G-MODES AND THE SOLAR-NEUTRINO PROBLEM

We show that low-order g-modes with large enough amplitudes to affect significantly the solar neutrino fluxes would produce surface velociti es that are 10(4) times larger than the observed upper limits and henc e are ruled out by existing data. We also demonstrate that any large-a mplitude, short-period oscillations that grow on a Kelvin-Helmholtz ti me scale will require, to affect solar neutrino fluxes, a large amount of energy (for g-modes, 10(9) times the energy in the observed p-mode oscillations) and a tiny amount of dissipation (for g-modes, 10(-8) t he fractional dissipation rate of the p-modes).