Radiative and other effects from internal waves in solar and stellar interiors

Details Radiative and other effects from internal waves in solar and stellar interiors Radiative and other effects from internal waves in solar and stellar interiors

Apr 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...245..286p&link_type=abstract

Astrophysical Journal, Part 1, vol. 245, Apr. 1, 1981, p. 286-303.

Astronomy and Astrophysics

Astrophysics

131

Internal Waves, Radiative Transfer, Solar Interior, Solar Neutrinos, Stellar Interiors, Stellar Radiation, Stellar Structure, Boussinesq Approximation, Collimation, Convection, Diffusivity, Nonlinearity, Opacity, Perturbation Theory, Plasma Frequencies, Plasma Waves, Stellar Models, Stellar Oscillations, Sun, Turbulence Effects

Scientific paper

Starting from the usual spherical mode and planar Boussinesq formulations, equations are derived for the propagation and dissipation of internal gravity waves in a stellar interior. The sun is 'transparent' to such waves if they have sufficiently low mode number (less than 10) and high frequency (more than 10 times the convective overturn frequency). Even when spatially and temporally incoherent, such waves focus toward the center of the sun, so that their amplitude greatly increases there. An order of magnitude estimate suggests that the internal waves generated at the base of the convective zone may become nonlinear in amplitude close to the solar center. If this happens, several effects become important and can affect, e.g., the expected Cl-37 solar neutrino signature. Possible effects include (1) hydraulically enhanced diffusion of entropy, which can increase the effective radiative opacity of the solar material by a factor of order unity, and (2) wave-induced turbulence, which can lead to species mixing.

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