0.5—1.5GHz快速射电频谱仪研究中的几个科学问题

本文介绍了０．５－１．５ＧＨｚ频段上的研究课题和技术方案，主要科学目标是：粒子加速过程及加速区位置的研究；小惊讶磁流力管的振荡；射电爆发精细结构和ＨＸＲ事件的相关性研究等。     

太阳硬X射线爆简单脉冲峰的理论模型

ＳＭＭ卫星上γ射线谱仪（ＧＲＳ）于１９８０年２月至１９８２年１２月间，观测到１０３个强硬Ｘ射线爆发。根据它们的时间轮廓图，发现其中的２４个事件含有变化幅度大，时间轮廓平滑的简单脉冲峰。２４个峰在５４－１００ｋｅＶ能道的统计结果显示，时间轮廓的上相斜率与下降相斜率具有较好的相关性，相关系数达０．８０，且上升相斜率略大于下降相斜率，平均值比值约为１．３７，为了定理比较，根据它们斜率的平均值构造成了一个     

空间扫描

价值１０亿美元的“太阳观测卫星”（ＳＯＨＯ）于６月２５日失控科学家已失去和ＳＯＨＯ的所有通信联系。该卫星是１９９５年１２月２日升空的，设计寿命２年。其上的仪器能以几种不同光谱及波长的光对太阳进行拍摄，还可以测量和分析由太阳产生的粒子和磁场，是人类有史...     

日本将实施4星气候监测计划

日本宇宙开发事业团（ＮＡＳＤＡ）预计将在２０００年４月开始实施一项包括４颗卫星的全球气候监视计划。ＮＡＳＤＡ目前已申请了大约１．２亿日元（合１００万美元），用于对２颗拟于２００５年发射的全球变化观测卫星（ＧＣＯＭ——ＧｌｏｂａｌＣｈａｎｇｅＯｂｓｅｒｖａｔｉｏｎＭｉｓｓｉｏｎ）进行研究。这笔研究经费尚待日本空间活动委员会的批准。第一颗卫星称为ＧＣＯＭ－Ａ１，其重点任务是大气监测。第二颗卫星是ＧＣＯＭ－Ｂ１，将携带５种遥感器，其重点任务是地球观测。它们的２颗后继星ＧＣＯＭ－Ａ２、Ｂ２，将于２０１０…     

1986年2月的高太阳活动研究—IV日地扰动事件耦合初析

利用光学、射电、软Ｘ射线和硬Ｘ射线观测资料,对１９８６年２月系列太阳爆发中最大的两个耀斑作相似与相异性的分析,解释它们近地空间效应的区别,对该系列太阳爆发事件和叠加在一起的地球事件作认证研究。     

GOES—9将使美国天气预报能力进一步加强

１９９５年５月２３日，美国在卡纳维拉尔角发射了一颗新的静止气象卫星，这是美国为进一步加强其天气预报能力的又一新举措。这颗静止气象卫星是ＮＯＡＡ新一代地球静止环境业务气象卫星（ＧＯＥＳ－ＮＥＸＴ）系列中的第二颗，卫星入轨前叫ＧＯＥＳ－Ｊ，入轨后则按习惯改称ＧＯＥＳ－９。随着它的发射，美国将拥有一个具有先进技术的双星观测系统，从而大大增强了美国气象部门在追踪和预报美国本土及附近区域灾害性天气系统的能力。ＧＯＥＳ－ＮＥＸＴ系列由５颗共耗资１０亿美元的卫星组成，其中ＧＯＥＳ－９的造价为２．２亿美元。该系…     

