Time evolution of the simulation with Σ₀ = 30 M_⊙ pc⁻² and speed of sound c_s = 3 km s⁻¹, as an example of strong accretion. Top: after a half revolution of the bar, a strong clumpy accretion flow with high Eddington outflow already starts, and decreases with time. Later on the strong accretion is established, which again is highly clumpy at first and reaches an accretion rate of 0.1 M_⊙   yr⁻¹. Bottom: initial clump formation is observed in the inner disk, but fades quickly. Then the inner disk becomes laminar until the strong accretion sets in. Afterward, the complete disk inside 1 kpc exhibits strong clump formation before a gravitational turbulent mode is reached.