Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-11T04:38:16.214Z Has data issue: false hasContentIssue false
  • English
  • Français

Study of the change of surface magnetic field associated with flares

Published online by Cambridge University Press:  26 August 2011

Yixuan Li ,
Ju Jing ,
Yuhong Fan  and
Haimin Wang
Yixuan Li
Affiliation:
Space Weather Research Lab, New Jersey Institute of Technology, Newark, USA email: yl89@njit.edu, jj4@njit.edu, haimin@flare.njit.edu
Ju Jing
Affiliation:
Space Weather Research Lab, New Jersey Institute of Technology, Newark, USA email: yl89@njit.edu, jj4@njit.edu, haimin@flare.njit.edu
Yuhong Fan
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research†, Boulder, USA email: yfan@ucar.edu
Haimin Wang
Affiliation:
Space Weather Research Lab, New Jersey Institute of Technology, Newark, USA email: yl89@njit.edu, jj4@njit.edu, haimin@flare.njit.edu
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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).

Keywords

Sun: flaressun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 417 - 421
Copyright
Copyright © International Astronomical Union 2011

References

Hudson, H. S., Fisher, G. H., & Welsch, B. T. 2008, Subsurface and Atmospheric Influences on Solar Activity, 383, 221Google Scholar
Liu, C., Deng, N., Liu, Y., Falconer, D., Goode, P. R., Denker, C., & Wang, H. 2005, Astrophys. J., 622, 722CrossRefGoogle Scholar
Fan, Y. 2010, Astrophys. J., 719, 728CrossRefGoogle Scholar
Metcalf, T. R. 1994, Solar Phys., 155, 235CrossRefGoogle Scholar
Moore, R. L., Sterling, A. C., Hudson, H. S., & Lemen, J. R. 2001, Astrophys. J., 552, 833CrossRefGoogle Scholar