Solar seismology. II. The stochastic excitation of the solar p-modes by turbulent convection

Journal Article · Tue Feb 15 04:00:00 EST 1977 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/155043· OSTI ID:7216478

Goldreich, P; Keeley, D A

We test the hypothesis that the solar rho-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 1 x 10/sup -2/ cm s/sup -1/ for the fundamental radial mode to 0.6 cm s/sup -1/ for the radial mode whose period is approximately 5 minutes. The predicted surface velocities for the low order p-modes (periods >20 min) are much smaller than the velocities inferred from recent observations by Hill, Stebbins, and Brown and by Brookes, Isaak, and van der Raay.

• Research Organization: California Institute of Technology
• OSTI ID: 7216478
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 212:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
CONVECTION
ENERGY TRANSFER
EQUATIONS
EQUATIONS OF STATE
HEAT TRANSFER
MATHEMATICAL MODELS
PULSATIONS
SOLAR ATMOSPHERE
STAR MODELS
STARS
SUN
TURBULENCE
VISCOSITY
VORTICES