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On the Relationship Between G-Band Bright Point Dynamics and Their Magnetic Field Strengths
Yang, Yunfei1,2; Li, Qiang1; Ji, Kaifan1; Feng, Song1,2; Deng, Hui1; Wang F(王锋)1,3; Lin, Jiaben2
Source PublicationSOLAR PHYSICS
2016-04-01
Volume291Issue:4Pages:1089-1105
DOI10.1007/s11207-016-0889-y
Contribution Rank第3完成单位
Indexed BySCI
KeywordBright points, Photosphere Dynamics, Magnetic Magnetic fields, Photosphere
Abstract

G-band bright points (GBPs) are regarded as good manifestations of magnetic flux concentrations. We aim to investigate the relation between the dynamic properties of GBPs and their longitudinal magnetic field strengths. High spatial and temporal resolution observations were recorded simultaneously with G-band filtergrams and Narrow-band Filter Imager (NFI) Stokes I and V images with Hinode/Solar Optical Telescope. The GBPs are automatically identified and tracked in the G-band images, and the corresponding longitudinal magnetic field strength of each GBP is extracted from the calibrated NFI magnetograms by a point-to-point method. After categorizing the GBPs into five groups by their longitudinal magnetic field strengths, we analyzed the dynamics of each group of GBPs. The results suggest that with increasing longitudinal magnetic field strengths of GBPs correspond to a decrease in their horizontal velocities and motion ranges as well as by showing more complex motion paths. This suggests that magnetic elements showing weaker magnetic field strengths move faster and farther along straighter paths, while stronger elements move more slowly in more erratic paths within a smaller region. The dynamic behaviors of GBPs with different longitudinal magnetic field strengths can be explained by that the stronger flux concentrations withstand the convective flows much better than weaker ones.

Funding ProjectNational Natural Science Foundation of China[11303011] ; National Natural Science Foundation of China[11573012] ; National Natural Science Foundation of China[11463003] ; National Natural Science Foundation of China[U1231205] ; Open Research Program of the Key Laboratory of Solar Activity of the Chinese Academy of Sciences[KLSA201414] ; Open Research Program of the Key Laboratory of Solar Activity of the Chinese Academy of Sciences[KLSA201505]
Funding OrganizationNational Natural Science Foundation of China[11303011, 11573012, 11463003, U1231205] ; Open Research Program of the Key Laboratory of Solar Activity of the Chinese Academy of Sciences[KLSA201414, KLSA201505]
Language英语
Subject Area天文学 ; 太阳与太阳系 ; 太阳物理学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherSPRINGER
Publication PlaceVAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
ISSN0038-0938
URL查看原文
WOS IDWOS:000378240000004
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordSOLAR OPTICAL TELESCOPE ; ACTIVE-REGION ; FLUX TUBES ; WAVE-PROPAGATION ; QUIET SUN ; PHOTOSPHERE ; SIMULATIONS ; CALIBRATION ; DISPERSAL ; ELEMENTS
Citation statistics
Cited Times:6[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/9615
Collection其他
Corresponding AuthorJi, Kaifan
Affiliation1.Faculty of Information Engineering and Automation/Yunnan Key Laboratory of Computer Technology Application, Kunming University of Science and Technology, 650500, Kunming, China
2.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China
3.Yunnan Observatory, Chinese Academy of Sciences, 650011, Kunming, China
Recommended Citation
GB/T 7714
Yang, Yunfei,Li, Qiang,Ji, Kaifan,et al. On the Relationship Between G-Band Bright Point Dynamics and Their Magnetic Field Strengths[J]. SOLAR PHYSICS,2016,291(4):1089-1105.
APA Yang, Yunfei.,Li, Qiang.,Ji, Kaifan.,Feng, Song.,Deng, Hui.,...&Lin, Jiaben.(2016).On the Relationship Between G-Band Bright Point Dynamics and Their Magnetic Field Strengths.SOLAR PHYSICS,291(4),1089-1105.
MLA Yang, Yunfei,et al."On the Relationship Between G-Band Bright Point Dynamics and Their Magnetic Field Strengths".SOLAR PHYSICS 291.4(2016):1089-1105.
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