Excitation of the solar p-modes.

Details Excitation of the solar p-modes. Excitation of the solar p-modes.

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998acaps..18...68b&link_type=abstract

Acta Astrophys. Sin., Vol. 18, No. 1, p. 68 - 76

Statistics

Computation

Solar Oscillations: Convection, Solar Oscillations: Turbulence

Scientific paper

The authors have revised the mechanism of solar p-mode generation by turbulent stress in the outer parts of the Sun, and estimated the product E˙ ≡ EαΓ, the rate at which energy is supplied to a single solar p-mode. They assume that the line width Γ measures the mode's energy decay rate. In this paper, they correct the earlier computations by incorporating an improved description of the spatial and temporal spectrum of the turbulent convection, and show that 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 contrast to the previous results, the authors show that the solar p-modes are primarily excited by the fluctuations of Reynolds stresses. Away from the peak, E˙ ∝ ν7 for ν < 3 mHz and E˙ ∝ ν5 for ν > 3 mHz, where ν is the frequency. The computed oscillation power spectra can be adjusted to agree with the observations.

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