Comparison between observation and simulation of magnetic field changes associated with flares

Document Type

Article

Publication Date

1-20-2011

Abstract

It has been a long-standing question in solar physics how magnetic field structure changes with eruptive events (e.g., flares and coronal mass ejections). In this Letter, we present the eruption-associated changes in the magnetic inclination angle, the horizontal component of magnetic field vectors, and the Lorentz force. The analysis is based on the observation of the X3.4 flare on 2006 December 13 and in comparison to the numerical simulation of 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 the flaring polarity inversion line (PIL) deceases after the flare; (2) the horizontal component of magnetic field increases at the lower altitude near the flaring PIL after the flare. The result suggests that the field lines at the flaring neutral line turn to more horizontal near the surface, that is in agreement with the prediction of Hudson et al. © 2011. The American Astronomical Society. All rights reserved. Printedin the U.S.A.

Identifier

79960245716 (Scopus)

Publication Title

Astrophysical Journal Letters

External Full Text Location

https://doi.org/10.1088/2041-8205/727/1/L19

e-ISSN

20418213

ISSN

20418205

Issue

1 PART II

Volume

727

Grant

AGS-0936665

Fund Ref

National Science Foundation

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