipole field, which is screened by the magnetopause, a tail field current system, and the field of a screened equatorial current disc.  相似文献   

Modelling water infiltration in cracked paddy field soil     

Chen‐Wuing Liu  Shih‐Kai Chen  Cheng‐Shin Jang 《水文研究》2004,18(13):2503-2513

Periodic paddy field flooding is a major source of groundwater recharge. Many paddy fields thus are used as groundwater recharge ponds after harvesting the first crop of the summer. Following rice harvesting, paddy field surfaces may crack into fissures as a result of drainage and exposure to sunlight. Field observation indicates that applying precipitation to the paddy field can increase the rate of infiltration. To quantitatively evaluate the amount of infiltration in a cracked paddy field, this study sets up a simple soil crack model to simulate the field infiltration process. A three‐dimensional groundwater model FEMWATER is adopted to simulate water movement in the paddy field subjected to various crack conditions. Using the field and laboratory data of irrigation water requirements, soil physical properties, hydraulic conductivities and soil profiles obtained from Ten‐Chung, FEMWATER simulates the water movement in the dry cracked paddy. Simulation results show that if the cracks develop extensively and penetrate the ploughed soil, the infiltration rate may increase significantly. The infiltration fluxes of crack with depths of 80, 60 and 27·5 cm are 18·77, 14·50 and 8·06 times higher than that of 20 cm, respectively. The simulation results of cracks with 80 cm depth correlated closely with field observations. The results of the study elucidate the processes of unsaturated water movement in a dry cracked paddy field. Copyright © 2004 John Wiley & Sons, Ltd.  相似文献   

Experimental Radar Studies of Anisotropic Diffusion of High Altitude Meteor Trails     

W. K. Hocking 《Earth, Moon, and Planets》2004,95(1-4):671-679

At altitudes above 93 km in the atmosphere, magnetic and electric fields can affect the modes and rates of non-turbulent diffusion of ionized meteor trails. Anisotropic diffusion is expected. Most theories of anisotropic diffusion, and indeed most experimental studies, have concentrated on the effects of the magnetic field in producing this anisotropy, and different rates of expansion are expected in directions parallel to and perpendicular to the magnetic field lines. In this study, we use interferometric meteor radars to investigate the dependence of the ambipolar diffusion coefficient on viewing direction relative to the magnetic field, and show that the dependence is at best weak when daily averages are used. We then demonstrate that the reason for this effect is that the positions of maximum and minimum diffusion rates varies as a function of time of day, and that daily averaging masks the anisotropy. One possibility to account for the observations is that this strong diurnal variation is a consequence of the electric fields in the upper atmosphere, which are often tidally driven. An alternative possibility is a diurnal cycle in mean meteor entrance speeds. We lean towards the first hypothesis, but both possibilities are discussed. We demonstrate our results with data from several sites, but particularly using the Clovar radar near London, Ontario, Canada.  相似文献   

3. Solar System Formation and Early Evolution: the First 100 Million Years     

Thierry Montmerle  Jean-Charles Augereau  Marc Chaussidon  Mathieu Gounelle  Bernard Marty  Alessandro Morbidelli 《Earth, Moon, and Planets》2006,98(1-4):39-95

The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is its relation with the circumstellar disks that are ubiquitous around young low-mass stars today? Is it possible to define a “time zero” (t ₀), the epoch of the formation of the solar system? Is the solar system exceptional or common? This astronomical chapter focuses on the early stages, which determine in large part the subsequent evolution of the proto-solar system. This evolution is logarithmic, being very fast initially, then gradually slowing down. The chapter is thus divided in three parts: (1) The first million years: the stellar era. The dominant phase is the formation of the Sun in a stellar cluster, via accretion of material from a circumstellar disk, itself fed by a progressively vanishing circumstellar envelope. (2) The first 10 million years: the disk era. The dominant phase is the evolution and progressive disappearance of circumstellar disks around evolved young stars; planets will start to form at this stage. Important constraints on the solar nebula and on planet formation are drawn from the most primitive objects in the solar system, i.e., meteorites. (3) The first 100 million years: the “telluric” era. This phase is dominated by terrestrial (rocky) planet formation and differentiation, and the appearance of oceans and atmospheres.  相似文献