  We argue that the solar g-modes are unlikely to have caused the discrete
peaks in the power spectrum of the solar wind flux observed by Thomson et al.
(1995). The lower limit to the energy of individual g-modes, using the
amplitudes given by Thomson et al., is estimated to be at least 10$^{36}$ erg
for low order g-modes; the resulting surface velocity amplitude is at least 50
cm s$^{-1}$, larger than the observational upper limit (5 cm s$^{-1}$).
  We suggest that the most likely source for the excitation of solar g-modes is
turbulent stresses in the convection zone. The surface velocity amplitude of
low degree and low order g-modes resulting from this process is estimated to be
of order 10$^{-2}$ cm s$^{-1}$. This amplitude is interestingly close to the
detection threshold of the SOHO satellite. The long lifetime of g-modes ($\sim
10^6$ years for low order modes) should be helpful in detecting these small
amplitude pulsations.
