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Influence of a Uniform Coronal Magnetic Field on Solar p Modes: Coupling to Slow Resonant MHD Waves

Published online by Cambridge University Press:  12 April 2016

P. Vanlommel ,
A. Debosscher ,
J. Andries  and
M. Goossens
P. Vanlommel
Affiliation:
Centre for Plasma Astrophysics, K.U.Leuven, Celestijnenlaan 200B, B-3001 Heverlee, Belgium
A. Debosscher
Affiliation:
Centre for Plasma Astrophysics, K.U.Leuven, Celestijnenlaan 200B, B-3001 Heverlee, Belgium
J. Andries
Affiliation:
Centre for Plasma Astrophysics, K.U.Leuven, Celestijnenlaan 200B, B-3001 Heverlee, Belgium
M. Goossens
Affiliation:
Centre for Plasma Astrophysics, K.U.Leuven, Celestijnenlaan 200B, B-3001 Heverlee, Belgium

Abstract

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The influence of a constant coronal magnetic field on solar global oscillations is investigated for a simple planar equilibrium model. The model consists of an atmosphere with a constant horizontal magnetic field on top of a unmagnetized solar interior. The focus is on the possible resonant coupling of global solar oscillation modes to local slow continuum modes of the atmosphere and the consequent damping of the global oscillations.

Type
Part 4. The Interaction between Convection and Pulsation
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 480 - 481
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

Vanlommel, P., & Goossens, M. 1999, Solar Phys., 187, 357 Google Scholar
Vanlommel, P., Debosscher, A., Andries, J., & Goossens, M. 2001, Solar Phys., in pressGoogle Scholar