尖峰爆发标度律及其对新一代太阳射电望远镜参数的约束  

Scaling-laws of Radio Spike Bursts and Their Constraints on New Solar Radio Telescopes

作　　者：谭宝林[1,2] 程俊 谭程明 寇洪祥[3] TAN Bao-lin;CHENG Jun;TAN Cheng-ming;KOU Hong-xiang(Key Laboratory of Solar Activity,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101;School of Astronomy and Space Sciences,University of Chinese Academy of Sciences,Beijing 100049;Shandong Zhengyuan Construction Engineering Co.Lit.,Jinan 250100)

机构地区：[1]中国科学院国家天文台太阳活动重点实验室,北京100101 [2]中国科学院大学天文与空间科学学院,北京100049 [3]山东正元建设工程有限责任公司,济南250100

出　　处：《天文学报》2018年第4期93-105,共13页Acta Astronomica Sinica

基　　金：国家自然科学基金项目(11433006;11373039;11573039;11661161015;11790301;11790305)资助

摘　　要：射电观测是太阳物理和日地空间科学的重要探测手段,尤其是对于太阳爆发过程中的太阳非热粒子加速、发射和传播等过程.迄今,世界各地研制建成了上百台太阳射电望远镜,包括射电流量计、射电动态频谱仪和射电日像仪等.基于技术进步和新的科学设想,人们还在不断提出新的太阳射电望远镜计划.研制新的太阳射电望远镜时,需要考虑观测频率、带宽、时间分辨率、频率分辨率、空间分辨率、偏振精度等设计参数.事实上,过度追求高参数往往会无法实现期望的科学目标.如何合理地选择太阳射电望远镜的参数呢?长期的观测研究发现太阳射电爆发常常可分成一系列从长到短不同时标的爆发过程,其中,尖峰爆发是最小时间尺度的爆发现象,同时也是太阳上目前发现的最小空间尺度上的爆发过程,可看成一种元爆发过程,可能对应于单一的磁场重联和磁能释放.根据太阳射电天文学研究,识别尖峰爆发是对新一代太阳射电望远镜的基本要求.尖峰爆发的时间尺度和空间尺度又是随频率而变化的.从分析不同频段太阳射电尖峰爆发的时间和带宽的标度律来说明如何为新一代望远镜的设计选择合理的参数指标,并提出谱-像结合观测模式,最大程度地保证望远镜科学目标的实现.这种观测模式或将成为未来太阳射电观测的主要方式,对揭示太阳爆发现象中的非热过程的物理本质具有非常重要的意义.Radio observation is one of important methods in solar physics and space sciences.Sometimes,it is almost the sole approach to observe physical processes such as the non-thermal processes,energetic particle acceleration,and propagations,etc.So far,more than 100 solar radio telescopes have been built in the world,including solar radio polarimeters,dynamic spectrometers,and radioheliographs.Some of them have been closed for their fulfillment of the primary scientific objectives,or for their malfunction and hence were replaced by other advanced instruments.At the same time,based on new scientific ideas and new technology,various kinds of new and much more complicated solar radio telescopes are being constructed by solar radio astronomers and space scientists.Such as the American E-OVSA and the solar radio observing system under the framework of Chinese Meridian Project II,etc.When we plan to develop a new solar radio telescope,it is crucial to design the most suitable technical parameters,e.g.,the observing frequency range,temporal cadence,frequency resolution,spatial resolution,polarization degree,and dynamic range.Then,how do we select a rational set of parameters?Based on the historical observations,it is obtained that a big strong solar radio burst is always composed of a series of small bursts with different time scales.Among them,radio spike bursts are the smallest one with the shortest lifetime,the narrowest bandwidth,and the smallest source regions.Solar radio spikes are related to a single magnetic energy release process,and can be regarded as an elementary burst in solar flares.It is a basic requirement for the new solar radio telescope to observe and discriminate solar radio spike bursts.This paper presents the scaling law of solar radio spikes with respect to the observing frequency.Such a scaling law provides a basic constraint on new solar radio telescopes,and helps us to select the rational telescope parameter.Besides,we propose a combined spectralimaging observation mode as the best operating mode for

关 键 词：太阳:太阳活动 太阳:日冕 太阳:射电辐射 射电望远镜 

分 类 号：P182[天文地球—天文学]