During the last decade, it has been suggested that the structure of the solar photosphere,
in the quiet sun, varies over the 11-year activity cycle but this variability of various
quiet sun parameters (intensity, granule sizes, overshoot, etc.) has not been fully
demonstrated yet. The recent advance in the knowledge of the solar granule properties
(flow evolutions, size distribution, spatial organization, interaction with magnetic field,
line asymmetry, penetration in stable layers, morphological properties, etc.) let us
optimistic to try to understand and to measure the cyclic variations of the photosphere.