  We examine the role of stratification in determining the scale for turbulent
anelastic convection. Motivated by the range of scales observed in convection
at the solar photosphere, we perform local numerical simulations of convection
for a range of density contrasts in large domains. We analyse both the Eulerian
and Lagrangian statistics of the convection and demonstrate that increasing the
stratification shifts the scale of the most energetic structures in the flow to
smaller scales; furthermore, the relative amplitude of vertical to horizontal
flows in the convection decreases with increasing stratification. We discuss
the implications of our results to the issue of solar mesogranulation.
