Physics
Scientific paper
Feb 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...211..934g&link_type=abstract
Astrophysical Journal, Part 1, vol. 211, Feb. 1, 1977, p. 934-942.
Physics
144
Pulsed Radiation, Seismology, Solar Atmosphere, Solar Physics, Stable Oscillations, Astronomical Models, Convective Flow, Eigenvalues, Linear Equations, Nonadiabatic Conditions, Optical Thickness, Radiative Transfer
Scientific paper
The stability of the radial p-modes of the sun is investigated by computing nonadiabatic eigenvalues and eigenfunctions for a solar envelope model which extends from an inner radius of about 0.3 solar radius out to an optical depth of about 0.0003. The calculations take into account in a crude fashion the response of the convective flux to the oscillation. The dynamical effect of turbulence in the convection zone is parametrized in terms of a turbulent shear viscosity. The results show that if damping by turbulent viscosity is neglected, all modes with periods longer than 6 minutes are unstable. The familiar kappa-mechanism, which operates in the H ionization-H(-) opacity region, is the dominant source of driving of the oscillations. Modes with periods shorter than 6 minutes are stabilized by radiative damping in the solar atmosphere. When turbulent dissipation of pulsational energy is included, all modes are predicted to be stable. However, the margin of stability is very small. In view of the large uncertainty that must be assigned to the estimate of turbulent damping, it is concluded that theoretical calculations cannot unequivocally resolve the question of the stability of the solar p-modes.
Goldreich Peter
Keeley Douglas Allan
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