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The Rotation of the Solar Photospheric Magnetic Field
Xu JC(徐景晨)1,2,3,4; Gao PX(高朋鑫)1,4; Xu, JC
发表期刊ASTROPHYSICAL JOURNAL
2016-12-20
卷号833期号:2
DOI10.3847/1538-4357/833/2/144
产权排序第1完成单位
收录类别SCI
关键词Sun: Activity Sun: Magnetic Fields Sun: Photosphere Sun: Rotation
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.
项目资助者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)
语种英语
学科领域天文学
文章类型Article
ISSN0004-637X
URL查看原文
归档日期2016-12-16
WOS记录号WOS:000391169600019
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]MICHELSON DOPPLER IMAGER ; LOMB-SCARGLE PERIODOGRAM ; DIFFERENTIAL ROTATION ; CYCLE 23 ; IRRADIANCE VARIATIONS ; SPECTRAL-ANALYSIS ; CONVECTION ZONE ; SUNSPOT GROUPS ; LEAST-SQUARES ; HIGH-LATITUDE
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被引频次:6[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/9850
专题太阳物理研究组
通讯作者Xu, JC
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
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Xu JC,Gao PX,Xu, JC. The Rotation of the Solar Photospheric Magnetic Field[J]. ASTROPHYSICAL JOURNAL,2016,833(2).
APA Xu JC,Gao PX,&Xu, JC.(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).
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