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Convection is the mechanism by which energy is transported through theoutermost 30% of the Sun. Solar turbulent convection is notoriously difficultto model across the entire convection zone where the density spans many ordersof magnitude. In this issue of PNAS, Hanasoge et al. (2012) employ recenthelioseismic observations to derive stringent empirical constraints on theamplitude of large-scale convective velocities in the solar interior. Theyreport an upper limit that is far smaller than predicted by a popularhydrodynamic numerical simulation.

Helioseismology challenges models of solar convection