Evolutionary Characteristics of the Interplanetary Magnetic Field Intensity
文献类型:期刊论文
作者 | Xiang NB(向南彬)1,2,3; Qu, Z. N.4 |
刊名 | ASTRONOMICAL JOURNAL |
出版日期 | 2018-10-01 |
卷号 | 156期号:4页码:11 |
ISSN号 | 0004-6256 |
关键词 | Sun: activity Sun: general Sun: magnetic fields |
DOI | 10.3847/1538-3881/aadb91 |
产权排序 | 第1完成单位 |
文献子类 | Article |
英文摘要 | We use several mathematical methods, such as the continuous wavelet transform, the wavelet coherence (WTC), and the partial wavelet coherence, to investigate the distribution and oscillation periods of the daily interplanetary magnetic field (IMF) intensity as well as the connection between IMF fluctuations and solar activity indices (the magnetic plage strength index and the Mount Wilson sunspot index). The daily IMF intensity generally approximately follows a log-normal distribution that is directly related to the distribution of the active region flux. The short-term periods of the IMF are about 13.7, 27.6, 37.1, and 75.3 days. They are driven by the quasiperiodicity of the magnetic surges on the solar surface. The medium-term periods of 1.07 and 1.82 years need to be derived from the stochastic interaction of local fields and meridional flows, since coronal holes reflect the transport of the magnetic flux on the solar surface and variations in the meridional flow are seen in the heliosphere. The 10.9-year period is the Schwabe solar cycle and is to be mentioned first. The solar cycle variation of the IMF is not thought to be related to weak solar magnetic activity, but is dominated by the strong solar magnetic field activity seen on the disk, because the footpoints of the time-varying component of the interplanetary magnetic flux are rooted in regions that are located near the sources of coronal mass ejections that are related to active regions, while the constant component in the IMF is thought to initially and mainly come from the weak solar magnetic field activity. Finally, the slow variation of the IMF indicates that it may have a period of longer than 50 years. |
学科主题 | 天文学 |
URL标识 | 查看原文 |
出版地 | TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND |
WOS关键词 | CORONAL MASS EJECTIONS ; LONG-TERM VARIATIONS ; SOLAR ROTATION ; MOUNT-WILSON ; GEOMAGNETIC-ACTIVITY ; TEMPORAL VARIATION ; WAVELET TRANSFORM ; SUNSPOT NUMBERS ; VOYAGER 1 ; CYCLE |
资助项目 | NASA ; ONR ; NSF ; Mount Wilson Institute ; National Natural Science Foundation of China[11573065] ; National Natural Science Foundation of China[11503082] ; National Natural Science Foundation of China[11633008] ; National Natural Science Foundation of China[11603069] ; Foundation of the Sichuan University of Science and Engineering[2015RC43] ; Chinese Academy of Sciences |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | IOP PUBLISHING LTD |
WOS记录号 | WOS:000444462300003 |
资助机构 | NASA ; ONR ; NSF ; Mount Wilson Institute ; National Natural Science Foundation of China[11573065, 11503082, 11633008, 11603069] ; Foundation of the Sichuan University of Science and Engineering[2015RC43] ; Chinese Academy of Sciences |
源URL | [http://ir.ynao.ac.cn/handle/114a53/17916] |
专题 | 云南天文台_抚仙湖太阳观测站 |
通讯作者 | Xiang NB(向南彬) |
作者单位 | 1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, People's Republic of China 2.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China 3.Key Laboratory of Solar Activity, National Astronomical Observatories, CAS, Beijing 100012, People's Republic of China 4.Department of Physics, School of Science, Sichuan University of Science and Engineering, Zigong 643000, People's Republic of China |
推荐引用方式 GB/T 7714 | Xiang NB,Qu, Z. N.. Evolutionary Characteristics of the Interplanetary Magnetic Field Intensity[J]. ASTRONOMICAL JOURNAL,2018,156(4):11. |
APA | Xiang NB,&Qu, Z. N..(2018).Evolutionary Characteristics of the Interplanetary Magnetic Field Intensity.ASTRONOMICAL JOURNAL,156(4),11. |
MLA | Xiang NB,et al."Evolutionary Characteristics of the Interplanetary Magnetic Field Intensity".ASTRONOMICAL JOURNAL 156.4(2018):11. |
入库方式: OAI收割
来源:云南天文台
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