Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...424..480g&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 424, no. 1, p. 480-490
Astronomy and Astrophysics
Astronomy
32
Acoustic Scattering, Solar Convection (Astronomy), Solar Oscillations, Turbulence, Reynolds Stress, Solar Atmosphere
Scientific paper
Acoustic modes are scattered by turbulent velocity fluctuations in the solar convection zone. The strongest scattering occurs near the top of the acoustic cavity where the mode changes character from propagating to evanescent. This layer is located at depth z1 approximately g/omega2 below the photosphere. The scattering optical depth taus is of order M12, where M1 is the Mach number of the energy-bearing eddies at z1. The corresponding contribution to the line width is gammas is approximately (omega) M12/(pi)(n+1), where n is the mode's radial order. At the top of the acoustic cavity the correlation time of energy-bearing eddies is much longer than omega-1. Also, the pressure scale height H and the eddy correlation length Lambda are comparable to omega/c, where c is the sound speed. Thus scattering couples modes of similar omega and all l and has little effect on the sum of their energies. Observations show that mode energies decline with decreasing n (increasing l) at fixed omega. Consequently, scattering damps p-modes and excites f-modes.
Goldreich Peter
Murray Norman
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