Development of solar flares and features of the fine structure of solar radio emission

The reason for the occurrence of different elements of the fine structure of solar radio bursts in the decimeter and centimeter wavelength ranges has been determined based on all available data from terrestrial and satellite observations. In some phenomena, fast pulsations, a zebra structre, fiber bursts, and spikes have been observed almost simultaneously. Two phenomena have been selected to show that the pulsations of radio emission are caused by particles accelerated in the magnetic reconnection region and that the zebra structure is excited in a source, such as a magnetic trap for fast particles. The complex combination of unusual fiber bursts, zebra structure, and spikes in the phenomenon on December 1, 2004, is associated with a single source, a magnetic island formed after a coronal mass ejection.     

Influence of Whistler Turbulence on Fast Electron Distribution and Their Microwave Emissions in a Flare Loop

The influence of whistlers on the distribution and gyrosynchrotron radiation of fast electrons injected into a coronal magnetic trap is considered. The kinetic equation in the Fokker–Planck approximation with consideration of fast electron scattering, both on background plasma particles and on whistlers, is solved for an inhomogeneous trap. It is supposed that the source of whistlers is a nonstationary process of flare energy release. Having found the fast electron distribution, we can calculate their gyrosynchrotron microwave emission. The influence of nonthermal electron scattering on whistlers are compared with the effects of scattering on Coulomb collisions. It is shown that whistlers considerably modify the emission characteristics of a loop at a certain energy density; in particular, they steepen the frequency spectrum. This is useful for microwave diagnostics of plasma turbulence in the flare loop.     

Fine structural features of radio-frequency radiation of the solar flare of February 12, 2010

Solar radio emission records received at the IZMIRAN spectrograph (25–270 MHz) during the solar flare event of February 12, 2010 are analyzed. Different fine structures were observed in three large groups of type III bursts against a low continuum. According to data from the Nancay radioheliograph, sources of all three groups of bursts were located in one active region, 11046, and their emissions were accompanied by soft X-ray bursts (GOES satellite): C7.9 at 0721 UT, B9.6 at 0940 UT, and M8.3 at 1125 UT. After the first group of bursts, classical fiber bursts were observed in combination with reverse-drift fiber bursts with unusual arc drift. After the third (the most powerful) group, stable second-length pulsations and slow-drift fiber bursts were observed, the instantaneous frequency bands of which were an order of magnitude larger than the frequency band of classical fiber bursts, and the frequency drift was several times lower. More complex fiber bursts were observed in the weakest group in the time range 0940:39–0942:00 UT. They were narrow-band (～0.5 MHz) fiber bursts, periodically recurring in a narrow frequency band (5–6 MHz) during several seconds. The presence of many chaotically drifting ensembles of fibers, crossing and superimposing on one another, is a feature of this event. It is assumed that occurrence of these structures can be connected with the existence of many small shock fronts behind the leading edge of a coronal mass ejection.     

中国北方地区冬季哨声的传播特征

本文对漠河、哈尔滨、北京三个台站1983年冬季的哨声观测资料进行了统计分析。结果表明,这三个地区的哨声活动在日落和后半夜都同时有高峰出现。在日落期间,哨声的平均色散值较高,出现有较高纬度的哨声穿出电离层后沿地球-电离层波导传播到较低纬度地区的现象;而在午夜后,哨声的平均色散值较低,有较低纬度的哨声穿出电离层后传播到较高纬度的现象。从哨声形态学特征判断,漠河和哈尔滨属于中纬度台站,而北京则属于低纬度台站的范畴。     

中国北方地区冬季哨声的传播特征

本文对漠河、哈尔滨、北京三个台站1983年冬季的哨声观测资料进行了统计分析。结果表明,这三个地区的哨声活动在日落和后半夜都同时有高峰出现。在日落期间,哨声的平均色散值较高,出现有较高纬度的哨声穿出电离层后沿地球—电离层波导传播到较低纬度地区的现象;而在午夜后,哨声的平均色散值较低,有较低纬度的哨声穿出电离层后传播到较高纬度的现象。从哨声形态学特征判断,漠河和哈尔滨属于中纬度台站,而北京则属于低纬度台站的范畴。     

Connections between whistlers and pulsation activity

Simultaneous whistler records of one station and geomagnetic pulsation (Pc3) records at three stations were compared. In a previous study correlation was found between occurrence and L value of propagation/excitation for the two phenomena. The recently investigated simultaneous records have shown that the correlation is better on longer time scales (days) than on shorter ones (minutes), but the L values of the propagation of whistlers/excitation of pulsations are correlated, i.e. if whistlers propagate in higher latitude ducts, pulsations have periods longer than in the case when whistlers propagate in lower latitude ducts.     

