The Rotation of the Solar Photospheric Magnetic Field
文献类型:期刊论文
作者 | Xu JC(徐景晨)1,2,3,4; Gao PX(高朋鑫)1,4 |
刊名 | ASTROPHYSICAL JOURNAL |
出版日期 | 2016-12-20 |
卷号 | 833期号:2 |
ISSN号 | 0004-637X |
关键词 | Sun: Activity Sun: Magnetic Fields Sun: Photosphere Sun: Rotation |
DOI | 10.3847/1538-4357/833/2/144 |
产权排序 | 第1完成单位 |
文献子类 | Article |
英文摘要 | The rotational characteristics of the solar photospheric magnetic field at four flux ranges are investigated together with the total flux of active regions (MFar) and quiet regions (MFqr). The first four ranges (MF1-4) are (1.5-2.9) × 1018, (2.9-32.0) × 1018, (3.20-4.27) × 1019, and (4.27-38.01) × 1019, respectively (the unit is Mx per element). Daily values of the flux data are extracted from magnetograms of the Michelson Doppler Imager on board the Solar and Heliospheric Observatory. Lomb-Scargle periodograms show that only MF2, MF4, MFqr, and MFar exhibit rotational periods. The periods of the first three types of flux are very similar, i.e., 26.20, 26.23, and 26.24 days, respectively, while that of MFar is longer, 26.66 days. This indicates that active regions rotate more slowly than quiet regions on average, and strong magnetic fields tend to repress the surface rotation. Sinusoidal function fittings and cross-correlation analyses reveal that MFar leads MF2 and MF4 by 5 and 1 days, respectively. This is speculated to be related with the decaying of active regions. MF2 and MFar are negatively correlated, while both MF4 and MFqr are positively correlated with MFar. At the timescale of the solar activity cycle, MFar leads (negatively) MF2 by around one year (350 days), and leads MF4 by about 3 rotation periods (82 days). The relation between MF2 and MFar may be explained by the possibility that the former mainly comes from a higher latitude, or emerges from the subsurface shear layer. We conjecture that MF4 may partly come from the magnetic flux of active regions; this verifies previous results that were obtained with indirect solar magnetic indices. |
学科主题 | 天文学 ; 太阳与太阳系 ; 太阳物理学 |
URL标识 | 查看原文 |
出版地 | TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND |
WOS关键词 | MICHELSON DOPPLER IMAGER ; LOMB-SCARGLE PERIODOGRAM ; DIFFERENTIAL ROTATION ; CYCLE 23 ; IRRADIANCE VARIATIONS ; SPECTRAL-ANALYSIS ; CONVECTION ZONE ; SUNSPOT GROUPS ; LEAST-SQUARES ; HIGH-LATITUDE |
资助项目 | National Natural Science Foundation of China[11573065] ; National Natural Science Foundation of China[11633008] ; National Natural Science Foundation of China[11273057] ; National Natural Science Foundation of China[11673061] ; Specialized Research Fund for State Key Laboratories ; Chinese Academy of Sciences ; Applied Basic Research Foundation of Yunnan Province, China[2014FB190] |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | IOP PUBLISHING LTD |
WOS记录号 | WOS:000391169600019 |
资助机构 | National Natural Science Foundation of China[11573065, 11633008, 11273057, 11673061] ; Specialized Research Fund for State Key Laboratories ; Chinese Academy of Sciences ; Applied Basic Research Foundation of Yunnan Province, China[2014FB190] |
源URL | [http://ir.ynao.ac.cn/handle/114a53/9850] |
专题 | 云南天文台_太阳物理研究组 |
通讯作者 | Xu JC(徐景晨) |
作者单位 | 1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China 2.University of Chinese Academy of Sciences, Beijing 100049, China 3.State Key Laboratory of Space Weather, Chinese Academy of Sciences, Beijing 100190, China 4.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China |
推荐引用方式 GB/T 7714 | Xu JC,Gao PX. The Rotation of the Solar Photospheric Magnetic Field[J]. ASTROPHYSICAL JOURNAL,2016,833(2). |
APA | Xu JC,&Gao PX.(2016).The Rotation of the Solar Photospheric Magnetic Field.ASTROPHYSICAL JOURNAL,833(2). |
MLA | Xu JC,et al."The Rotation of the Solar Photospheric Magnetic Field".ASTROPHYSICAL JOURNAL 833.2(2016). |
入库方式: OAI收割
来源:云南天文台
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