1980年中层大气温度波空间特征的初步分析

利用1980年Nimbus-7卫星网络点资料(温度场)对中层大气行星波的空间结构进行诊断和分析后发现,行星波扰动主要集中于冬半球,夏半球及赤道地区上空的扰动则相对较弱,但也不可忽视.冬半球行星波扰动中的瞬变波部分可以跨过赤道向夏半球传播,且传播主要集中于20kin和70km两个高度层附近.波数1冬季以准定常行里波为主,夏季瞬变行星波与准定常行星波波幅相当.行星波扰动的波幅从冬到夏的衰减主要表现在波数1和波数2上,波数3变化不大.      

局部涂敷RAM复杂目标的电磁散射特性计算

给出了平行和垂直极化平面波投射到物体时散射场的通用表达式,阐述了确定目标主要回波源位置的方法,提出选取吸波材料涂敷区域的有效方法,同时分析了局部涂敷吸波材料(RAM)的复杂目标电磁散射特性的计算,最后给出计算结果,并经验证.这种方法提高了复杂目标雷达散射截面计算的精度,适用于工程应用.     

Improving accuracy of damage quantification based on two-level consistency control of PZT layers

Structural health monitoring-based quantitative damage diagnosis technique plays a key role in real-time condition monitoring. Among the current research, piezoelectric (PZT) sensor and Guided Wave (GW) based damage quantification methods are promising, which normally establish a calibration model between GW feature and damage degree by experiments on batch specimens, and then conduct the calibration model on the monitored specimen. However, the accuracy of PZT and GW based damage quantification is affected by dispersion introduced by sensor network performance, structural material, and damage propagation among the adopted batch specimens. For improving the accuracy of damage quantification, this paper adopts PZT layer as sensor network and creatively implements theoretical and experimental research on batch PZT layers consistency control. On one hand, a two-level consistency control method based on multidimensional features-Euclidean distance is proposed to ensure the performance consistency of PZT layers placed on different specimens. On the other hand, experimental research on typical aircraft lug structures is also carried out to evaluate the requirement on performance consistency of PZT layers when performing quantitative damage diagnosis, and further verify the proposed two-level consistency control method. Experimental results show that the accuracy of damage quantification raises by 38% when the dispersion of different PZT layers is controlled within 5%.     

大气波动传播问题的一种无反射数值边界格式

根据无反射边界条件的基本原则,考虑到高阶的数值边界格式可以减小边界误差和虚假反射,利用曲线拟合中最小二乘法的思想,提出了一种高阶的光滑拟合外推边界格式(SFEBS).因为大气运动的控制方程简化后可以归结为一个对流方程,所以作为边界格式之间的比较和检验,在一维情况下用对流方程和数值模拟中具有代表性的波包和激波作为算例,将其与传统的基于Taylor展开思想构造的边界条件(TEBS)进行了比较.计算结果表明,在高阶情况下,用SFEBS计算波动传播问题的虚假反射约为用同阶TEBS计算的1/6,说明高阶的SFEBS可以作为一种很好的无返射数值边界格式.为今后模拟大气波动提供了一种很好的数值边界格式.      

直立墙前能谱与反射系数计算的谱分析法

 通过波谱分析方法研究了堤前能谱和反射系数的各自分布规律,分析了它们的相互关系,如不考虑反射系数的沿程变动因素,则堤前能谱的实验值与计算值将有较大差异.由于堤前能谱与入射波能谱均可测,因此,可由堤前能谱表达式得到反射系数表达式,并依据该式计算出反射系数在各点处的值.采用青岛海洋大学谱对反射系数进行计算,计算结果与已采用JONSWAP谱的反射系数结果一致.     

近壁区理论耗散率模型的改进

提出了在边界层的近壁区,采用共振三波的理论模型描述湍流边界层相干结构,由此解决了对称三维波理论模型不能处理三阶相关量的问题,根据新的理论模型对ε方程逐项进行计算和分析.与原理论模型计算结果相比,本文理论结果与直接数值模拟(DNS)符合更好.     

