学术
太阳表面磁场的分布与演化研究进展
宋文彬[1,2] 冯学尚[1] 汪景琇[2]
[1]中国科学院空间科学与应用研究中心空间天气学国家重点实验室,北京100080 [2]中国科学院国家天文台,北京100012
摘 要:
太阳磁场、较差自转和内部对流使得日面磁场与磁活动在很大的时间尺度和空间尺度范围均表现得相当复杂。其中最有名的是太阳活动的11年周期，或22年磁周期。在较小时间尺度上，从几秒到几小时，有时太阳大气中会发生一些壮观的爆发事件，如耀斑、日珥爆发、日冕物质抛射等。所有这些形式的事件都与太阳磁场紧密关联。简单评述了太阳磁场起源与观测方法，重点论述了不同尺度太阳磁场的空间分布与演化，介绍了从太阳磁活动现象统计得到的有关太阳磁场的几个典型特征，同时讨论了进一步研究的方向。[著者文摘]
文章出处:
《天文学进展》-2007年25卷4期 -296-304页
栏目信息:
分 类 号:
文献标识码:
A
文章编号:
1000-8349（2007）04-0296-09
Progress in the Studies on Distribution and Evolution of Solar Surface Magnetic Fields
SONG Wen-bin, FENG Xue-shang , WANG Jing-xiu （1. State Key Laboratory of Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100080, China; 2. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China）
Abstract:
The Sun＇s magnetic fields, differential rotation and plasma convection give rise to complexity in the magnetic structure and activity over a large range in both spatial and temporal scales. The most notable among these is the solar activity cycle of 11 years, or magnetic cycle of 22 years. On small time scales of a few seconds to several hours, spectacular explosive events occur in the solar atmosphere, such as solar flares, prominence eruptions and coronal mass ejections. These forms of activity are all closely related to solar magnetic fields （SMF）. This paper focuses on the introduction of SMFs＇ origin, the related observational technique, SMFs＇ distribution and evolution, and several associated typical characteristics, such as the complexities, active longitudes and active holes, the periodicities, and so on. The detailed content is organized as follows. In section 1, four typical forms of solar magnetic activity （sunspot, flare, filament, and coronal mass ejection） and their corresponding theoretical models are described briefly. Section 2 is devoted to solar dynamos responsible for explaining where SMF comes from and the course of instrument development built for observing it at higher and higher temporal and spatial resolutions. Section 3 summarizes the laws of SMFs＇ distribution and evolution on different spatial scales, including magnetic fields associated to active regions, quiet sun, and network, intra-network magnetic fields, obtained by using magnetograms and solar activity catalogues. Finally, some associated unresolved problems and highlights are discussed in the last section.[著者文摘]
Key words:
astrophysics; solar physics; solar surface magnetic fields; solar dynamo
基金资助:
国家自然科学基金资助项目（40336053、40374056、40536029、40604019）
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