The Photospheric Convection Spectrum |
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| Authors: | Hathaway DH Beck JG Bogart RS Bachmann KT Khatri G Petitto JM Han S Raymond J |
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| Institution: | (1) NASA/Marshall Space Flight Center, Huntsville, AL , 35812, , U.S.A.;(2) Stanford University, Stanford, CA, , U.S.A.;(3) Birmingham-Southern College, Birmingham, AL , 35254, , U.S.A.;(4) Tennessee Technological University, Cookeville, TN , 38505, , U.S.A. |
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| Abstract: | Spectra of the cellular photospheric flows are determined from observations acquired by the MDI instrument on the SOHO spacecraft. Spherical harmonic spectra are obtained from the full-disk observations. Fourier spectra are obtained from the high-resolution observations. The p-mode oscillation signal and instrumental artifacts are reduced by temporal filtering of the Doppler data. The resulting spectra give power (kinetic energy) per wave number for effective spherical harmonic degrees from 1 to over 3000. Significant power is found at all wavenumbers, including the small wavenumbers representative of giant cells. The time evolution of the spectral coefficients indicates that these small wavenumber components rotate at the solar rotation rate and thus represent a component of the photospheric cellular flows. The spectra show distinct peaks representing granules and supergranules but no distinct features at wavenumbers representative of mesogranules or giant cells. The observed cellular patterns and spectra are well represented by a model that includes two distinct modes – granules and supergranules. |
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