Astronomy and Astrophysics – Astronomy
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008iaus..247..123v&link_type=abstract
Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology, Proceedings of the International Astronomical Unio
Astronomy and Astrophysics
Astronomy
3
(Magnetohydrodynamics:) Mhd, Waves, Magnetic Fields, Sun: Oscillations, Sun: Magnetic Fields, Sun: Fundamental Parameters, Sun: Corona
Scientific paper
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.
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