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Driving and damping of oscillations

  • Robert F. Stein
  • Åke Nordlund
Part III Excitation Mechanism of Oscillations
Part of the Lecture Notes in Physics book series (LNP, volume 367)

Abstract

We have simulated the upper 2.5 Mm of the solar convection zone using a realistic, three-dimensional, compressible, hydrodynamic computer code. P-mode oscillations are excited at the eigenfrequencies of the simulation volume. We have calculated the time averages of the work terms in the kinetic energy equation, using the internal energy equation to evaluate the fluctuations in the gas pressure. This calculation shows that the modes are excited near the surface by the divergence of the convective flux and damped by the divergence of the radiative flux. The fundamental mode is also spuriously driven at the lower boundary, by density and turbulent pressure fluctuations induced when downward plunging convective plumes pass through the lower boundary of the simulation.

Keywords

Fundamental Mode Solar Surface Convective Flux Boundary Work Solar Convection Zone 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

  1. Ando, H., and Osaki, Y. 1975, Publ. Astron. Soc. Japan, 27, 581.Google Scholar
  2. Christensen-Dalsgaard, J., and Frandsen, S. 1983, Solar Phys., 82, 165.Google Scholar
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  5. Libbrecht, K.G. 1988, in Seismology of the Sun and Sun-Like Stars, ed. E.J. Rolfe, ESA SP-286 (ESA Publication Division, Noordwijk), p.3.Google Scholar
  6. Stein, R.F., and Nordlund, A. 1989, Astrophys. J. Letters, 342, L95.Google Scholar

Copyright information

© Springer-Verlag 1990

Authors and Affiliations

  • Robert F. Stein
    • 1
  • Åke Nordlund
    • 2
  1. 1.Dept. Physics-AstronomyMichigan State UniversityEast LansingUSA
  2. 2.Copenhagen University ObservatoryCopenhagen KDenmark

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