磁纬20°以下地区哨声多台宽带定向观测及其初步结果

武汉大学哨声组与日本名古屋大学空电研究所合作于1988年1月在我国南方进行了哨声多台宽带定向测量。利用近两年研制的宽带数字化频率追踪定向分析系统,首次获得了磁纬20°以下地区哨声波出口区与偏振状态的实验结果。初步分析发现,在湛江附近（磁纬约10°N）存在一个比较稳定的哨声路径出口区,三台同时接收到的哨声大多从这同一出口区透射出来;有时存在两个出口区,一个仍位于湛江附近,另一个位于桂林和武昌之间;沿两条不同路径传播的同源哨声具有几乎相同的色散。本文所做的非导管射线追踪计算能比较满意地解释定向实验结果。另外,此次观测中还发现一些新的有意义的现象,如记录到近百例两跳、三跳及五跳回波等,这在低纬地区是非常少见的。     

磁纬20°以下地区哨声多台宽带定向观测及其初步结果

武汉大学哨声组与日本名古屋大学空电研究所合作于1988年1月在我国南方进行了哨声多台宽带定向测量。利用近两年研制的宽带数字化频率追踪定向分析系统,首次获得了磁纬20°以下地区哨声波出口区与偏振状态的实验结果。初步分析发现,在湛江附近（磁纬约10°N）存在一个比较稳定的哨声路径出口区,三台同时接收到的哨声大多从这同一出口区透射出来;有时存在两个出口区,一个仍位于湛江附近,另一个位于桂林和武昌之间;沿两条不同路径传播的同源哨声具有几乎相同的色散。本文所做的非导管射线追踪计算能比较满意地解释定向实验结果。另外,此次观测中还发现一些新的有意义的现象,如记录到近百例两跳、三跳及五跳回波等,这在低纬地区是非常少见的。     

低纬导管哨声

本文利用在我国海南岛三亚地区（18.24°N,109.5°E;磁纬7.04°N）观测到的哨声和吱声资料,研究了低纬哨声的物理性质。观测资料和理论分析的结果表明,在低纬仍能接收到沿着按场排列的导管传播的导管哨声。结果间接地表明,在电离层中也存在哨声导管,导管哨声的临界截止纬度应当位于比磁纬7.04°N更低的地区。     

Conditions for Whistler Generation by Nonthermal Electrons in Flare Loops

Geomagnetism and Aeronomy - Constraints are imposed on whistler generation in solar-flare loops. It is shown that the effective generation of whistlers is possible only under specific conditions:...     

甚低纬多跳哨声的非导管传播

实验发现,在磁纬20°以下区域地面可重复接收到多跳哨声.本文着重考察了低纬多跳哨声非导管传播的可能性.计算结果证明,在给定的电离层状态下,该地区可以形成多跳哨声的非导管传播路径.射线追踪得到的多跳路径特征能满意地解释文中所列实验结果.因此,作为一种可能的传播机制,低纬多跳哨声的非导管传播方式值得重视.     

低纬哨声通过低电离层传播的透射特征——全波解

本文利用全波解方法研究了低纬哨声通过低电离层传播的过程。文中主要计算了哨声波的透射损失和反射系数随投射角与方位角的变化,并结合哨声多站同时观测结果进行了简要的讨论。全波解数值计算结果表明,透射损失随投射角的变化具有南北不对称性,当波矢沿磁力线方向时透射损失最小,且这种不对称性随磁倾角的减小而明显加剧。计算结果还表明,下行哨声的内反射系数基本上不随投射角而变化;但随波频率的升高而减小,并伴有数个相间的极大和极小值,这可能导致哨声回波频谱畸变。     

低纬导管哨声

本文利用在我国海南岛三亚地区（18.24°N,109.5°E;磁纬7.04°N）观测到的哨声和吱声资料,研究了低纬哨声的物理性质。观测资料和理论分析的结果表明,在低纬仍能接收到沿着按场排列的导管传播的导管哨声。结果间接地表明,在电离层中也存在哨声导管,导管哨声的临界截止纬度应当位于比磁纬7.04°N更低的地区。     

南极长城站夏季哨声的观测与分析

在中国首次南极考察期间,我们对哨声和VLF发射进行了37天的连续观测。本文首先对观测设备作了介绍,在对观测资料进行统计分析的基础上就哨声类型、发生率、色散特征等作了描述,然后重点对磁暴期间两天的哨声活动作了较细致的分析,并由此推求出其传播途径上的电子浓度变化。观测到了磁暴期间等离子体层的倒空现象和其后的回填过程。计算表明,倒空的速率为109el/cm2·s,向上的回填通量为5x108 el/cm2·s。     

