武昌哨声的传播特征及其与地磁活动的相关

本文利用武昌(磁纬19.2°N)连续三年的哨声观测资料,研究了武昌地区哨声传播的一般特征。着重对武昌哨声的传播路径进行了分析推断,并讨论了它们与地磁活动的相关特性。发现:武昌哨声的显著特征是色散与电离层f₀F₂有明显的正相关关系;其次常出现一类色散值稳定、出现率也很高的哨声。此外,对典型事件的分析及统计分析都表明武昌哨声出现率在地磁扰动时明显增高;哨声色散在磁暴急始后不久即有一个急剧的上升,上升幅度达18%至37%。      

海南岛三亚哨声观测资料的初步分析

本文主要介绍1983年初在海南岛三亚观测哨声的部分结果.记录到大量哨声,其中包括短哨、多源哨和多路哨;约有10%的哨声下截频在0.8kc/s左右.经分析发现:(1)三亚哨声几乎全部出现在f₀F₂下降的过程中,哨声出现率的峰值在f₀f₂下降最快处,即电子浓度下降变化急剧处;(2)哨声活动和磁暴的关系与中高纬有所不同,存在明显的相反情况.      

哨声“源”的分析

根据雷雨云和闪电的宏观结构和电特性,作者在理论上仔细研究了哨声源的主要观测结果,得出了下述结论:引起哨声的闪电,仅仅是云地闪电中的一部分。      

磁暴期间甚低纬哨声的导管传播

对磁暴期间甚低纬哨声导管传播的机理进行了初步的讨论，根据暴时低纬哨声的特点，认为暴时出现的扩展哨、多跳回波是沿东向扰动电场导致的场列电离增强路径传播的。对在东向电场影响下低纬Ｆ层的数值模拟表明，东向电场导致的场列电离增强结构有利于哨声的捕获和传播。     

chirp-scaling算法中运动补偿问题研究

由于避免了插值计算,在大前视角和大范围成像时,chirp-scaling算法(CSA)的性能优于距离-多普勒算法(RDA).自聚焦算法在SAR成像处理中通常是必不可少的,但是现有的自聚焦算法几乎都是与RDA相结合的.本文提出了能够将自聚焦算法与CSA相结合的方法,使得CSA更具有实用性.本文同时也提出了将基于运动传感器的运动补偿和基于雷达数据的自聚焦算法与CSA结合的方法.该方法非常适合于高分辨率机载SAR成像处理.      

哨声显示电路

哨声接收机的终端一般都采用监听的方法,没有终端显示装置。最近我们设计了一种能连续显示哨声的电路,电路结构简单,配接低频示波器就可以用来作为哨声接收机的终端显示,克服了人耳监听的缺点。      

南极长城站的哨声定向观测

在中国首次南极考察期间,使用我们研制的GM型接收机对哨声进行了连续的定向观测,本文介绍了仪器性能和一些初步的观测结果,并对哨声导管在本地上空的形成过程做了分析和讨论。      

相位梯度自聚焦的离散域分析与实现

通常的自聚焦方法基于低阶相位误差模型,只能估计低阶相位误差,所以不适合高分辨力机载合成孔径雷达SAR(Synthetic Aperture Radar)的要求.本文研究的相位梯度自聚焦PGA(Phase Gradient Autofocus)是非模型的相位误差估计,因此对任意阶相位误差都有非常好的自聚焦性能.本文在离散时域和频域探讨和综述了PGA的有关问题及其实现方法.最后给出了PGA算法与一种基于低阶相位误差模型的mapdrift自聚焦算法比较的实验结果.      

哨声模波通过低纬电离层传播的某些特征

本文采用IGRF(1980)模型进行了哨声模三维射线跟踪计算, 研究了夜间哨声通过低纬电离层传播的射线与波法的特征.着重讨论了形成非导管哨声可透射路径的条件、射线的聚焦效应及射线的低纬截止.数值计算得到路径终纬度截止约在倾角纬度10.7°N.      

哨声模合声波与地球同步轨道高能电子通量增强事件事例研究

局部加速机制是磁暴期间地球外辐射带高能电子通量增强事件发生的重要原 因. 此加速机制需要两个基本条件, 一是存在种子电子, 二是存在能与种子 电子产生共振的加速波动, 包括哨声模合声波. 通过对2004-2006年 Pi1地磁脉动持续时间与种子电子通量的相关性分析, 更明确提出Pi1地磁脉 动的持续时间可以作为种子电子通量的指示剂. 通过对三个磁暴事例地球同 步轨道的种子电子通量、高能电子通量及哨声模合声波变化情况的分析, 发 现在高能电子通量较强的事例中, 均观测到较高的种子电子通量和较强的 哨声模合声波, 这在一定程度上验证了哨声模合声波对种子电子的回旋加速 机制, 且合声波强度与高能电子通量有正的相关性.      

哨声波的自聚焦(Ⅱ)——当磁层对波有放大作用时的讨论

本文指出, 当磁层对波有放大作用时, 哨声波的自聚焦容易发生;当磁层对波有吸收时, 哨声波的自聚焦不容易发生.      

磁层哨声波的丝化不稳定性

本文分析了磁层内哨声波的丝化不稳定性,并计算了增长率.结果表明,对于L(?)4和电场强度约1mV/m的哨声波最大增长率约0.13/1000km,对应最大增长率的横向波长约400km(赤道位置).并进而指出,这种丝化不稳定性有可能是多路径哨声形成的一种非线性机制.      

