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Magnetic helicity transported by flux emergence and shuffling motions

Published online by Cambridge University Press:  18 July 2013

Y. Zhang ,
R. Kitai  and
K. Takizawa
Y. Zhang
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of Chinese Academy of Sciences email: zhangyin@bao.ac.cn Kwasan and Hida Observatories, Kyoto University, Yamashina-ku, Kyoto 607-8471 email: takizawa@kwasan.kyoto-u.ac.jpkitai@kwasan.kyoto-u.ac.jp
R. Kitai
Affiliation:
Kwasan and Hida Observatories, Kyoto University, Yamashina-ku, Kyoto 607-8471 email: takizawa@kwasan.kyoto-u.ac.jpkitai@kwasan.kyoto-u.ac.jp
K. Takizawa
Affiliation:
Kwasan and Hida Observatories, Kyoto University, Yamashina-ku, Kyoto 607-8471 email: takizawa@kwasan.kyoto-u.ac.jpkitai@kwasan.kyoto-u.ac.jp
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Abstract

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Magnetic helicity can be transported from sub-photosphere into corona by the emergence of helical magnetic field lines and the shuffling motions of foot-points of pre-existing coronal field lines. Active region NOAA 10930 was observed by SP and NFI of SOT on board Hinode when it pass through the solar meridian. Based on these observations, we calculate magnetic helicity flow of both terms, by regarding Doppler velocity as normal velocity. The results are compared with which calculated by method proposed by Zhang et. al. (2012). Our results show that helicity injection maps calculated by both methods have similar distribution and the integration values have the same magnitude.

Keywords

sun: activitysun: photospheresun: surface magnetism
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S294: Solar and Astrophysical Dynamos and Magnetic Activity , August 2012 , pp. 319 - 320
Copyright
Copyright © International Astronomical Union 2013 

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