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Accretion of clumpy cold gas onto massive black hole binaries: a possible fast route to binary coalescence

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Figure 1. Angular momentum orientations of the initial orbit for 20 ran- ran-domly selected clouds from different F distributions, as indicated at the top of each projection
Figure 2. Distribution of pericentre distances as a function of the time at which each cloud is included to the simulation
Figure 3. Angular momentum evolution for the lower resolution runs (50k). The upper panels of each plot show the evolution of the angular momentum magnitude of the entire system (red solid lines) and the binary (dashed blue lines)
Figure 4. Evolution of the binary semimajor axis (top panels), eccentricity (upper middle panels), total accreted mass (lower middle panels), and accretion rate (bottom panels) for all the simulations
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