Sound Speed in a Random Flow and Turbulent Shifts of the Solar Eigenfrequencies

Details Sound Speed in a Random Flow and Turbulent Shifts of the Solar Eigenfrequencies Sound Speed in a Random Flow and Turbulent Shifts of the Solar Eigenfrequencies

1997-05-05

arxiv.org/abs/astro-ph/9705026v1

ApJ, 498 (1998), 458

Astronomy and Astrophysics

Astrophysics

18 pages Latex, uses aasms4

Scientific paper

10.1086/305522

Perturbation theory is used to calculate the frequency shift of acoustic modes of an homogeneous turbulent fluid and the frequency shifts of solar modes due to turbulent convection. For sound waves in a random flow, the fractional frequency shift is +(11/30)M^2 in the long-wavelength limit, and the shift at short wavelengths is -(2/3)M^2, where M is the average Mach number of the flow. In our model of the solar convection, the low-degree f-mode shift is positive and unobservably small, whereas the fractional frequency shift at high degrees (l\gg 500) is -M^2, where M is the Mach number of convection near the solar surface.

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