Excitation of solar p-modes

On the basis of a 5-dimensional, time/space separated description of convec tive turbulence and the mixing length theory we: calculated the excitation rate (E) over dot = E Gamma for a single solar p-mode. We found that (E) ov er dot varies as nu(7) or nu(-5) according as nu is below or above 3 mHz. O ur result for the higher frequencies resolves a previous difficulty with th e observations. It appears that solar p-modes are excited mainly by Reynold s stress fluctuations, rather than by entropy fluctuations.