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The solar active region magnetic field and energetics

Published online by Cambridge University Press:  26 August 2011

Qiang Hu ,
Na Deng ,
Debi P. Choudhary ,
B. Dasgupta  and
Jiangtao Su
Qiang Hu
Affiliation:
CSPAR, University of Alabama in Huntsville, Huntsville, AL, United States email: qh0001@uah.edu
Na Deng
Affiliation:
California State University Northridge, Northridge, CA, United States
Debi P. Choudhary
Affiliation:
California State University Northridge, Northridge, CA, United States
B. Dasgupta
Affiliation:
CSPAR, University of Alabama in Huntsville, Huntsville, AL, United States email: qh0001@uah.edu
Jiangtao Su
Affiliation:
National Astronomical Observatories, Beijing, China
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Abstract

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Motivated by increasingly more advanced solar observations, we recently develop a method of coronal magnetic field extrapolation, especially for an active region (sunspot region). Based on a more complex variational principle, the principle of minimum (energy) dissipation rate (MDR), we adopt and solve a more complex equation governing the coronal magnetic field that is non-force-free in general. We employ the vector magnetograms from multiple instruments, including Hinode, NSO, and HSOS, and particularly observations at both photospheric and chromospheric levels for one active region. We discuss our results in the context of quantitative characterization of active region magnetic energy and magnetic topology. These quantitative analyses aid in better understanding and developing prediction capability of the solar activity that is largely driven by the solar magnetic field.

Keywords

MHDmethods: data analysisSun: corona
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 369 - 373
Copyright
Copyright © International Astronomical Union 2011

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