Refined Magnetoseismological Technique for the Solar Corona

Details Refined Magnetoseismological Technique for the Solar Corona Refined Magnetoseismological Technique for the Solar Corona

Nov 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...687l..45v&link_type=abstract

The Astrophysical Journal, Volume 687, Issue 1, pp. L45-L48.

Astronomy and Astrophysics

Astronomy

28

Magnetohydrodynamics: Mhd, Sun: Corona, Sun: Magnetic Fields, Sun: Oscillations

Scientific paper

We present a step-by-step guide of a refined magnetoseismological technique for plasma diagnostics in the Sun's corona. Recently developed MHD wave theory which models a coronal loop as an expanding magnetic flux tube with an arbitrary longitudinal plasma density profile is applied to TRACE observations of fast kink oscillations. The theory predicts that using the observed ratio of the first overtone and fundamental mode to predict the plasma density scale height and not taking account of loop expansion will lead to an overestimation of scale height. For the first time, the size of this correction is quantified directly from observation and for the particular case study presented here, it is found that the overestimation is approximately by a factor of 2.

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