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 velocities that are 10 times larger than the observed upper limits and hence are ruled out by existing data. We also demonstrate that any large-amplitude, short-period oscillations that grow on a Kelvin-Helmholtz time scale will require, to affect solar neutrino fluxes, a large amount of energy (for g-modes, 10 times the energy in the observed p− mode oscillations) and a tiny amount of dissipation (for g-modes, 10 the dissipation rate of the p-modes).