Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...212..243g&link_type=abstract
Astrophysical Journal, Part 1, vol. 212, Feb. 15, 1977, p. 243-251.
Astronomy and Astrophysics
Astrophysics
190
Atmospheric Turbulence, Convective Flow, Seismology, Solar Atmosphere, Stochastic Processes, Turbulence Effects, Atmospheric Models, Kinetic Energy, Modal Response, Perturbation Theory, Vortices
Scientific paper
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.
Goldreich Peter
Keeley Douglas Allan
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