The spectrograms were digitized and processed with wavelet techniques and regression analysis. The latter was applied to granular convective flow and the apparently associated turbulence in order to investigate their mutual connection. This will have consequences for our understanding of the p-mode excitation and provide better insight into the physics of the origin of the turbulence in the deep photosphere and its implications for helioseismology. Images of solar surface velocity and magnetic field strength with 4'' spatial resolution and a 60 second temporal resolution are analyzed. A two dimensional gaussian aperture with a FWHM of 10'' is applied to the data in regions of sunspot, plage and quiet sun and the resulting averaged signal is returned each minute.
Significant power is observed in the magnetic field oscillations with periods of five minutes.
It is assumed that the large amplitude acoustic waves with 5 minute periods are the driving mechanism behind the magnetic oscillations. The nature of the magnetohydrodynamic oscillations are characterized by their phase relations with simultaneously observed solar surface velocity oscillations. The data, including simultaneous line shift, line depth, and continuum intensity measurements at disk center, have been obtained from a MDI time series in its high resolution mode. Line depth and continuum intensity are used to calculate the line intensity which is the more frequently used parameter in phase difference studies. We compare the results to ground based observations.