Excitation of solar G modes with periods near 160 minutes
Solar g modes with ℓ 1 to 4 and periods near 160 minutes have been investigated using a solar model with normal structure. Radiative dissipation in the region below the convection zone is much greater than the driving provided by nuclear reactions or the opacity mechanism. A crude treatment of convection suggests that it also is not an important source of driving. The damping due to turbulent viscosity is also small. Excitation of these modes by coupling to convective turbulence is substantial in terms of the rms energy of the modes, but the surface velocity is very small because of the large amount of mass involved in the oscillation.
KeywordsConvection Zone Solar Model Convective Turbulence Convective Flux Solar Convection Zone
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- Brookes J.R. Isaak G.R. and van der Raay, H.B. 1976, Nature, 259, 92.Google Scholar
- Cox, J.P., Cox, A.N., Olsen, K.H., King, D.S. and Eilers, D.D. 1966, Ap. J., 144, 1038.Google Scholar
- Goldreich, P. and Keeley, D.A. 1977, Ap. J., 212, 243.Google Scholar
- Osaki, Y. 1975, Publ. Astron. Soc. Japan, 27, 237.Google Scholar
- Scherrer, P.H., Wilcox, J.M., Kotov, V.A., Severny, A.B. and Tsap, T.T. 1979, Nature, 277, 635.Google Scholar
- Severny, A.B., Kotov, V.A. and Tsap, T.T. 1976, Nature, 259, 87. *** DIRECT SUPPORT *** A3418083 00008Google Scholar