太阳射电快速精细结构的日面分布

对云南天文台“四波段太阳射电高时间分辨率同步观测系统”自１９８９年１２月－１９９４年１月期间观测到的１００个射电爆发和与其共生的２９个快速精细结构在日球和日面的经度分布做了统计,并做了初步的分析的讨论。     

一个含有丰富快速精细结构的射电大爆发

本文对１９９０年７月３０日云南天文台四波段太阳射电高时间分辨率同步观测系统＾「１，２」所观测到的太阳射电大爆发进行了分析，对在１．４２ＧＨｚ，２．００ＧＨｚ，２．８４ＧＨｚ三个波段上观测到的大量尖峰辐射作了关于寿命和强度的统计，最后，针对本次爆发中的ｍｓ－ｓｐｉｋｅｓ的特点做了一些讨论。     

1998年4月15日微波爆发观测

北京天文台１ ．０２ ．０ＧＨｚ 太阳射电频谱仪从１９９４ 年开始观测至１９９８ 年９ 月记录到太阳射电爆发１７１ 个,２ ．６３ ．８ＧＨｚ 太阳射电频谱仪１９９６ 年９ 月投入观测至１９９８ 年９ 月,记录到１４６ 个太阳射电爆发。１９９８ 年４ 月１５ 日太阳射电爆发同时在这两台频谱仪上记录到。这个事件在时间和频率上显示了丰富的幅度和结构的变化。发现了微波Ⅲ型爆发对群,并存在着丰富的快速活动现象。取得了高时间分辨率、高质量的动态谱资料,为研究耀斑各种尺度的时间及空间演化过程提供了丰富的信息。     

太阳二十二周峰年云南天文台四波段射电同步观测结果

本文主要介绍云南天文台“四波段太阳射电高时间分辨率同步观测系统”１９８９年１２月至１９９３年４月观测事件的统计结果，对１０２个射电爆发进行了初步分析，着重揭示几个类别典型事件的时间轮廓，说明射电高时间分辨率观测的意义。     

太阳二十二周峰年云南天文台四波段射电同步观测结果

本文主要介绍云南天文台“四波段太阳射电高时间分辨率同步观测系统”（１．４２，２．１３，２．８４和４．２６ＧＨｚ）１９８９年１２月至１９９３年４月观测事件的统计结果，对１０２个射电爆发进行了初步分析，着重揭示几个类别典型事件的时间轮廓，说明射电高时间分辨率观测的意义。     

2003年10月26日至11月3日CME事件的射电初步分析

基于我国的太阳射电宽带频谱仪(0．625～7．600GHz)在2003年10月22日～11月3日观测到8个伴生日冕物质抛射(CME)的太阳射电爆发,结合Nobeyama Radio Polarimeter(NORP)的单频观测、Nobeyama Radioheliograph (NORH)、Siberian Solar Radio Telescope(SSRT)的成像观测以及Culgoora和WAVE／WIND的低频射电频谱观测,对8个射电爆发的射电辐射特征进行了初步分析．试图从中寻找与CME伴生的射电爆发的特征。     

一个含有丰富快速精细结构的射电大爆发

本文对１９９０年７月３０日云南天文台四波段（１．４２ＧＨｚ、２．００ＧＨｚ、２．８４ＧＨｚ和４．００ＧＨｚ）太阳射电高时间分辨率同步观测系统［１，２］所观测到的太阳射电大爆发进行了分析，对在１．４２ＧＨｚ、２．００ＧＨｚ、２．８４ＧＨｚ三个波段上观测到的大量尖峰辐射（ｍｓ—ｓｐｉｋｅｓ）作了关于寿命和强度的统计，最后，针对本次爆发中的ｍｓ—ｓｐｉｋｅｓ的特点做了一些讨论。     

