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3D model atmospheres for giants, dwarfs, and white dwarfs, computed with theCO5BOLD code and part of the CIFIST grid, have been used for spectroscopic andasteroseismic studies. Unlike existing plane-parallel 1D structures, thesesimulations predict the spatially and temporally resolved emergent intensity sothat granulation can be analysed, which provides insights on how convectiveenergy transfer operates in stars. The wide range of atmospheric parameters ofthe CIFIST 3D simulations (3600 < Teff (K) < 13,000 and 1 < log g < 9) allowsthe comparison of convective processes in significantly different environments.We show that the relative intensity contrast is correlated with both the Machand Peclet numbers in the photosphere. The horizontal size of granules variesbetween 3 and 10 times the local pressure scale height, with a tightcorrelation between the factor and the Mach number of the flow. Given thatconvective giants, dwarfs, and white dwarfs cover the same range of Mach andPeclet numbers, we conclude that photospheric convection operates in a verysimilar way in those objects.

Granulation properties of giants, dwarfs, and white dwarfs from the CIFIST 3D model atmosphere grid