Abstract
Coronal holes are characterized by open magnetic field lines morphology. The strongest solar wind originates exactly from the area of solar coronal holes. From the other hand the solar oscillation is present at every point of the solar surface. Currently the mechanism which is responsible for formation of open coronal regions is still unidentified. We present a novel study of waves propagation and frequency distribution in coronal holes, which can bring a new insights in its origin. We investigate the discrepancies in the in waves propagation inside the coronal hole are and in its surrounding, using multi-channel intensity observations data from Atmospheric Imaging Assembly (AIA) and Dopplergrams from Helioseismic and Magnetic Imager (HMI) on board Solar Dynamics Observatory (SDO) at the level of photosphere, chromosphere and corona. We study power distribution of p-modes (5-minute oscillation) and wave frequencies above the acoustic cut-off frequency ѵ=5.3 mHz, for very fast waves, in the various levels of solar atmosphere, through helioseismic approach of wavelet 2D-spatial maps of the power spectral density estimated for the coronal hole area.
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