1995年10月24日昆明日食观测选题

本文介绍了１９９５年１０月２４日亚洲将要发生的日全食概况。提出了届时昆明日食的观测选题。文中对时频、射电和色球观测选题的意义和可能的观测结果作了预测性的讨论。     

1995年10月24日昆明日食观测选题

本文介绍了１９９５年１０月２４日亚洲将要发生的日全食概况，提出了届时昆明日食的观测选题，文中对时频、射电和色球观测选题的意义和可能的观测结果作了预测性的讨论。     

1997年昆明日偏食射电快速过程的观测

介绍了１９９７年３月９日昆明日食偏过程中云南天文台四波段射电高时间分辨率同步观测结果,通过掩食和露放黑子前后射电快速起伏率的变化现象,推测日冕缓变源存在电子加速过程,它可能对射电快速起伏率的增强有贡献。     

A Study of Solar Radio Bursts with Fine Structures during Flare/CME Events

We have selected 27 solar microwave burst events recorded by the Solar Broadband Radio Spectrometer (SBRS) of China, which were accompanied by M/X class flares and fast CMEs. A total of 70.4% of radio burst events peak at 2.84 GHz before the peaks of the related flares’ soft X-ray flux with an average time difference of about 6.7 minutes. Almost all of the CMEs start before or around the radio burst peaks. At 2.6?–?3.8 GHz bandwidth, 234 radio fine structures (FSs) were classified. More often, some FSs appear in groups, which can contain several individual bursts. It is found that many more radio FSs occur before the soft X-ray maxima and even before the peaks of radio bursts at 2.84 GHz. The events with high peak flux at 2.84 GHz have many more radio FSs and the durations of the radio bursts are independent of the number of radio FSs. Parameters are given for zebra patterns, type III bursts, and fiber structures, and the other types of FSs are described briefly. These radio FSs include some special types of FSs such as double type U bursts and W-type bursts.     

三厘米波段太阳射电爆发中的短时标精细结构

在1989年3月至1990年4月间,我们对太阳射电辐射进行快速采样观测.发现三厘米波段射电爆发亦具有快速精细结构,时标尺度在0.1至2秒间。     

太阳米波和分米波Ⅱ型、Ⅲ型射电暴及其精细结构观测研究进展

太阳米波和分米波的射电观测是对太阳爆发过程中耀斑和日冕物质抛射现象研究的重要观测手段。米波和分米波的太阳射电暴以相干等离子体辐射为主导,表现出在时域和频域的多样性和复杂性。其中Ⅱ型射电暴是激波在日冕中运动引起电磁波辐射的结果。在Ⅱ型射电暴方面,首先对米波Ⅱ型射电暴的激波起源问题和米波Ⅱ型射电暴与行星际Ⅱ型射电暴的关系问题进行了讨论;其次,结合Lin-Forbes太阳爆发理论模型对Ⅱ型射电暴的开始时间和起始频率进行讨论:最后,对Ⅱ型射电暴信号中包含的两种射电精细结构,Herringbone结构(即鱼骨结构)和与激波相关的Ⅲ型射电暴也分别进行了讨论。Ⅲ型射电暴是高能电子束在日冕中运动产生电磁波辐射的结果。在Ⅲ型射电暴方面,首先介绍了利用Ⅲ型射电暴对日冕磁场位形和等离子体密度进行研究的具体方法;其次,对利用Ⅲ型射电暴测量日冕温度的最新理论进行介绍;最后,对Ⅲ型射电暴和Ⅱ型射电暴的时间关系、Ⅲ型射电暴和粒子加速以及Ⅲ型射电暴信号中包含的射电精细结构(例如斑马纹、纤维爆发及尖峰辐射)等问题进行讨论并介绍有关的最新研究进展。     

High time resolution observations of solar radio emission at four frequencies: evidence for energy release in microflares

As evidence for energy release in microflares, high time resolution observations of solar radio emission obtained with our “synchronous observation system of solar radio radiation with high time resolution at four frequencies (1.42, 2.13, 2.84 and 4.26 GHz)” from December 1989 to April 1993 are presented in this paper. The observed events include weak ms spikes, “spike-likes”, fast pulsations as well as two kinds of newly discovered fast fine structures, i.e., microwave type III bursts and microwave patch-like structures. A statistical study of the duration of fast fine structures has been made and on its basis the various types of phenomena are illustrated with actual examples.     

