Towards a self-consistent model of the convective core boundary in upper main sequence stars - I. 2.5D and 3D simulations

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Fig. 5.

Time evolution of the convective velocity u_conv in all of our simulations with radiative diffusion. The time axis shows simulation time as a fraction of the thermal timescale τ_th(b). Each data point corresponds to a time average over 0.05τ_th. The right vertical axis shows the corresponding Mach numbers computed using the reference sound speed c_ref = 7.96 × 10⁷ cm s⁻¹.

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