南海大气低层风场的气候特征分析     

黄志兴  刘嘉玲 《热带海洋学报》1995,(4)

分析１９８０－１９８７年欧洲中长期预报中心（ＥＣＭＷＦ）每日风场、温度场格点资料及同期南海区域测站和船舶资料，讨论南海低层风场的气候特征。南海为典型的季风活动区，冬季盛行东北季风，夏季盛行西南季风。流场的季节转换表现为季风系统的交替，相应不同的季风系统，南北温度梯度有一逆转过程，南海北部是温度梯度大且发生明显逆转的海区。１２°Ｎ以南海区气温全年变化极小，整个海区大气温度的季节变化不如流场变化快和显著。  相似文献   

AEL—1型风向,风速仪     

郑宝兴  李伟 《台湾海峡》1990,9(3):283-286

本文介绍并叙述了AEL-1型风向、风速仪的设计原理,仪器各部分的电路设计,工作过程及系统软件。该仪器适用于气象台站、工矿企业、海上浮标及科研单位等部门。  相似文献   

风浪周期分布与谱宽度的关系     

文凡  高志一 《海洋湖沼通报》2006,(3):1-5

本文通过分析实验室风浪周期分布,发现风浪周期累积概率分布曲线低于Longuet-Higgins理论结果,在小概率周期区域实验结果与理论结果的差异明显。对实验结果进一步分析发现,在谱不是很窄时,在小概率处风浪周期累积概率随谱宽度的增大而降低,这与窄谱假定下的理论结果相反,Longuet-Higgins理论结果在小概率处不便于描述周期分布随谱宽度的变化。根据实验结果提出风浪周期的Weibull分布经验公式,Weibull分布中的参数依赖于谱宽度。  相似文献   

A Study on the Spectral Form of Nearshore Water Waves     

Kuo Yiyu Chien Chungching Professor 《中国海洋工程》1993,(3)

- The spectral form of wind waves is investigated based on the ocean wave data observed at three nearshore stations of Taiwan. In this study, the generalized forms of Pierson-Moskowitz spectrum and JONSWAP spectrum are used to describe the local wave spectrum by selecting suitable spectral form parameters. It is shown that, at a specific site, the similarity of wave spectral form exists. Thus it is possible to use a representative spectral form for a given nearshore region to describe the wave spectrum at this nearshore. On the other hand, the effects of relative water depth on spectral form are examined. The feasibility of two spectral models in finite water depth is evaluated by using the same field wave data.  相似文献   

GPS测量船舶航速算法浅析     

胡飞荣 《全球定位系统》2008,33(1):46-48

简要介绍了GPS的定位原理和测速原理,并对利用GPS测试船舶航速的四种算法进行了说明。在多个船舶航速算例的基础上,进行了分析并得出结论。  相似文献   

基于高光谱Hyperion数据的线性光谱混合模型与神经网络模型的比较   总被引：1，自引：1，他引：0  

吴剑  程朋根  何挺  王静 《测绘科学》2008,33(1):137-140

混合像元问题是定量遥感中的热点问题之一,为了改进从遥感数据中提取定量信息,人们建立了各种混合光谱分解技术,其中线性光谱混合模型和神经网络模型就是两种比较成熟的方法。以陕西省横山地区的高光谱Hyperion数据为研究基础,通过最小噪声变换(MNF)、像元纯度指数(PPI)转换和RMS误差分析的迭代方法相结合提取影像中的纯净像元作为终端端元。分别运用神经网络模型和线性光谱混合模型对影像进行光谱分解,得到各个组分的分解图像。以标准植被指数(NDVI)影像为衡量标准,选取训练样本点,分别对两种模型进行回归分析,结果显示NDVI影像与线性光谱混合模型植被分解图像的判定系数(R2=0.91)要大于其与神经网络模型的判定系数(R2=0.81)。进一步分析表明在一般情况下,线性光谱混合模型具有比神经网络模型略高的分离精度,但是神经网络模型对细部信息的提取的效果要好于线性光谱混合模型,最后提出了端元均方根误差(EAR)指数,一种新的混合像元分解的思路。  相似文献   

