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Relaxation of magnetic field relative to plasma density during solar flares

Published online by Cambridge University Press:  18 July 2013

Sijie Yu ,
Yihua Yan  and
Baolin Tan
Sijie Yu
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China email: sjyu@nao.cas.cn
Yihua Yan
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China email: sjyu@nao.cas.cn
Baolin Tan
Affiliation:
Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, Beijing 100012, China email: sjyu@nao.cas.cn
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Abstract

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We investigated the variations of 74 microwave ZP structures observed by Chinese Solar Broadband Radio Spectrometer at 2.6–3.8 GHz in 9 solar flares, found that the ratio between the plasma density scale height LN and the magnetic field scale height LB in emission source displays a tendency of decrease during the flaring process, indicates that LB increases faster than the LN during solar flares. The detailed analysis of the step-wise decrease of LN/LB in three typical X-class flares reveals the magnetic field relaxation relative to the plasma density.

Keywords

Sun: flares — Sun: magnetic topology — Sun: radio radiation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S294: Solar and Astrophysical Dynamos and Magnetic Activity , August 2012 , pp. 589 - 590
Copyright
Copyright © International Astronomical Union 2013 

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