The Sun is thought to consist of hot gases in highly turbulent motion—but how turbulent is it? Results from modeling and computer simulations give us a partial picture, but there are no direct measurements so far. In this talk, we examine how one can infer the interior motion of the Sun from the satellite observations of its surface and discuss the surprising result of inferred convection velocities 10 to 100 times smaller than previously believed. Does this result mean that our past understanding needs drastic revision? We explore these results as well as the gaps in our understanding of the internal motion of the Sun.

Simultaneous Arabic translation will be provided.

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