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Magneto‐seismology of the solar atmosphere
Author(s) -
Verth G.
Publication year - 2007
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.200710796
Subject(s) - physics , magnetohydrodynamic drive , solar atmosphere , magnetohydrodynamics , corona (planetary geology) , atmosphere (unit) , coronal loop , amplitude , space weather , coronal mass ejection , magneto , computational physics , nanoflares , coronal hole , solar wind , measure (data warehouse) , solar physics , astrophysics , geophysics , magnetic field , astrobiology , optics , meteorology , power (physics) , quantum mechanics , database , venus , computer science
Magnetohydrodynamic (MHD) waves in solar coronal loops, which were previously only predicted by theory have actually been detected with space‐borne instruments. These observations have given an important and novel tool to measure fundamental parameters in the magnetically embedded solar corona. This paper will illustrate how information about the magnetic and density structure along coronal loops can be determined by measuring the frequency or amplitude profiles of standing fast kink mode oscillations. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)