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Limiting eccentricity of subparsec massive black hole binaries surrounded by self gravitating gas discs

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Academic year: 2020

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Figure 1. Face-on view of the circumbinary disc surrounding a BH binary of initial eccentricity e 0 = 0.6 after 180 orbits
Figure 3. Additional high eccentricity runs where the initial semi-major axis is reduced by a factor 1.8, compared to the default runs
Figure 4. Mass accretion rates onto the BHs, for the runs with e 0 = 0.2, 0.4, 0.6, 0.8 (bottom to top)
Figure 5. Power spectrum of the accretion rate (in arbitrary units 2 ) onto the primary (blue) and secondary (red) BHs
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