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We present a new model of large-scale multilayer convection in solar typestars. This model allows us to understand such self-similar structures observedat solar surface as granulation, supergranulation and giant cells. We study theslow-rotated hydrogen star without magnetic field with thespherically-symmetric convective zone. The photon's flux comes to theconvective zone from the central thermonuclear zone of the star. Theinteraction of these photons with the fully ionized hydrogen plasma with$T>10^5K$ is carried out by the Tomson scattering of photon flux on protons andelectrons. Under these conditions plasma is optically thick relative to theTomson scattering. This fact is the fundamental one for the multilayerconvection formation. We find the stationary solution of the convective zonestructure. This solution describes the convective layers responsible to theformation of the structures on the star's surface.

On laminar convection in solar type stars