Fig. 17

Time evolution of the accretion rate, Eddington outflow, and black hole mass of the simulation with Σ0 = 30 M⊙ pc−2 and bcool = 6. Even before the bar potential is switched on completely (186 Myr), there is strong clumpy accretion. The inner disk mass rises quickly and high accretion rates up to 2 M⊙ yr −1 are attained. Later on the Eddington outflow declines much more quickly than the accretion rate. This suggests a decrease in the clumpy accretion.
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