Chebyshev逼近滤波器在位场分离中的应用   总被引：1，自引：0，他引：1  

蒋甫玉  孟令顺  张凤旭  高丽坤 《物探与化探》2008,32(3):311-315

在对经典FIR数字滤波器的设计方法进行研究的基础上,提出了一种可以用于位场分离的基于Chebyshev最佳一致逼近原理的FIR滤波器的设计方法。在理论模型实验中,采用基于Hanning窗的低通滤波器计算出的区域异常最大误差为6.266×10^-6 m/s² ,均方差为2.115×10^-6 m/s² ,最大百分比误差为22.2%,而且计算点在±9 km以外的误差均大于10.1%。而利用最佳一致逼近原理分离出的区域场和局部场与理论异常值拟合得较好,曲线基本重合。分离出的区域异常最大误差为3.101×10^-6 m/s² ,均方差为0.989×10^-6 m/s² ,最大百分比误差仅在边部的几个数据上,为7.76%,其余各点的误差均小于4.1%。实例检验中将该方法用于孙吴—嘉荫剖面布格重力异常场的分离,分离出的区域场中局部场残留少,分离彻底,效果较为理想。  相似文献   

渤海GNSS-R机载测风试验及其反演结果     

周兆明  符养 《武汉大学学报(信息科学版)》2008,33(3):241-244

对渤海GNSS-R机载试验进行了海面风场反演.结果表明,风速精度优于1 m/s,风向精度优于20°.  相似文献   

The origin of accretionary lapilli   总被引：1，自引：0，他引：1  

J. S. Gilbert  S. J. Lane 《Bulletin of Volcanology》1994,56(5):398-411

Experimental investigations in a recirculating wind tunnel of the mechanisms of formation of accretionary lapilli have demonstrated that growth is controlled by collision of liquid-coated particles, due to differences in fall velocities, and binding as a result of surface tension forces and secondary mineral growth. The liquids present on particle surfaces in eruption plumes are acid solutions stable at 100% relative humidity, from which secondary minerals, e.g. calcium sulphate and sodium chloride, precipitate prior to impact of accretionary lapilli with the ground. Concentric grain-size zones within accretionary lapilli build up due to differences in the supply of particular particle sizes during aggregate growth. Accretionary lapilli do not evolve by scavenging of particles by liquid drops followed by evaporation — a process which, in wind tunnel experiments, generates horizontally layered hemispherical aggregates. Size analysis of particles in the wind tunnel air stream and particles adhering to growing aggregates demonstrate that the aggregation coefficient is highly grain-size dependent. Theoretical simulation of accretionary lapilli growth in eruption plumes predicts maximum sizes in the range 0.7–20 mm for ash cloud thicknesses of 0.5–10 km respectively.  相似文献   

Structure and energy transfer of unstable hot star winds     

A. Feldmeier 《Astrophysics and Space Science》1994,221(1-2):393-408

Due to the instability of the radiation line force, the winds of hot, luminous stars should show a pronounced time-dependence resulting from the nonlinear growth of initially small perturbations. Following the method of Owocki, Castor & Rybicki (1988), we describe the time-dependent wind structure obtained with an independently developed code. Under the central assumption ofisothermality, our results are in very good agreement with the ones by Owocki et al. We find that the response of the wind to periodic base perturbations remains largely periodic, at least up tor 2...3R _* , with no clear evidence of stochastic behaviour.In order to test the foregoing assumption of isothermality and to compute the X-ray emission from models of structured winds, we have also incorporated theenergy equation into our simulations. We encountered the numerical problem that all radiative cooling zones collapse because of the oscillatory thermal instability (cf. Langer et al. 1981). We present a method to hinder this collapse by changing the cooling function at low temperatures. The resulting wind showsresolved cooling zones; but, for a supergiant wind relatively close to the star (r 10R _* ), the macroscopic wind structure is very similar to isothermal calculations. Most of the hot material is caused by shell-shell collisions.  相似文献