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Effect of a Steady Flow and an Atmospheric Magnetic Field on the Solar p- and f-Modes

Published online by Cambridge University Press:  13 May 2016

R. Erdélyi  and
Y. Taroyan
R. Erdélyi
Affiliation:
Department of Applied Mathematics, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK. Email: Robertus@sheffield.ac.uk
Y. Taroyan
Affiliation:
Department of Applied Mathematics, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK. Email: Robertus@sheffield.ac.uk

Abstract

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The combined effect of a subsurface steady homogeneous flow and a chromospheric uniform magnetic field on the solar p- and f-modes is evaluated theoretically for a simple model of the Sun. The derived dispersion relation is solved analytically in limit of the long wavelength approximation and is evaluated numerically for arbitrary wavelengths. The influence of an equilibrium flow is more dominant in limit of small wavenumbers. For arbitrary wavelengths the effect of a magnetic field might be stronger than frequency shifts caused by a steady homogeneous flow.

Information

Type
Session II: Convection Zone and Local Area Helioseismology
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 208 - 210
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

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