One-to-one relationship between low latitude whistlers and conjugate source lightning discharges and their propagation characteristics

One-to-one relation with its causative lightning discharges and propagation features of night-time whistlers recorded at low-latitude station, Allahabad (geomag. lat. 16.05°N, L = 1.08), India, from continuous observations made during 1–7 April, 2011 have been studied. The whistler observations were made using the Automatic Whistler Detector (AWD) system and AWESOME VLF receiver. The causative lightning strikes of whistlers were checked in data provided by World-Wide Lightning Location Network (WWLLN). A total of 32 whistlers were observed out of which 23 were correlated with their causative lightnings in and around the conjugate location (geom. lat. 9.87°S) of Allahabad. A multi-flash whistler is also observed on 1 April with dispersions 15.3, 17.5 and 13.6 s^1/2. About 70% (23 out of 32) whistlers were correlated with the WWLLN detected causative lightnings in the conjugate region which supports the ducted mode of propagation at low latitude. The multi-flash and short whistlers also propagated most likely in the ducted mode to this station.     

Rare observation of daytime whistlers at very low latitude (L = 1.08)

The source region and propagation mechanism of low latitude whistlers (Geomag. lat. <30°) have puzzled scientific community for last many decades. In view of recent reports, there is consensus on the source region of low latitude whistlers in the vicinity of the conjugate point. But the plausible conditions of ionospheric medium through which they travel are still uncertain. In addition to that, the whistlers in daytime are never observed at geomagnetic latitudes less than 20°. Here, for the first time, we present a rare observations of whistlers during sunlit hours from a very low-latitude station Allahabad (Geomag. Lat: 16.79°N, L = 1.08) in India on 04 February 2011. More than 90 whistlers are recorded during 1200–1300 UT during which the whole propagation path from lightning source region to whistler observation site is under sunlit. The favorable factors that facilitated the whistlers prior to the sunset are investigated in terms of source lightning characteristics, geomagnetic and background ionospheric medium conditions. The whistler activity period was found to be geomagnetically quiet. However, a significant suppression in ionospheric total electron content (TEC) compared to its quiet day average is found. This shows that background ionospheric conditions may play a key role in low latitude whistler propagation. This study reveals that whistlers can occur under sunlit hours at latitudes as low as L = 1.08 when the source lightning and ionospheric medium characteristics are optimally favorable.     

A model for stochastic acceleration of electrons during geomagnetic storms

The theory of resonant diffusion is extended to fully relativistic plasmas, and we examine resonant interactions between electrons and electromagnetic R mode (whistler) and L-mode (EMIC) waves. Resonant diffusion curves are constructed for plasma parameters representative of the Earth's storm time magnetosphere, both inside and outside the plasmapause. EMIC waves can resonate with electrons > 1 MeV, but the energies remain nearly constant along the diffusion curves. Storm-time EMIC waves can induce rapid pitch—angle scattering, but the waves are ineffective for stochastic acceleration of elections. Substantial energy change can occur along the diffusion curves for interactions between resonant electrons and whistler—mode waves, especially in regions of low plasma density. Specifically, whistlers can accelerate electrons from energies near 100 keV to above 1 MeV outside the plasmapause. A model is proposed comprising energy diffusion by whistler-mode chorus and pitch-angle scattering by EMIC waves to account for the gradual acceleration of electrons over the region 4 ≤ L ≤ 6 during the recovery phase of a geomagnetic storm.     

Simultaneous observations of some unusual whistlers and VLF hiss emission at a low L-value (L = 1.17)

The purpose of this paper is to describe some unusual whistlers (doublets and triplets) and VLF hiss emission recorded simultaneously on February 18, 1998 during nighttime at a low latitude Indian ground station Jammu (geomag. lat., 22° 26′ N; L = 1.17), and to make some discussions about their origin. The detailed structures of the observed VLF hiss emission clearly show that these emissions confined to a narrow continuous frequency band. Some times the frequency of hiss band oscillates and subsequently touches the upper edge of the first whistler component of the doublet. Detailed structures of the dynamic spectra of whistler and VLF hiss emission are briefly presented. From the dispersion analysis of the whistler doublets and triplets, it is found that the individual whistlers of the doublets and triplets simultaneously observed on the same day are one-hop whistlers having propagation path along higher and closely spaced L-values. Our result also shows that VLF hiss has been generated in the equatorial region of higher L-values. Generation and propagation mechanisms are briefly discussed.     

关于磁层中磁力线几何结构的研究

磁层磁场的几何结构是空间物理中的重要研究内容.本文采用曲率半径分析方法,结合Cluster立体探测的相关知识和背景,利用Cluster立体探测的优势,通过对Cluster 2001年的立体探测数据的研究,分析了磁层各区域的磁力线结构,包括背阳面、Cusp区以及昏侧,得出各区域中磁力线的曲率半径大小,曲率矢量以及磁力线密切面的法线矢量的方向.利用这些参量直接确定出该区域中磁力线的空间几何构型,进而揭示了该区域磁场的三维立体结构.所得结果也验证了曲率半径分析方法的正确性.在科学探测数据完备的情况下,将这一研究方法应用到磁层中其他所有区域,可以得到整个磁层的详细三维结构模型,这具有重要的科学意义.