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Title:
Putting Coronal Seismology Estimates of the Magnetic Field Strength to the Test
Authors:
De Moortel, I.; Pascoe, D. J.
Affiliation:
AA(School of Mathematics and Statistics, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS, UK), AB(School of Mathematics and Statistics, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS, UK)
Publication:
The Astrophysical Journal Letters, Volume 699, Issue 2, pp. L72-L75 (2009). (ApJL Homepage)
Publication Date:
07/2009
Origin:
IOP
Astronomy Keywords:
Sun: activity, Sun: corona, Sun: magnetic fields, Sun: oscillations
DOI:
10.1088/0004-637X/699/2/L72
Bibliographic Code:
2009ApJ...699L..72D

Abstract

The magnetic field strength inside a model coronal loop is "estimated" using coronal seismology, to examine the reliability of magnetic field strengths derived from observed, transverse coronal loop oscillations. Three-dimensional numerical simulations of the interaction of an external pressure pulse with a coronal loop (modeled as a three-dimensional density enhancement inside a two-dimensional magnetic arcade) are analyzed and the "observed" properties of the excited transverse loop oscillations are used to derive the value of the local magnetic field strength, following the method of Nakariakov & Ofman. Due to the (unexpected) change in periodicity, the magnetic field derived from our "observed" oscillation is substantially different from the actual (input) magnetic field value (approximately 50%). Coronal seismology can derive useful information about the local magnetic field, but the combined effect of the loop curvature, the density ratio, and aspect ratio of the loop appears to be more important than previously expected.
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