日环境观测技术卫星搭载用的探测器

日本环境观测技术卫星（ＡＰＥＯＳ－２），是对其地球观测平台技术卫星（ＡＤＥＯＳ）大面积观测技术的进一步发展，作为人类共同关心的地球环境问题，日本拟从弄清全球规模的水、能量循环的机理入手，通过ＡＤＥＯＳ－２卫星获得大量珍贵的地球科学数据。该卫星拟于１９９８年用Ｈ－２火箭发射。为达到上述目标，ＡＤＥＯＳ－２卫星上应该搭载能提供下列数据集的探测器，其中最为核心的探测器有高性能微波扫描辐射计（ＡＭＳＲ）和全球成像器（ＧＬＩ），此外，还搭载其它机构的探测器，如环境厅的改进型大气边缘红外分光计（ＩＬＡＳ－２…     

空间扫描

英国微型卫星ＰｏＳＡＴ－１发回高质量地球遥感图像　由地球成像系统公司收到的该卫星的１００多幅图片，显示出了气象云图和道路桥梁等细节。ＰｏＳＡＴ－１卫星是在１９９３年９月２９日搭载在阿里安火箭上发射的，卫星仅重５０公斤，制造和发射费用不到１２０万英磅。英国ＳＳＥ技术公司引进Ｋｕ波段卫星收发两用机　这种ＡＳＡＴ－１２１４／ＡＢ型收发两用机能快速选择ＫＵ波段卫星，在全Ｋｕ波段１０．９５～１２．７５ＧＨｚ频段内搜索。该收发机由３个部件组成：一个上下行转换器，一个电源，一个宽波段ＬＮＡ。美国德尔它－　（Ｄ…     

日本BS—3N广播卫星发射成功

日本ＢＳ－３Ｎ广播卫星发射成功日本广播卫星的发展一直不顺利。１９９０年２月因阿里安火箭发射失败，导致了１颗ＢＳ－２Ｘ卫星爆炸；１９９１年４月用美国阿特拉斯火箭发射时又损失了１颗ＢＳ－３Ｈ卫星。不但如此，倒霉的事还接连发生，１９９０年８月发射的ＢＳ－３...     

广播卫星接收机PCM数字伴音解码器的研制

论文详细研究了日本１２ＧＨｚ频段广播卫星（ＢＳ）电视中所采用的ＰＣＭ数字伴音,并结合目前中国收听收看日本直播卫星电视的特点,研制出了一种小型的ＰＣＭ数字伴音解码器。该解码器和Ｃ波段卫星接收机配合,可以替代进口的日本Ｋｕ波段卫星接收机,具有较大的经济效益．该解码器经卫星地球站检测中心测试表明：它解调出的Ａ、Ｂ两种模式数字伴音清晰、悦耳,其解调音质和进口的Ｋｕ频段卫星接收机的音质相当。     

同无黑子耀斑相协的微波爆发机制的探讨

1980—1984年期间,我们在云南天文台9375MHz,3653MHz和2902 HHz三个波段的射电观测资料中,查到11组微波爆发与无黑子耀斑相伴随。本文研究了这些爆发与耀斑的大气层高度,射电爆发类型以及通过落进峰值流量-时间图的位置,确认出爆发机制是活动区中作麦克斯韦分布电子的热轫致辐射。     

On the correlation of microwave bursts with the Hα flares

High correlation between microwave bursts and H_α flares has already been reported. However, Solar Maximum Year cooperation made it possible to do simultaneous observations of selected active regions with good spatial resolution. In this paper the results of the direct comparison of solar microwave recordings at the Metsähovi Radio Research Station and H_α films at the Hvar Observatory are reported. This comparison reveals that the correlation of microwave gradual rise and fall (GRF) events (time scale tens of minutes) with H_α flares is practically 100 percent. On the other hand the correlation of the impulsive microwave bursts (time scale tens of seconds) with H_α flares is low. From this it can be concluded that the main contribution to the microwave GRF bursts comes from thermal radiation.     

