Sources and Propagation of High Frequency Waves in the Solar Photosphere and Chromosphere

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Scientific paper

We study the spatial distribution of oscillatory power in two sequences of high-cadence, high-resolution images taken by the Solar Optical Telescope on board Hinode. The sequences consist of simultaneous, co-registered G-Band (GB) and Ca II H-Line (HL) images with pixel scale 80 km and fields of view 40 x 40 Mm and 80 x 40 Mm. The first sequence has cadence 21 s over 3 hours on 2007 April 14; the other has cadence 24 s over 2 hours on 2007 March 30. Both sequences include network and internetwork at heliocentric angle 35 degrees.
Time averaging of Morlet wavelet transforms gives smoothed Fourier spectra for each spatial location in the GB and HL data. We averaged over four different frequency bands to highlight different physical regimes: "evolutionary” timescales (f < 1.2 mHz); evanescent frequencies just below the acoustic cutoff ( 2.6 mHz < f < 4.2 mHz); high frequencies just above the cutoff (5.5 mHz The evanescent and high frequency spectral images display clear magnetic shadowing in both GB and HL channels, though more strongly in the HL. Thus the heights at which the GB and HL are formed must both straddle the magnetic canopy, with the HL higher up. Interestingly, in the VHF band the magnetic shadowing is markedly weakened. The VHF case shows GB power in the internetwork that is arranged in the boundary web of a cellular pattern with scales 2 - 3 Mm. These are found to coincide with the boundaries of stable clusters of granules. These dark boundaries may correspond to downflows that control the cell structuring and that could be the source of acoustic power.

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