High-Resolution Time Profiles of Fiber Bursts at 1420 and 2695 MHz

To obtain constraints for models of fiber bursts, high-resolution time (0.01 s) profiles of the fiber bursts recorded at 1420 and 2695 MHz by the Trieste radiometers are studied in detail. The fiber bursts were identified using Ond?ejov radio spectra. During the years 2000?–?2005, 18 intervals with fiber bursts were selected; 26 groups were defined and about 700 fibers were analyzed in detail. More than 300 pulsations, present almost simultaneously with the fibers, were also selected and studied in order to find similarities or differences between these two types of fine structures. It was found that the polarization of the associated continuum, both for fiber bursts and pulsations, is practically the same. Evaluating the ratio between absorption over emission of many single fibers we found that this parameter is very different even for nearby bursts; however, we realized that this ratio shows a tendency to decrease with time. Finally, the time profile of one selected fiber burst was fitted using a recent model based on the modulation of the broadband radio emission by fast magnetoacoustic waves. The results are discussed.     

Bursts with temporal fine structure at 5730 MHz

An analysis of solar radio bursts with temporal fine structure (TFS) at 5730 MHz in relation to the magnetic configuration of the corresponding active regions (AR) is presented. We found that the occurrence of TFS bursts increases with increasing complexity of the AR's magnetic configuration. The degree of polarization of TFS bursts varies over a wide range. Most of these fast bursts with a high degree of polarization were observed in active regions with a simple magnetic configuration β. Most of the unpolarized fast bursts were observed in active regions with the most complicated configuration βγδ. Because bursts that are polarized in different modes have different displacements of position with respect to that of associated microwave bursts, we conclude that there are at least two types of TFS bursts at 5730 MHz. We think that fast bursts that are polarized in the ordinary mode are due to microwave type III bursts.     

Observations of Solar Type II bursts at frequencies 10–30 MHz

We present the results of radio telescope UTR-2 observations of solar Type II radio bursts in the 10–30 MHz frequency range. These events possess a fine structure consisting of fast drift sub-bursts similar to Type III bursts. The frequency drift rate of the Type II bursts at decameter wavelengths is smaller than 0.1 MHz s^–1. One of these bursts with herringbone structure has a wave-like backbone that almost does not drift. The features of the observed bursts are discussed.     

3厘米波段太阳射电爆发中精细结构的特征

本文扼要介绍南京大学天文系3厘米波段在1989－1992年间观测射电精细结构的结果，指出该波段存在三种类型的精细结构，并简要讨论它们可能的产生机制．     

On a suggested explanation for fine structures observed in some wide-band bursts

Plasma radiation arising from non-linear coupling of upper hybrid plasma waves and Bernstein waves is examined as a possible explanation (Rosenberg, 1972) for the fine structures observed in some wide-band solar radio bursts. This radiation is found to be weakly polarized and therefore it cannot account for the fine structures, which are strongly polarized. The difficulties encountered in explaining several bands of radiation at comparable intensities are indicated.     

Fine structure of large flare radioemission

Several recent phenomena with zebra patterns (ZPs) and fiber bursts on the dynamic spectra of solar type IV radio bursts have been complexly analyzed using all available ground-based and satellite data (SOHO, TRACE, RHESSI). ZPs and fiber bursts were observed at frequencies of 50–3800 MHz. The main relative spectral parameters and the degree of circular polarization of ZPs and fiber bursts are almost identical. The fine structure was observed in powerful and weak phenomena (and was more impressive in weak phenomena) during impulsive and decline phases at instants of recurring continuum bursts. The shape of the fine structure depends on that of the magnetic loops in a radio source, the type of fast particle acceleration (impulsive or prolonged), and the presence of shock waves and coronal mass ejections. Several new effects of the interaction between zebra stripes and fiber bursts have been detected. Specifically, up to 40 fiber bursts with different frequency ranges were simultaneously observed in the frequency range 1–2 GHz against a background of sudden absorptions. It has been indicated that different effects in the ZP stripe behavior can be explained within the scope of the model with whistlers, if the quasi-linear diffusion of fast particles on whistlers (which deforms the particle velocity distribution function) is taken into account.