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TIDAL DISRUPTIONS IN CIRCUMBINARY DISKS I STAR FORMATION, DYNAMICS, AND BINARY EVOLUTION

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Figure

Figure 1. Gas density projected in the X–Y plane perpendicular to the angular momentum vector of the system for beta1, beta2, beta3a, beta3b, beta3c, and beta5, from the left to the right and from the top to the bottom
Figure 2. Accumulated stellar mass formed in the disk in M  for our fiducial case of a binary of 3.5 ×10 6 M 
Figure 5. Same as Figure 1 for the simulation beta3b. At the SPH time 95 the closest stellar cluster hurls itself on to the binary and leads to an enhancement in the TDEs
Figure 6. Left panel: initial configuration in the X–Y plane perpendicular to the angular momentum vector of the system for simulation beta3b95 of Table 1
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