On the motions of RHESSI flare footpoints

The footpoint motions of flare hard X-ray (HXR) sources are directly related to the reconnection scenario of a solar flare. In this work, we tried to extract the information of footpoint motions for a number of flares observed with RHESSI. We found that the RHESSI flare results of the footpoint motions strongly support the classification proposed from the observations of YOHKOH/HXT. Furthermore, it is found that a flare can consist of two types of footpoint motions. We discussed the connections of the footpoint motions with the two-dimensional reconnection models.     

射电爆发显著事件与Ⅱ型爆发

本文分析了北京天文台2840MHz射电望远镜,1989年1月-1993年12月期间观测到的太阳射电爆发的显着事件与米波Ⅱ型、Ⅳ型爆发的对应关系,从相关结果来看,爆发的峰值流量越高△T越短,这说明当太阳流量越大,高达500s.f.u.以上时,Ⅱ型爆发会在爆发的峰值前后很短时间内发生,可能与粒子的加速有关。      

RHESSI and radio imaging observations of microflares

We present an analysis of five microflares, three observed simultaneously by RHESSI in hard X-rays and Nobeyama RadioHeliograph (NoRH) in microwaves (17 GHz) and two observed by RHESSI and Nancay RadioHeliograph (NRH) at metric wavelengths (150–450 MHz). Since we have no radio imaging telescopes simultaneously operating at microwave and meter wavelengths in the same time zone, we are obliged to use a different set of metric events in contrast to that used for comparison with the two radio wavelengths. We are interested in using the locations and other imaging characteristics of the events from both RHESSI and radio observations instead of just temporal correlation. So we have used the Nancay (France) metric radioheliograph at 150–450 MHz for this purpose. Here we describe the properties of five events – three in microwaves and two at metric wavelengths. We discuss the brightness temperatures, emission measures and the hard X-ray spectral properties of these microevents. One sees small (mini) flaring loops clearly in NoRH and RHESSI images. The microwave emission often seems to come from the RHESSI foot points (for higher energies), and from the entire small (mini) flaring loop (for lower energies).The RHESSI microflares seem to be associated in position with metric type III bursts. Frequently, the hard X-ray spectrum of the microwave associated RHESSI microflares can be fit by a thermal component at low energies (∼3–12 keV) and a nonthermal component at higher energies (∼12–20 keV).     

1986年2月的高太阳活动研究──Ⅳ日地扰动事件耦合初析

利用光学、射电、软X射线和硬X射线观测资料,对1986年2月系列太阳爆发中最大的两个耀斑作相似与相异性的分析,解释它们近地空间效应的区别,对该系列太阳爆发事件和叠加在一起的地球事件作认证研究.      

Escaping near-relativistic electron beams from the solar corona

Processes in the solar corona are prodigious accelerators of energetic ions, and electrons. The angular distribution, composition, and spectra of energetic particles observed near Earth gives information on the acceleration mechanisms. A class of energetic particle observations particularly useful in understanding the solar acceleration is the near-relativistic impulsive beam-like electron events. During five years of operation the Advanced Composition Explorer (ACE) has measured well over 400 electron events. Approximately 25% of these electron events are impulsive beam-like events that are released onto interplanetary field lines predominantly from western solar longitudes. We extend our initial 3 year study during the rise to solar maximum (Haggerty and Roelof, 2002; Simnett et al., 2002) to a five year statistical analysis of these beam-like energetic electron events in relationship to optical flares, microwave emission, soft X-ray emission, metric and decametric type-III radio bursts, and coronal mass ejections.     

