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The purpose of this paper is to characterize the statistical properties ofsolar granulation in the photosphere and low chromosphere up to 650 km. We usevelocity and intensity variations obtained at different atmospheric heightsfrom observations in BaII 4554 A. The observations were done during good seeingconditions at the VTT at the Observatorio del Teide on Tenerife. The line coreforms rather high in the atmosphere and allows granulation properties to bestudied at heights that have been not accessed before in similar studies. Inaddition, we analyze the synthetic profiles of the BaII 4554 A line by the samemethod computed taking NLTE effects into account in the 3D hydrodynamical modelatmosphere. We suggest a 16-column model of solar granulation depending on thedirection of motion and on the intensity contrast measured in the continuum andin the uppermost layer. We calculate the heights of intensity contrast signreversal and velocity sign reversal. We show that both parameters dependstrongly on the granulation velocity and intensity at the bottom photosphere.The larger the two parameters, the higher the reversal takes place in theatmosphere. On average, this happens at about 200-300 km. We suggest that thisnumber also depends on the line depth of the spectral line used inobservations. Despite the intensity and velocity reversal, about 40% of thecolumn structure of granulation is preserved up to heights around 650 km.

Solar granulation from photosphere to low chromosphere observed in BaII 4554 A line