Damping and frequency reduction of the f-mode due to turbulent motion in the solar convection zone

Details Damping and frequency reduction of the f-mode due to turbulent motion in the solar convection zone Damping and frequency reduction of the f-mode due to turbulent motion in the solar convection zone

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...349..312m&link_type=abstract

Astronomy and Astrophysics, v.349, p.312-316 (1999)

Astronomy and Astrophysics

Astrophysics

8

Convection, Sun: Atmosphere, Sun: Granulation, Sun: Oscillations, Turbulence

Scientific paper

Solar f-mode properties were observed recently with high accuracy using high-resolution Michelson Doppler Imager (MDI) data from SOHO (Duvall et al. 1998). According to these observations, linewidths increase with wavenumber k and the f-mode frequency omega is significantly lower than the frequency omega_0 given by the simple dispersion relation omega_ {0}(2) = gk. This paper provides a possible explanation of these observations on the basis of the turbulent flow that is in the convection zone. The f-mode spends more time propagating against the flow than with the flow. As a result, its effective speed and consequently frequency are reduced. This reduction is revealed by the real part of omega . A negative imaginary part of the frequency omega represents the damping of the coherent f-mode field due to scattering by the turbulent flow. The f-mode damping is a result of the generation of the turbulent field at the expense of the coherent field.

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