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Solar seismology. II - The stochastic excitation of the solar p-modes by turbulent convection
Goldreich, P.; Keeley, D. A.
AA(California Institute of Technology, Pasadena, Calif.), AB(Lick Observatory, Santa Cruz, Calif.)
Astrophysical Journal, Part 1, vol. 212, Feb. 15, 1977, p. 243-251. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Atmospheric Turbulence, Convective Flow, Seismology, Solar Atmosphere, Stochastic Processes, Turbulence Effects, Atmospheric Models, Kinetic Energy, Modal Response, Perturbation Theory, Vortices
Bibliographic Code:


We test the hypothesis that the solar p-modes are stabilized by damping due to turbulent viscosity in the convective zone. Starting from the assumption that the modes are stable, we calculate expectation values for the modal energies. We find that the interaction between a p-mode and the turbulent convection is such that the modal energy tends toward equipartition with the kinetic energy of turbulent eddies whose lifetimes are comparable to the modal period. From the calculated values of the modal energies, we compute rms surface velocity amplitudes. Our predicted rms surface velocities range from 0.01 cm/sec for the fundamental radial mode to 0.6 cm/sec for the radial mode whose period is approximately 5 minutes. The predicted surface velocities for the low order p-modes are much smaller than the velocities inferred from recent observations.

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