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Study of the change of surface magnetic field associated with flares

Published online by Cambridge University Press:  26 August 2011

Yixuan Li
Affiliation:
Space Weather Research Lab, New Jersey Institute of Technology, Newark, USA email: [email protected], [email protected], [email protected]
Ju Jing
Affiliation:
Space Weather Research Lab, New Jersey Institute of Technology, Newark, USA email: [email protected], [email protected], [email protected]
Yuhong Fan
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research†, Boulder, USA email: [email protected]
Haimin Wang
Affiliation:
Space Weather Research Lab, New Jersey Institute of Technology, Newark, USA email: [email protected], [email protected], [email protected]
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Abstract

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How magnetic field structure changes with eruptive events (e.g., flares and CMEs) has been a long-standing problem in solar physics. Here we present the analysis of eruption-associated changes in the magnetic inclination angle, the transverse component of magnetic field and the Lorentz force. The analysis is based on an observation of the X3.4 flare on Dec.13 2006 and a numerical simulation of a solar eruption made by Yuhong Fan. Both observation and simulation show that (1) the magnetic inclination angle in the decayed peripheral penumbra increases, while that in the central area close to flaring polarity inversion line (PIL) deceases after the flare; (2) the transverse component of magnetic field increases at the lower altitude near flaring PIL after the flare. The result suggests that the field lines at flaring neutral line turn to more horizontal near the surface, that is in agreement with the prediction of Hudson, Fisher & Welsch (2008).

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

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