台风激发的声重力波的可探测性研究

通过对北京大学高频多普勒台站(39.4°N,116.2°E)多年的观测资料及相关台风资料的统计分析,着重研究了高频多普勒探测手段对由台风引起的扰动电离层响应的可探测性问题.通过对台风登陆前后的高频多普勒观测记录的细致分析及与宁静条件下记录的对比研究,表明高频多普勒观测手段可以很好地探测由台风激发的声重力波,尤其是对台风登陆前后所激发的扰动具有较高的可探测性.在所分析的24次台风事件中有明显扰动记录的高达22次(22/24).结合观测事实与Huang等的统计结果(2/12)进行了比较,并进行了可能的原因分析.通过数值模拟的方法对观测到的主要扰动的非线性传播过程进行了模拟再现,结果基本上与观测结果及线性传播理论一致.确认了一般情况下高可探测性这一事实,但同时也表明可探测性和台风激发源与探测位置及中尺度TIDs在电离层中的传播模式有密切关系.      

内重力波传播的3维传输函数模式研究

在考虑背景风场及大气耗散的条件下,建立了3维内重力波传输函数数值模式.分析了300 km高度3维传输函数在频率波数域的特性,并以近地面单位脉冲点源为激发源,得到了内重力波在3维空间中的时空分布.讨论了不同时空尺度地面方波源激发的内重力波在电离层高度的能量分布特征.结果表明,(1)对内重力波而言,背景大气相当于一个带通滤波器,只有波动周期和波长分别在15～30 min和200～400 km之间的重力波扰动最容易上传到300km高度;(2)在背景风场的作用下水平面上以同心圆扩散的波阵面以及垂直方向上成漏斗状的波阵面发生了变形,并且逆风方向比顺风方向更有利于声重力波由对流层向电离层高度传播;(3)300km高度对时间尺度和空间尺度分别在20～30 min和150～250 km之间的地面方波源响应的总能量最强.      

Seismogenic ionospheric anomalies associated with the strong Indonesian earthquake occurred on 11 April 2012 (M = 8.5)

Ionospheric perturbations in possible association with a major earthquake (EQ) (M?=?8.5) which occurred in India-Oceania region are investigated by monitoring subionospheric propagation of VLF signals transmitted from the NWC transmitter (F?=?19.8?kHz), Australia to a receiving station at Varanasi (geographic lat. 25.3°N, long 82.99°E), India. The EQ occurred on 11 April 2012 at 08:38:35?h UT (magnitude?≈?8.5, depth?=?10?km, and lat.?=?2.3°N, long.?=?93.0°E). A significant increase of few days before the EQ has been observed by using the VLF nighttime amplitude fluctuation method (fixed frequency transmitter signal). The analysis of total electron contents (TEC) derived from the global positioning system (GPS) at three different stations namely, Hyderabad (latitude 17.38°N, longitude 78.48°E), Singapore (latitude 1.37°N, longitude 103.84°E) and Port Blair (latitude 11.62°N, longitude 92.72°E) due to this EQ has also been presented. Significant perturbation in TEC data (enhancements and depletion) is noted before and after the main shock of the EQ. The possible mechanisms behind these perturbations due to EQ have also been discussed.     

Science objectives of the magnetic field experiment onboard Aditya-L1 spacecraft

The Aditya-L1 is first Indian solar mission scheduled to be placed in a halo orbit around the first Lagrangian point (L1) of Sun-Earth system in the year 2018–19. The approved scientific payloads onboard Aditya-L1 spacecraft includes a Fluxgate Digital Magnetometer (FGM) to measure the local magnetic field which is necessary to supplement the outcome of other scientific experiments onboard. The in-situ vector magnetic field data at L1 is essential for better understanding of the data provided by the particle and plasma analysis experiments, onboard Aditya-L1 mission. Also, the dynamics of Coronal Mass Ejections (CMEs) can be better understood with the help of in-situ magnetic field data at the L1 point region. This data will also serve as crucial input for the short lead-time space weather forecasting models.The proposed FGM is a dual range magnetic sensor on a 6?m long boom mounted on the Sun viewing panel deck and configured to deploy along the negative roll direction of the spacecraft. Two sets of sensors (tri-axial each) are proposed to be mounted, one at the tip of boom (6?m from the spacecraft) and other, midway (3?m from the spacecraft). The main science objective of this experiment is to measure the magnitude and nature of the interplanetary magnetic field (IMF) locally and to study the disturbed magnetic conditions and extreme solar events by detecting the CME from Sun as a transient event. The proposed secondary science objectives are to study the impact of interplanetary structures and shock solar wind interaction on geo-space environment and to detect low frequency plasma waves emanating from the solar corona at L1 point. This will provide a better understanding on how the Sun affects interplanetary space.In this paper, we shall give the main scientific objectives of the magnetic field experiment and brief technical details of the FGM onboard Aditya-1 spacecraft.