甚低纬多跳哨声的非导管传播

实验发现,在磁纬20°以下区域地面可重复接收到多跳哨声.本文着重考察了低纬多跳哨声非导管传播的可能性.计算结果证明,在给定的电离层状态下,该地区可以形成多跳哨声的非导管传播路径.射线追踪得到的多跳路径特征能满意地解释文中所列实验结果.因此,作为一种可能的传播机制,低纬多跳哨声的非导管传播方式值得重视.     

张衡一号感应磁力仪数据闪电哨声波自动识别

张衡一号卫星感应式磁力仪（Search Coil Magnetometer,SCM）探测到了大量的低频电磁波动数据.本文探索从中自动识别闪电哨声波（Lightning Whistler,LW）的算法,相关结果对进一步研究空间天气闪电事件的时空变化规律具有重要研究意义.首先,以20 s的时间窗提取SCM原始波形数据,再对其做短时傅里叶变换（Short-Time Fourier Transform,STFT）得到时频图;接着,以LW在时频图中呈现明显的L形态特征为依据创建LW时频图像数据集,该数据集包括316个LW时频图,8000个非闪电哨声波的时频图;再对时频图像进行灰度化处理和尺度缩放处理以降低计算维度,同时增强闪电哨声波特征;通过设计模糊卷积核,对图像进行卷积计算以滤除大量阶跃边缘信息的影响;基于LW的形态特征设计L形态卷积核,对图像进行卷积处理以进一步增强图像中的L形态特征.最后,将增强后的L特征图输入支持向量机（Support Vector Machines,SVM）进行分类识别.大量数据处理实验结果表明：本文提出的闪电哨声波自动识别方案有效,其识别效果在精度、召回率、F1值（F1 score）和接受者操作特性曲线面积（Area Under Curve,AUC）指标上均达到94%以上.

     

南极长城站夏季哨声的观测与分析

在中国首次南极考察期间,我们对哨声和VLF发射进行了37天的连续观测。本文首先对观测设备作了介绍,在对观测资料进行统计分析的基础上就哨声类型、发生率、色散特征等作了描述,然后重点对磁暴期间两天的哨声活动作了较细致的分析,并由此推求出其传播途径上的电子浓度变化。观测到了磁暴期间等离子体层的倒空现象和其后的回填过程。计算表明,倒空的速率为10⁹el/cm²·s,向上的回填通量为5x10⁸ el/cm²·s。     

低纬哨声通过低电离层传播的透射特征——全波解

本文利用全波解方法研究了低纬哨声通过低电离层传播的过程。文中主要计算了哨声波的透射损失和反射系数随投射角与方位角的变化,并结合哨声多站同时观测结果进行了简要的讨论。全波解数值计算结果表明,透射损失随投射角的变化具有南北不对称性,当波矢沿磁力线方向时透射损失最小,且这种不对称性随磁倾角的减小而明显加剧。计算结果还表明,下行哨声的内反射系数基本上不随投射角而变化;但随波频率的升高而减小,并伴有数个相间的极大和极小值,这可能导致哨声回波频谱畸变。     

Ion whistlers in mid-latitude trough of light ions

Summary In the set of VLF data from the Interkosmos-14 satellite (launched on 11 December 1975 with apogee height of 1707 km, perigee 345 km and inclination 74°) as received in direct telemetry transmissions at the Observatory Panská Ves (Czechoslovakia), ion cyclotron whistlers were found at unusually high geomagnetic latitudes. These whistlers indicate a marked decrease of proton density in the close vicinity of the satellite with increasing geomagnetic latitude. It appeared, moreover, that proton whistlers at higher geomagnetic latitudes even sensitively reflected the rapid changes of plasma parameters within the region of the mid-latitude trough of light ions.     

Modulation of whistlers

Analysis of the experimental data obtained at Paratunka observatory (53.02° N, 158.65° E; L = 2.3) has revealed a nonstandard form of whistlers involving spectral lines that are symmetric with respect to the whistler. We have shown that this form is most likely due to the amplitude modulation of whistlers by electromagnetic pulses with a length of around 1 s and carrier frequency of around 1.1 kHz. We have suggested that these pulses could be emitted by the auroral electrojet modified by heating radiation from the HAARP facility (62.30° N, 145.30° W; L > 4.2).