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Magneto-seismology of solar atmospheric loops by means of longitudinal oscillations

Published online by Cambridge University Press:  05 July 2012

M. Luna-Cardozo ,
G. Verth  and
R. Erdélyi
M. Luna-Cardozo
Affiliation:
Instituto de Astronomía y Física del Espacio (IAFE), CONICET-UBA, CC. 67, Suc. 28, 1428 Buenos Aires, Argentina. email: mluna@iafe.uba.ar Solar Physics and Space Plasma Research Centre (SP2RC), University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK. email: robertus@sheffield.ac.uk
G. Verth
Affiliation:
School of Computing, Engineering and Information Sciences, Northumbria University, Newcastle Upon Tyne, NE1 8ST, UK. email: gary.verth@northumbria.ac.uk
R. Erdélyi
Affiliation:
Solar Physics and Space Plasma Research Centre (SP2RC), University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK. email: robertus@sheffield.ac.uk
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Abstract

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There is increasingly strong observational evidence that slow magnetoacoustic modes arise in the solar atmosphere. Solar magneto-seismology is a novel tool to derive otherwise directly un-measurable properties of the solar atmosphere when magnetohydrodynamic (MHD) wave theory is compared to wave observations. Here, MHD wave theory is further developed illustrating how information about the magnetic and density structure along coronal loops can be determined by measuring the frequencies of the slow MHD oscillations. The application to observations of slow magnetoacoustic waves in coronal loops is discussed.

Keywords

(magnetohydrodynamics:) MHDSun: coronaSun: fundamental parametersSun: magnetic fieldsSun: oscillationsWaves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S286: Comparative Magnetic Minima: Characterizing quiet times in the Sun and Stars , October 2011 , pp. 437 - 440
Copyright
Copyright © International Astronomical Union 2012

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