Observations of solar radio bursts from meter to kilometer wavelengths

Using the Clark Lake Radioheliograph data we present direct evidence that type III electron streams propagate in dense coronal streamers. We also present imaging observations of meter-decameter microbursts, which appear to be similar to those observed in hard X-rays. At meter-decameter wavelengths, these microbursts appear to be due to plasma radiation. From observations made with ISSE-3, we discuss the characteristics of hectometer and kilometer wavelength radio bursts. In particular, we show that from studies of type III storms that the exciter electrons propagate along spiral structures, where the density is enhanced and that there is an acceleration of the solar wind. We discuss type II bursts at kilometer wavelengths, compare them with meter type II bursts and discuss their association with interplanetary shocks. We show that the interaction between type III electron streams and shocks at kilometer wavelengths can provide information on the interplanetary shock geometry. Finally, we discuss the possibility that some shock associated (SA) events may be emissions caused by electrons accelerated lower in the atmosphere rather than high in the corona in type II shocks.Recent advances in solar research have resulted from new work on plasma radiation theory, new observations of active regions and flares across the electromagnetic spectrum and the availability of spacecraft in situ measurements of solar ejecta. In this paper, we review some results obtained with the Clark Lake multifrequency radioheliograph at meter-decameter wavelengths and from satellite multifrequency directive observations at hectometer and kilometer wavelengths. We present evidence that type III electrons propagate in dense coronal streamers, and that frequently observed microbursts (presumably of type III) at meter-decameter wavelengths are due to plasma radiation. We discuss observations of hectometer and kilometer type III radio storms which reveal information about active region structures, interplanetary magnetic field configuration, and solar wind acceleration. We also discuss kilometer type II bursts, interactions between type III electrons and interplanetary shocks, and present some new results on shock associated (SA) events.     

On solar 5.7 GHz subsecond burst source sizes

Due to the narrow bandwidth and the small size of the subsecond microwave pulses, we can use them as probe sources for study of propagation effects in the low corona. More than 160 microwave bursts with subsecond pulses (SSP) have been observed with the Siberian Solar Radio Telescope at 5.7 CHz for the period 2000–2004. Working with a large dataset of homogeneous observational material (spatial resolution from 15″ to 20″, temporal resolution 14 mc), we estimated sizes of SSP and studied relation between SSP sizes and sense of the polarization and their position on the Sun. Our results are in accordance with those obtained during the 22nd solar cycle. The apparent sizes of SSP increase toward the solar limb. The obtained dependence is in agreement with Bastian‘s (Bastian, T.S. Angular scattering of solar radio emission by coronal turbulence. ApJ 426, 774, 1994.) model calculations. The center-to-limb variation of the source size is explained by scattering on plasma turbulence along the ray path in the solar corona. The most events with high polarization occur near the central meridian (±30°). The polarization sense corresponds mainly to the ordinary mode.     

Recent results on solar activity at submillimeter wavelengths

Since the installation of the Solar Submillimeter Telescope (SST) in 1999 in the Complejo Astronómico El Leoncito (CASLEO, Argentina), the almost unexplored solar emissions at frequencies >100 GHz started to reveal new insights about thermal and non-thermal processes in active regions. SST operates at the frequencies of 212 and 405 GHz providing the unique opportunity to distinguish and investigate emission mechanisms. We present a review of the most relevant findings obtained. An statistical study made with observations of a selected sample of active regions shows that their flux density spectra increase with frequency. Rapid brightenings (pulses) are always observed both at 212 and 405 GHz in association to solar flares lasting for some tens to hundreds of milliseconds. They are well correlated between the two frequencies and have flux spectra either flat or increasing with frequency. The flux of submillimeter wave pulses remain within the same order of magnitude for different bursts, ranging typically 100–300 s.f.u. at 212 GHz and 500–1000 s.f.u. at 405 GHz. The time evolution of the pulse occurrence rate usually reproduces the time profile of the X-rays/γ-rays emission, and the bulk emission at submillimeter waves, when the latter is observable. There are examples of good correlation between individual pulses at submillimeter waves and hard X-rays/γ-rays. Submillimeter pulses are not restricted to flare events, but appear to be a general phenomenon that occurs over active regions as well. The starting time of the rapid submillimeter wave pulses is coincident or precedes the projected launch time of the coronal mass ejections. SST observations of the November 4, 2003 large flare revealed a new and yet unknown spectral component with intensities increasing towards even higher frequencies, appearing along with, but separated from the well-known microwave component.