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Title:
On sound generation by turbulent convection: A new look at old results
Authors:
Musielak, Z. E.; Rosner, R.; Stein, R. F.; Ulmschneider, P.
Affiliation:
AA(Univ. of Alabama in Huntsville, Huntsville, AL), AB(Univ. of Alabama in Huntsville, Huntsville, AL), AC(Univ. of Alabama in Huntsville, Huntsville, AL), AD(Univ. of Alabama in Huntsville, Huntsville, AL)
Publication:
The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 423, no. 1, p. 474-487 (ApJ Homepage)
Publication Date:
03/1994
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
SOUND WAVES, STELLAR ATMOSPHERES, STELLAR CONVECTION, TURBULENT FLOW, WAVE GENERATION, ENERGY SPECTRA, FOURIER TRANSFORMATION, REYNOLDS STRESS, WAVE EQUATIONS
DOI:
10.1086/173825
Bibliographic Code:
1994ApJ...423..474M

Abstract

We have revisited the problem of acoustic wave generation by turbulent convection in stellar atmospheres. The theory of aerodynamically generated sound, originally developed by Lighthill and later modified by Stein to include the effects of stratification, has been used to estimate the acoustic wave energy flux generated in solar and stellar convection zones. We correct the earlier computations by incorporating an improved description of the spatial and temporal spectrum of the turbulent convection. We show the dependence of the resulting wave fluxes on the nature of the turbulence, and compute the wave energy spectra and wave energy fluxes generated in the Sun on the basis of a mixing-length model of the solar convection zone. In contrast to the previous results, we show that the acoustic energy generation does not depend very sensitively on the turbulent energy spectrum. However, typical total acoustic fluxes of order FA = 5 x 107 ergs/sq cm/s with a peak of the acoustic frequency spectrum near omega = 100 mHz are found to be comparable to those previously calculated. The acoustic flux turns out to be strongly dependent on the solar model, scaling with the mixing-length parameter alpha as alpha3.8. The computed fluxes most likely constitute a lower limit on the acoustic energy produced in the solar convection zone if recent convection simulations suggesting the presence of shocks near the upper layers of the convection zone apply to the Sun.

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