Hostname: page-component-586b7cd67f-g8jcs Total loading time: 0 Render date: 2024-11-27T23:05:26.608Z Has data issue: false hasContentIssue false
  • English
  • Français

Damping rates of p-modes by an ensemble of randomly distributed thin magnetic flux tubes

Published online by Cambridge University Press:  26 August 2011

Andrew Gascoyne  and
Rekha Jain
Andrew Gascoyne
Affiliation:
Department of Applied Mathematics, University of Sheffield, UK email: [email protected], [email protected]
Rekha Jain
Affiliation:
Department of Applied Mathematics, University of Sheffield, UK email: [email protected], [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The magnetohydrodynamic (MHD) sausage tube waves are excited in the magnetic flux tubes by p-mode forcing. These tube waves thus carry energy away from the p-mode cavity which results in the deficit of incident p-mode energy. We calculate the loss of incident p-mode energy as a damping rate of f- and p-modes. We calculate the damping rates of f- and p-modes by a model Sun consisting of an ensemble of many thin magnetic flux tubes with varying plasma properties and distributions. Each magnetic flux tube is modelled as axisymmetric, vertically oriented and untwisted. We find that the magnitude and the form of the damping rates are sensitive to the plasma-β of the tubes and the upper boundary condition used.

Keywords

Sun: magnetic fieldsSun: helioseismologySun: oscillationsMHDScattering
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 351 - 355
Copyright
Copyright © International Astronomical Union 2011

References

Abramowitz, M. & Stegun, I. A. 1964, Handbook of Mathematical Functions (New York: Dover)Google Scholar
Bogdan, T. J. & Cally, P. S. 1995, Astrophys. J., 453, 919CrossRefGoogle Scholar
Bogdan, T. J., Hindman, B. W., Cally, P. S., & Charbonneau, P. 1996, Astrophys. J., 465, 406CrossRefGoogle Scholar
Braun, D. C., Duvall, T. L., & LaBonte, B. J. 1988, Astrophys. J., 335, 1015CrossRefGoogle Scholar
Braun, D. C., Birch, A. C. 2008, Solar Phys., 251, 267CrossRefGoogle Scholar
Couvidat, S., Birch, A. C., & Kosovichev, A. G. 2006, Astrophys. J., 640, 516CrossRefGoogle Scholar
Crouch, A. D. & Cally, P. S. 2005, Solar Phys., 227, 1CrossRefGoogle Scholar
Hindman, B. W. & Jain, R. 2008, Astrophys. J., 677, 769CrossRefGoogle Scholar
Jain, R., Hindman, B., Braun, D. C., & Birch, A. C. 2009, Astrophys. J., April 10 issue.Google Scholar
Maltby, P., Avrett, E. H., Carlsson, M., Kjelsdeth-Moe, O., Kurucz, R. L., & Loeser, R. 1986, Astrophys. J., 306, 284CrossRefGoogle Scholar
Spruit, H. C. 1991, in Toomre, J., Gough, D. O., eds, Lecture Notes in Physics, Vol. 388, Challenges to Theories of the Structure of Moderate Mass Stars. Springer-Verlag, Berlin, p. 121CrossRefGoogle Scholar