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The variations of solar magnetic networks over the solar cycle 23

Published online by Cambridge University Press:  18 July 2013

Chong Huang
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China
Yihua Yan
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China
Yuanyong Deng
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China
Yin Zhang
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China
Baolin Tan
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China
Gang Li
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China Department of Physics and CSPAR, University of Alabama in Huntsville, AL, 35899, USA email: chuang@nao.cas.cn
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Abstract

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This work analyzed the morphologic properties of magnetic networks during Carrington Rotations (CRs) 1955 to 2091 by applying the watershed algorithm to magnetograms observed by the Michelson Doppler Interferometer on board the Solar and Heliospheric Observatory spacecraft. We found that the magnetic networks are of fractal and the average fractal dimension is Df=1.253±0.011. We also find that both the fractal dimension and the size of magnetic networks are anti-correlated with the solar magnetic activity.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013 

References

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