Excitation of the solar p-modes by turbulent stress
Shaolan Bi and
Received 14 October 1996 / Accepted 6 October 1997
We have revisited the problem of solar p-mode generation by turbulent stress in the outer part of the Sun, and the product , the rate at which energy is suppLied to a single solar p-mode. We assume that measures energy decay rate of the mode. Away from the peak, for and for . 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.
Key words: convection Sun: interior Sun: oscillations
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© European Southern Observatory (ESO) 1998
OnLine pubLication: June 18, 1998