Excitation of the solar p-modes by turbulent stress

We have revisited the problem of solar p-mode generation by turbulent stress in the outer part of the Sun, and the product (E) over dot = E Gamma, the rate at which energy is supplied to a single solar p-mode. We assume that Gamma measures energy decay rate of the mode. Away from the peak, (E) over dot proportional to nu(7) for nu < 3mHz and (E) over dot proportional to nu(-5) for nu > 3mHz. The resulting oscillation power spectra can be made to agree roughly with the observations by adjusting theoretical parameters. In this paper, we correct the earlier computations by incorporating an improved description of the spatial and temporal spectrum of turbulent convection, and show how the mode energy generated in the Sun on the basis of a mixing-length model of the solar convection zone is strongly dependent on the solar model. In the present paper, we argue that the solar p-modes are primarily excited as a consequence of the emission of acoustic radiation by turbulent convective flows.