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Magneto-seismology: effect of inhomogeneous magnetic field on transversal coronal loop oscillations

Published online by Cambridge University Press:  01 September 2007

G. Verth
G. Verth*
Affiliation:
SP2RC, Department of Applied Mathematics, University of Sheffield, Sheffield S3 7RH, UK email: G.Verth@sheffield.ac.uk
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Abstract

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The extreme-ultraviolet (EUV) imagers onboard the planned Solar Dynamics Observatory (SDO) and Solar Orbiter (SO) will offer us the best chance yet of using observations of post-flare loop oscillations to probe the fine structure of the corona. Recently developed magnetohydrodynamic (MHD) wave theory has shown that the properties of loop oscillations depend on their plasma fine structure. Up to this point, many studies have concentrated solely on the effect of plasma density stratification on coronal loop oscillations. In this paper we develop MHD wave theory which models the effect of an inhomogeneous magnetic field on coronal loop oscillations. The results have the potential to be used in testing the efficacy of photospheric magnetic field extrapolations and have important implications regarding magneto-seismology of the corona.

Keywords

(magnetohydrodynamics:) MHDwavesmagnetic fieldsSun: oscillationsSun: magnetic fieldsSun: fundamental parametersSun: corona
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S247: Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology , September 2007 , pp. 123 - 132
Copyright
Copyright © International Astronomical Union 2008

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