Solar seismology. I. The stability of the solar p-modes

Journal Article · Tue Feb 01 04:00:00 EST 1977 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/155005· OSTI ID:7223002

Goldreich, P; Keeley, D A

We investigate the stability of the radial p-modes of the Sun by computing nonadiabatic eigenvalues and eigenfunctions for a solar envelope model which extends from an inner radius rapprox. =0.3 R/sub sun/ out to an optical depth tauapprox. =3 x 10/sup -4/. Our 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 of our calculations are as follows. If damping by turbulent viscosity is neglected all modes with periods longer than 6 minutes are unstable. The familiar k-mechanism, which operates in the H ionization--H/sup -/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 our estimate of turbulent damping, we conclude that theoretical calculations cannot unequivocally resolve the question of the stability of the solar p-modes.

• Research Organization: California Institute of Technology, Pasadena
• OSTI ID: 7223002
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 211:3; 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
FLUID MECHANICS
HEAT TRANSFER
HYDRODYNAMICS
MATHEMATICAL MODELS
MECHANICS
OSCILLATION MODES
PULSATIONS
SOLAR ACTIVITY
SOLAR GRANULATION
STAR MODELS
STARS
STELLAR ATMOSPHERES
SUN
TURBULENCE
VISCOSITY